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Download Citation (0) © PTL OPEN April 17, 2021 at 4:01:45 AM Fabrication of Non-volatile Charge Storage Memory Device by Novel doped ZnO nanoparticles with 4.79 eV bandgap Nowadays, the drastic participation of the nanosized materials in technology have been implicated with various applications which mainly aims the performance optimization, dimensional downscaling, ultra-low power consumption etc. to overcome the fundamental limits of the microscale devices. It is the requisite stage to familiarize a convenient alternative of the traditional large-scale technologies in the purpose of accelerating the flow of the applied science for mankind. This article presents two novel non-volatile device structures which are fabricated by layer by a layer deposition method. I-V measurements for both the samples justify the device characteristic as p-type –insulator–n-type configuration. The measurements confirm that the successful fabrication of those devices and proves the high-density charge capacity with an improved lifetime of the carriers compared to erstwhile reports. The measured the threshold voltage for this device is 0.939V. Material Science Letters Keylines Introduction To unfold the hidden mysteries of the molecules and their applications the nanoscience have been presented plenty of its morphism in order to rapid performance scale up with drastic dimensional down scaling. Manipulation of the molecular information technology has numerous existing approaches for instance molecular non-volatile memory, electron spin devices, nano-memorister, quantum dot island based devices, capacitive devices etc. which have proven their superior activities in binary logic and storage device applications. Nowadays, the utility of the hard storage has become quite crucial and instantaneous which claims to be tinier and fastest to meet the present requirements of the mankind. The fabrication of the non-volatile charge storage devices opens a convenient way with millions charge storing capacity in a few nanometer areas. In this letter the ZnO nanoparticle-based non-volatile memory device has reported which provides a better optimization to the device efficiency. To fabricate this device three major materials have involved those are PMMA, Ag NPs, ZnO NPs. In another type of the device is fabricated by using Nafion which exhibits a benchmarking of the p-i-n diode. The PMMA layer is used as the tunneling barrier for the electrons that provides a path to the electrons to be tunnelled during the biasing application but resistance during cutoff state. It also acts as the high impedance to the electrons during cutoff state that resists from the discharging by defending the reverse tunnelling. To fabricate this device the ZnO and Ag doped ZnO NPs are utilized and specifically sputtered on the surface of the ITO. Two different types of devices have been walked through firstly ITO/PMMA/Nafion has been examined and next is ITO/PMMA /ZnO-NPs doped with Ag NPs. The reduced bandgap of the doped ZnO layer works as the electron hopping state and allows to operate it at ultra-low power input. Conclusion This work is performed for fabricating the non-volatile devices based on ZnO and metal-doped ZnO nanoparticles. In collaboration with the four probe I-V characteristics measurement, the devices have proven that both are having a non-volatile nature and the those are having very less threshold voltage which can trigger device at very low power. The improvement in the charge storage capacity is notable in both the devices. The unexpected bandgap for the ZnO is being verified through several observations and experiments. In the future articles, this may come across. References [1] Fushan Li, et.al. , "Nonvolatile Memory Effects of ZnO Nanoparticles Embedded in an Amorphous Carbon Layer", Japanese Journal of Applied Physics 49 (2010) 070209. [2] Biswanath Mukherjee and Moumita Mukherjee, "Nonvolatile memory device based on Ag nanoparticle: Characteristics improvement" Applied Physics Letters 94, 173510 (2009); doi: 10.1063/1.3127233. [3] V. L. Covin, M. C. Schlamp, and A. P. Alivisatos: Nature (London) 370 (1994) 354. [4] T. Homma, T. Kutsuzawa, K. Kunimune, and Y. Murao: Thin Solid Films 235 (1993) 80. [5] M. Horie: J. Vac. Sci. Technol. A 3 (1995) 2490. [6] S. Mizuno, A. Verma, H. Tran, P. Lee, and B. Nguyen: Thin Solid Films 283 (1996) 30. [7] H. J. Ko, K. M. Lee, H. J. Lee, and C. K. Choi: Thin Solid Films 506–507 (2006) 8 . [8] Z. J. Donhauser, B. A. Mantooth, K. F. Kelly, L. A. Bumm, J. D. Monnell, J. J. Stapleton, Jr., D. W. Price, A. M. Rawlett, D. L. Allara, J. M. Tour, and P. S. Weiss, Science 292, 2303 2001 . Submit a manuscript

Theoretical Physics Letters HOME JOURNALS PRICING AND PLANS SUBMIT Locked Tphysicsletters/6879/10/1490/9586tpl/Surface-Enhanced Raman Scattering from Au Nanorods, Nanotriangles, and Nanostars with Tuned Plasmon Resonances Citation (0) Tuesday, October 3, 2023 at 11:45:00 AM UTC Request Open Apply Now Article Rating by Publisher 8 NanoPhysics Article Rating by Readers 9.2 Premium doi.wikipt.org/10/1490/9586tpl Surface-Enhanced Raman Scattering from Au Nanorods, Nanotriangles, and Nanostars with Tuned Plasmon Resonances Boris N. Khlebtsov,1 Andrey M. Burov,1 Sergey V. Zarkov,1 Nikolai G. Khlebtsov,1,2,* ---------------------------------------------------- 1 Institute of Biochemistry and Physiology of Plants and Microorganisms, "Saratov Scientific Centre of the Russian Academy of Sciences," 13 Prospekt Entuziastov, Saratov 410049, Russia 2 Saratov State University, 83 Ulitsa Astrakhanskaya, Saratov 410012, Russia Theoretical Physics Letters 2023 ° 03(10) ° 0631-9586 https://www.wikipt.org/tphysicsletters DOI : https://www.doi.wikipt.org/10/1490/9586tpl TOA Abstract Introduction Conclusion Acknowledgement This research was supported by the Russian Science Foundation (project no. № 23-24-00062). The work on computer simulations was funded by the Ministry of Science and Higher Education of the Russian Federation as a state assignment for the Saratov Scientific Centre of the Russian Academy of Sciences (research topic no. 121032300310-8). We thank A.A. Merdalimova for SERS measurements with LabRam HR Evolution spectrometer. Unlock Only Changeover the Schrödinger Equation This option will drive you towards only the selected publication. If you want to save money then choose the full access plan from the right side. Unlock all Get access to entire database This option will unlock the entire database of us to you without any limitations for a specific time period. This offer is limited to 100000 clients if you make delay further, the offer slots will be booked soon. Afterwards, the prices will be 50% hiked. Buy Unlock us Newsletters Abstract Electromagnetic theory predicts that the optimal value of the localized plasmon resonance (LPR) wavelength for the maximal SERS enhancement factor (EF) is half the sum of the laser and Raman wavelengths. For small Raman shifts, the theoretical EF scales as the fourth power of the local field. However, experimental data often disagree with these theoretical conclusions, leaving the question of choosing the optimal plasmon resonance for the maximal SERS signal unresolved. Here, we present experimental data for gold nanorods (AuNRs), gold nanotriangles (AuNTs), and gold nanostars (AuNSTs) simulating 1D, 2D, and 3D plasmonic nanostructures, respectively. The LPR wavelengths were tuned by chemical etching within 550 1050 nm at constant number concentrations of the particles. The particles were functionalized with Cy7.5 and NBT, and the dependence of the intensity at 940 cm-1 (Cy7.5) and 1343 cm-1 (NBT) on the LPR wavelength was examined for laser wavelengths of 633 nm and 785 nm. The electromagnetic SERS EFs were calculated by averaging the product of the local field intensities at the laser and Raman wavelengths over the particle surface and their random orientations. The calculated SERS plasmonic profiles were redshifted compared to the laser wavelength. For 785- nm excitation, the calculated EFs were five to seven times higher than those for 633-nm excitation. With AuNR@Cy7.5 and AuNT@ Cy7.5, the experimental SERS was 35-fold stronger than it was with NBT-functionalized particles, but with AuNST@Cy7.5 and AuNST@NBT, the SERS responses were similar. With all nanoparticles tested, the SERS plasmonic profiles after 785 nm excitation were slightly blue-shifted, as compared with the laser wavelength, possibly owing to the inner filter effect. After 633-nm excitation, the SERS profiles were redshifted, in agreement with EM theory. In all cases, the plasmonic EF profiles were much broadened compared to the calculated ones and did not follow the four-power law. Introduction Strong local field enhancement near plasmonic nanoparticles is the primary physical mechanism behind the surface-enhanced Raman scattering (SERS).1,2 Recent advances in wetchemical technologies3 provide great possibilities for precise tuning of the localized plasmonresonance (LPR) to any desired wavelength from blue (~400 nm) to NIR.4 These synthesis advances raise the following important question:5 Which excitation wavelength maximizes the SERS response for a given LPR nanostructure? There are two possible approaches to answer. The first one is the so-called plasmon-sampled SER excitation spectroscopy (PS-SERES) in which a set of substrates such as nanosphere-lithography (NL) Ag prisms,6 Au nanostar (AuNST)7 or Au nanorod (AuNR) colloids8 with different LPRs is excited by a fixed laser wavelength to find the sample with the maximal SERS response. The second approach is the wavelength-scanned SER excitation spectroscopy (WS-SERES) in which light with variable wavelengths excites a particular Ag-island film,9, 10 Ag-NL,11 or vertically aligned AuNRs12 with a specific LPR spectral profile. This method seems straightforward but is more technically challenging because of the limited laser source with variable wavelength. Nevertheless, the multiple-laser-wavelength excitation of AuNRs functionalized with different dyes allows for SERS bioimaging of cells within the 514-1064 nm spectral band.13Although it is usually believed that excitation at the LPR wavelength gives maximal SERS response,14 15 there is experimental evidence for optimal excitation wavelengths that are slightly blue shifted, as compared with the LPR.16 What is more, Weitz et al.9 proposed a phenomenological relation to approximate the relative SERS intensity, from which the optimal LPR resonance wavelength was found17 to be half of the excitation and Raman scattering wavelengths ( )/2  LPR ex RS     (the absorption spectrum is assumed to have the Lorentzian shape). This rule has been confirmed in experiments with Ag island film substrates and, more precisely, with Ag-NL substrates in PS-SERES,6 WS-SERES,11 and WS-SERRES18 experiments. Read more related publications. X-ray polarization properties of partially ionized equatorial obscurers around a Buy Now Perturbative aspects of mass dimension one fermions non-minimally coupled to ele Buy Now CMOS + stochastic nanomagnets: heterogeneous computers for probabilistic inferen Buy Now Conclusion In this work, we synthesized, characterized by spectroscopy and TEM methods, and studied the dependence of the SERS electromagnetic amplification factor on the plasmon resonance wavelength of three types of colloidal nanoparticles (AuNRs, AuNTs, AuNSTs) functionalized by two types of Raman molecules and excited by two laser wavelengths of 785 and 633 nm. Comparing the simulated extinction spectra of AuNRs with the T-matrix and COMSOL methods, we showed that the theoretical dependence of the LPR wavelength on the aspect ratio does not agree with the TEM-derived data if the 3-nm CTAB layer on the nanorod surface is not included in simulations. Using the chemical etching method, we synthesized 13 AuNR samples with LPR wavelengths from 1017 to 580 nm, functionalized them with Cy7.5 and NBT molecules, and measured their SERS spectra upon excitation with 633 nm and 785 nm lasers. For comparison with the measurement data, the plasmon profiles of the SERS enhancement factor EF were calculated by averaging the product of the field intensities of the local field at the laser and Raman wavelengths over the surface of particles and their random orientations. Qualitatively, the simulation results agree with the measurements. In particular, the theoretical maximum EF for AuNR@Cy7.5 particles is two times greater than the maximum for AuNR@NBT. Together with a higher Raman cross section of Cy7.5 (compared to NBT), this explains the experimental 35-fold difference between SERS EFs for AuNR@Cy7.5 and AuNR@NBT particles. The main difference between measurements and simulations is that the experimental maximum EF upon excitation with a 785 nm laser is observed at a wavelength LPR less than the laser wavelength, while in theory, it is vice versa. Finally, the width of the experimental plasmon gain SERS profile is much broader than the calculated one. For gold nanotriangles, efficient methods have been developed for averaging the integral optical cross sections over random particle orientations. The results of measurement and analysis of the SERS spectra for AuNT@Cy7.5 and AuNT@NBT particles upon excitation by 633 nm and 785 nm lasers are largely similar to the conclusions obtained for nanorods. In the case of gold nanostars, the main difference from the results for previous experimental models is a small difference between the maximum EF values for AuNT@Cy7.5 and AuNT@NBT particles. The rest of the conclusions apply to these particles as well. 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Theoretical Physics Letters HOME JOURNALS PRICING AND PLANS SUBMIT PTL LOCKED Tphysicsletters/vol-10/no-1296/CInteger and fractional Chern insulators in twisted bilayer MoTe2 Citation (0) Tuesday, May 2, 2023 at 6:30:00 AM UTC Request Open Apply Now DOI: 10.1490/698700.590tpl Integer and fractional Chern insulators in twisted bilayer MoTe2 Yihang Zeng1 Theoretical Physics Letters 2023 ° 02(05) ° 10-1296 https://www.wikipt.org/tphysicsletters DOI: 10.1490/698700.590tpl TOA Abstract Introduction Conclusion Unlock Only Changeover the Schrödinger Equation This option will drive you towards only the selected publication. If you want to save money then choose the full access plan from the right side. Unlock all Get access to entire database This option will unlock the entire database of us to you without any limitations for a specific time period. This offer is limited to 100000 clients if you make delay further, the offer slots will be booked soon. Afterwards, the prices will be 50% hiked. Buy Unlock us Newsletters Abstract Chern insulators, which are the lattice analogs of the quantum Hall states, can potentially manifest high-temperature topological orders at zero magnetic field to enable next-generation topological quantum devices 1-4 . To date, integer Chern insulators have been experimentally demonstrated in several systems at zero magnetic field 3, 5-11, but fractional Chern insulators have been reported only in graphene-based systems under a finite magnetic field 12, 13. The emergence of semiconductor moiré materials 14, 15, which support tunable topological flat bands 16, 17, opens a new opportunity to realize fractional Chern insulators 18-20. Here, we report the observation of both integer and fractional Chern insulators at zero magnetic field in small-angle twisted bilayer MoTe2 by combining the local electronic compressibility and magneto-optical measurements. At hole filling factor 𝝂 = 𝟏 and 2/3, the system is incompressible and spontaneously breaks time reversal symmetry. We determine the Chern number to be 1 and 2/3 for the 𝝂 = 𝟏 and 𝝂 = 𝟐/𝟑 gaps, respectively, from their dispersion in filling factor with applied magnetic field using the Streda formula. We further demonstrate electric-field-tuned topological phase transitions involving the Chern insulators. Our findings pave the way for demonstration of quantized fractional Hall conductance and anyonic excitation and braiding 21 in semiconductor moiré materials. Introduction Fractional Chern insulators (FCIs), which can in principle host the fractional quantum Hall effect and non-Abelian excitations at zero magnetic field, are highly sought-after phases of matter in condensed matter physics 22-28. The experimental realization of FCIs may also revolutionize other fields, such as topological quantum computation 21. But FCIs have proven notoriously challenging to realize experimentally because they require not only a topological flat band but also particular quantum band geometry 17-19, 29-33 . Band-structure engineering by forming moiré superlattices has emerged as a powerful approach to realize topological flat bands 11, 14, 15, 29, 34. A recent experiment has shown that FCIs can be stabilized in magic-angle twisted bilayer graphene at about 5 T, where the magnetic field is mainly responsible for redistributing the Berry curvature of the original topological bands 13. With widely tunable electronic properties, moiré materials based on transition metal dichalcogenide (TMD) semiconductors have been predicted to support topological flat bands with appropriate band geometry to favor FCIs at zero magnetic field 18-20. Of particular interest are small-angle twisted TMD homobilayers of the AA-stacking type (Fig. 1a). They support a honeycomb moiré lattice with two sublattices residing in two different layers 16, 17. The topmost moiré valence bands are composed of the spin-valley locked states from the K or K’ valley of the monolayers. Theoretical studies have shown that the complex interlayer hopping between the sublattice sites can induce topological moiré valence bands with non-zero spin/valley-resolved Chern numbers (𝐶) 16, 17 , and for certain twist angles, the topmost moiré band (with |𝐶| = 1) is nearly flat and exhibits a flat Berry curvature distribution 16-19. This opens the possibility of stabilizing FCIs at fractional fillings. Here we report the observation of an integer Chern insulator (CI) at 𝜈 = 1 and FCI at 𝜈 = 2/3 under zero magnetic field in 3.4-degree twisted bilayer MoTe2 (tMoTe2). The filling factor 𝜈 measures the hole doping density (n) in units of the moiré unit cell density (𝑛𝑀), and 𝜈 = 1 corresponds to quarter-band filling. These states display hallmarks of a CI. Specifically, they are incompressible, spontaneously break time reversal symmetry (TRS), linearly disperse in doping density with applied magnetic field, and carry an orbital magnetization that jumps across the charge gap. Furthermore, as the interlayer potential difference increases, our experiment at 1.6 K indicates a continuous topological phase transition from the integer CI to a topologically trivial Mott insulator, whereas the FCI becomes compressible. Conclusion We demonstrate an integer and a fractional CI at zero magnetic field in small-angle tMoTe2 by the local measurements of the electronic compressibility and TRS breaking. We also observe evidence for a continuous topological phase transition for both CI states that is induced by the interlayer potential difference. Our findings leave open many questions, such as the nature of the FCI and possible existence of FCIs in tMoTe2 and related materials that have no analogs in the fractional quantum Hall system. A pressing experimental task is to develop electrical contacts to these materials for transport measurements and for manipulation of the anyonic excitation for topological quantum applications. During the preparation of this manuscript, we learned about the work that reports signatures of FCIs in tMoTe2 using optical spectroscopy techniques 48 , as well as another work that reports integer CIs in tWSe2 using local compressibility measurements 49. TOC (TphysicsLetters) TOC (TphysicsLetters) The Nature of the 1 MeV-Gamma Quantum in a Classic Interpretation of the Quantum Nebular spectra from Type Ia supernov Physics Tomorrow TOC HIGHLIGHTS 2023 TOC HIGHLIGHTS 2023 Theoretical Physics Letters Physics Tomorrow ZZ Ceti stars of the southern ecliptic hemisphere re-observed by TESS ZZ Ceti stars of the southern ecliptic hemisphere re-observed by TESS Physics Tomorrow References 1. Haldane, F.D.M. Model for a Quantum Hall Effect without Landau Levels: Condensed-Matter Realization of the "Parity Anomaly". Physical Review Letters 61, 2015-2018 (1988). 2. Hasan, M.Z. & Kane, C.L. Colloquium: Topological insulators. Reviews of Modern Physics 82, 3045-3067 (2010). 3. Liu, C.-X., Zhang, S.-C. & Qi, X.-L. The Quantum Anomalous Hall Effect: Theory and Experiment. Annual Review of Condensed Matter Physics 7, 301-321 (2016). 4. Chang, C.-Z., Liu, C.-X. & MacDonald, A.H. Colloquium: Quantum anomalous Hall effect. Reviews of Modern Physics 95, 011002 (2023). 5. Chang, C.-Z. et al. Experimental Observation of the Quantum Anomalous Hall Effect in a Magnetic Topological Insulator. Science 340, 167-170 (2013). 6. Sharpe, A.L. et al. Emergent ferromagnetism near three-quarters filling in twisted bilayer graphene. Science 365, 605-608 (2019). 7. Serlin, M. et al. Intrinsic quantized anomalous Hall effect in a moiré heterostructure. Science 367, 900-903 (2020). 8. Chen, G. et al. Tunable correlated Chern insulator and ferromagnetism in a moiré superlattice. Nature 579, 56-61 (2020). 9. Deng, Y. et al. Quantum anomalous Hall effect in intrinsic magnetic topological insulator MnBi2Te4. Science 367, 895-900 (2020). 10. Li, T. et al. Quantum anomalous Hall effect from intertwined moiré bands. Nature 600, 641-646 (2021). 11. Liu, J. & Dai, X. Orbital magnetic states in moiré graphene systems. Nature Reviews Physics 3, 367-382 (2021). 12. Spanton, E.M. et al. Observation of fractional Chern insulators in a van der Waals heterostructure. Science 360, 62-66 (2018). 13. Xie, Y. et al. Fractional Chern insulators in magic-angle twisted bilayer graphene. Nature 600, 439-443 (2021). 14. Kennes, D.M. et al. Moiré heterostructures as a condensed-matter quantum simulator. Nature Physics 17, 155-163 (2021). 15. Mak, K.F. & Shan, J. Semiconductor moiré materials. Nature Nanotechnology 17, 686-695 (2022). 16. Wu, F., Lovorn, T., Tutuc, E., Martin, I. & MacDonald, A.H. Topological Insulators in Twisted Transition Metal Dichalcogenide Homobilayers. Physical Review Letters 122, 086402 (2019). 17. Devakul, T., Crépel, V., Zhang, Y. & Fu, L. Magic in twisted transition metal dichalcogenide bilayers. Nature Communications 12, 6730 (2021). 18. Li, H., Kumar, U., Sun, K. & Lin, S.-Z. Spontaneous fractional Chern insulators in transition metal dichalcogenide moir\'e superlattices. Physical Review Research 3, L032070 (2021). 19. Valentin Crépel, L.F. Anomalous Hall metal and fractional Chern insulator in twisted transition metal dichalcogenides. arXiv:2207.08895 (2022). 20. Nicolás Morales-Durán, J.W., Gabriel R. Schleder, Mattia Angeli, Ziyan Zhu, Efthimios Kaxiras, Cécile Repellin, Jennifer Cano. Pressure--enhanced fractional Chern insulators in moiré transition metal dichalcogenides along a magic line. arXiv:2304.06669 (2023). 21. Nayak, C., Simon, S.H., Stern, A., Freedman, M. & Das Sarma, S. Non-Abelian anyons and topological quantum computation. Reviews of Modern Physics 80, 1083-1159 (2008). 22. Sheng, D.N., Gu, Z.-C., Sun, K. & Sheng, L. Fractional quantum Hall effect in the absence of Landau levels. Nature Communications 2, 389 (2011). 23. Neupert, T., Santos, L., Chamon, C. & Mudry, C. Fractional Quantum Hall States at Zero Magnetic Field. Physical Review Letters 106, 236804 (2011). 24. Tang, E., Mei, J.-W. & Wen, X.-G. High-Temperature Fractional Quantum Hall States. Physical Review Letters 106, 236802 (2011). 25. Regnault, N. & Bernevig, B.A. Fractional Chern Insulator. Physical Review X 1, 021014 (2011). 26. Qi, X.-L. Generic Wave-Function Description of Fractional Quantum Anomalous Hall States and Fractional Topological Insulators. Physical Review Letters 107, 126803 (2011). Abstract Introduction Conclusion References All Products Quick View Newly listed Tphysletters A Unifying Bag Model of Composite Fermionic Structures in a Cold Genesis Theory Regular Price $700.00 Sale Price $400.00 Excluding Sales Tax Quick View TphysicsLetters Detection of the large-scale tidal field with galaxy multiplet alignment in the Regular Price $1,900.00 Sale Price $950.00 Excluding Sales Tax Quick View Newly listed Tphysletters Violation of γ in Brans-Dicke gravity Regular Price $1,000.00 Sale Price $600.00 Excluding Sales Tax Quick View Astrophysics Observations and detectability of young Suns’ flaring and CME activity in optica Regular Price $1,000.00 Sale Price $450.00 Excluding Sales Tax Quick View TphysicsLetters Tunable structure-activity correlations of molybdenum dichalcogenides (MoX2; X=S Regular Price $2,000.00 Sale Price $400.00 Excluding Sales Tax Quick View New Thphysletters Bayesian and frequentist investigation of prior effects in EFTofLSS analyses of Regular Price $3,000.00 Sale Price $370.00 Excluding Sales Tax Quick View New Thphysletters A search for faint resolved galaxies beyond the Milky Way in DES Year 6: A new f Regular Price $1,900.00 Sale Price $750.00 Excluding Sales Tax Quick View New X-ray polarization properties of partially ionized equatorial obscurers around a Regular Price $800.00 Sale Price $350.00 Excluding Sales Tax Quick View New Unravelling multi-temperature dust populations in the dwarf galaxy Holmberg II Regular Price $1,200.00 Sale Price $400.00 Excluding Sales Tax Quick View New SpookyNet: Advancement in Quantum System Analysis through Convolutional Neural N Regular Price $1,500.00 Sale Price $500.00 Excluding Sales Tax Quick View New Rapid neutron star cooling triggered by accumulated dark matter Regular Price $1,500.00 Sale Price $500.00 Excluding Sales Tax Quick View Newly listed Tphysletters Searching for Radio Outflows from M31* with VLBI Observations Price $300.00 Excluding Sales Tax Quick View New Thphysletters Measurement of the scaling slope of compressible magnetohydrodynamic turbulence Regular Price $680.00 Sale Price $612.00 Excluding Sales Tax Quick View MAKE OPEN ACCESS New method to revisit the gravitational lensing analysis of the Bullet Cluster u Price $1,030.00 Excluding Sales Tax Quick View New Thphysletters New method to revisit the gravitational lensing analysis of the Bullet Cluster u Regular Price $599.00 Sale Price $359.40 Excluding Sales Tax Quick View New Nebular spectra from Type Ia supernova explosion models compared to JWST observa Regular Price $503.00 Sale Price $271.62 Excluding Sales Tax Quick View New Thphysletters The Nature of the 1 MeV-Gamma quantum in a Classic Interpretation of the Quantum Price $399.00 Excluding Sales Tax Quick View Exceptional Classifications of Non-Hermitian Systems Price $399.00 Excluding Sales Tax Quick View New Thphysletters On the occurrence of stellar fission in binary-driven hypernovae Price $399.00 Excluding Sales Tax Quick View New ApplSciLettersA AC frequency influence on pump temperature Price $399.00 Excluding Sales Tax Quick View New ApplSciLett. 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Theoretical Physics Letters HOME JOURNALS PRICING AND PLANS SUBMIT PTL LOCKED Tphysicsletters/6981/1296/Calculation of the Hubble Constant, the Minimum Mass, and the Proton Citation (0) Friday, June 2, 2023 at 6:30:00 AM UTC Request Open Apply Now DOI: 10.1490/369869.0692tpl Calculation of the Hubble Constant, the Minimum Mass, and the Proton Charge Radius Using the Dirac’s Hypothesis on the Ratio of the Electrostatic Force to the Gravitational Force Paul Talbot Theoretical Physics Letters 2023 ° 02(06) ° 0631-1296 https://www.wikipt.org/tphysicsletters DOI: 10.1490/369869.0692tpl TOA Abstract Introduction Conclusion Unlock Only Changeover the Schrödinger Equation This option will drive you towards only the selected publication. If you want to save money then choose the full access plan from the right side. Unlock all Get access to entire database This option will unlock the entire database of us to you without any limitations for a specific time period. This offer is limited to 100000 clients if you make delay further, the offer slots will be booked soon. Afterwards, the prices will be 50% hiked. Buy Unlock us Newsletters Abstract This publication suggests that some physical values could be calculated using the Dirac’s hypothesis on the observed ratio of the electrostatic force to the gravitational force. The calculated value of the Hubble constant is H ≈ 72.013 km s‑1 Mpc‑1 and that of the minimum mass, M min ≈ 1.720 6 × 10‑68 kg. Recent observations suggest that the proton charge radius could also be calculated using an additional but related assumption: r p ≈ 0.826 4 fm. Introduction Currently, the local value of the Hubble constant is determined by observation. The observed values are more or less precise, and oscillate between 70 km s‑1 Mpc-1 and 74 km s‑1 Mpc-1, depending on the techniques used (Riess et al., 2022) (Freedman, 2021) (Khetan et al., 2021) (Liao et al., 2020) (Pesce et al., 2020) (Yang et al., 2020). We know that some physical quantities are limited by minimum values. For example, the quantum of action h is the minimum value of action. The elementary charge e can also be regarded as the minimum charge. Quarks are associated with a fractional charge, but they are confined inside hadrons, which do have an integer charge (Perl et al., 2004). Conclusion Using the observed ratio of the electrostatic force to the gravitational force, the assumed relation Eq. 6 allows precisely calculating the Hubble constant and the minimum mass. These values agree with observation and previous works. Recent observations suggest that the proton charge radius could also be calculated using an additional but related assumption (Eq. 16). It is unlikely that an arbitrary value of E ep could lead to such consistent results. More precise observed values of H and r p could confirm or refute some of these hypotheses. TOC (TphysicsLetters) TOC (TphysicsLetters) The Nature of the 1 MeV-Gamma Quantum in a Classic Interpretation of the Quantum Nebular spectra from Type Ia supernov Physics Tomorrow TOC HIGHLIGHTS 2023 TOC HIGHLIGHTS 2023 Theoretical Physics Letters Physics Tomorrow ZZ Ceti stars of the southern ecliptic hemisphere re-observed by TESS ZZ Ceti stars of the southern ecliptic hemisphere re-observed by TESS Physics Tomorrow References Berman , M. (1992). Large number hypothesis. International Journal of Theoretical Physics, 31 , 1447-1450. doi:10.1007/BF00673977 Beyer, A., Maisenbacher, L., Matveev, A., Pohl, R., Khabarova, K., Grinin, A., . . . Udem, T. (2017). The Rydberg constant and proton size from atomic hydrogen. Science, 358 , 79-85. doi:10.1126/science.aah6677 Bezginov, N., Valdez, T., Horbatsch, M., Marsmsn, A., Vuta, A., & Hessels, E. (2019). A Measurement of the Atomic Hydrogen Lamb Shift and the Proton Charge Radius. Science, 365 , 1007-1012. doi:10.1126/science.aau7807 Cetto, A., Peña, L. d., & Santos, E. (1986). Dirac’s large-number hypothesis revised. Astronomy and Astrophysics, 164, Bibcode: 1986A&A...164....1C , 1-5. Dirac, P. A. (1938). A new basis for cosmology. Proceedings of the Royal Society of London, 165 , 199-208. doi:10.1098/rspa.1938.0053 Dirac, P. A. (1974). Cosmological Models and the Large Numbers Hypothesis. Proceedings of the Royal Society of London, 338 , 439-446. doi:10.1098/rspa.1974.0095 Dirac, P. A. (1979). The Large Numbers hypothesis and the Einstein theory of gravitation. Proceedings of the Royal Society (365), 19-30. doi:10.1098/rspa.1979.0003 Djukanovic, D., Harris, T., von Hippel, G., Junnarkar, P., Meyer, H., Mohler, D., . . . Wilhelm, J. (2021). Isovector electromagnetic form factors of the nucleon from lattice QCD and the proton radius puzzle. Physical Review D, 103 (094522), 25. doi:10.48550/arXiv.2102.07460 Freedman, W. (2021). Measurements of the Hubble Constant: Tensions in Perspective. The Astrophysical Journal, 919:16 , 22. doi:10.3847/1538-4357/ac0e95 Khetan, N., Izzo, L., Branchesi, M., Wojtak, R., Cantiello, M., Murugeshan, C., . . . Valenti, S. (2021). A new measurement of the Hubble constant using Type Ia supernovae calibrated with surface brightness fluctuations. Astronomy & Astrophysics, 647 (A72), 20. doi:10.1051/0004-6361/202039196 Kritov, A. (2021). Explicit Values for Gravitational and Hubble Constants from Cosmological Entropy Bound and Alpha-Quantization of Particle Masses. Progress in Physics, 17, ISSN: 1555-5615 (online), Corpus ID: 245259641 , 158-163. Lau, Y., & Prokhovnik, S. J. (1986). The Large Numbers Hypothesis and a Relativistic Theory of Gravitation. Australian Journal of Physics, 39 , 339-346. doi:10.1071/PH860339 Liao, K., Shafieloo, A., Keeley, R. E., & Linder, E. V. (2020). A Model-independent Determination of the Hubble Constant from Lensed Quasarsand Supernovae Using Gaussian Process Regression. The Astrophysical Journal Letters, 886 (L23), 7. doi:10.3847/2041-8213/ab5308 Lusso, E., Piedipalumbo, E., Risaliti, G., Paolillo, M., Bisogni, S., Nardini, E., & Amati, L. (2019). Tension with the flat ΛCDM model from a high-redshift Hubble diagram of supernovae, quasars, and gamma-ray bursts. Astronomy & Astrophysics, 628 (L4), 5. doi:10.1051/0004-6361/201936223 Mercier, C. (2019). Calculation of the Universal Gravitational Constant, of the Hubble Constant, and of the Average CMB Temperature. Journal of Modern Physics, 10 , 641-662. doi:10.4236/jmp.2019.106046 Perl, M. L., Lee, E. R., & Loomba, D. (2004). A Brief Review of the Search for Isolatable Fractional Charge Elementary Particles. Modern Physics Letters, 19.35 , 16. doi:10.1142/S0217732304016019 Pesce, D. W., Braatz, J. A., Reid, M. J., Riess, A. G., Scolnic, D., Condon, J., . . . Lo, K. (2020). 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Monthly Notices of the Royal Astronomical Society, 497 , 56-61. doi:10.1093/mnrasl/slaa107 Abstract Introduction Conclusion References All Products Quick View Newly listed Tphysletters A Unifying Bag Model of Composite Fermionic Structures in a Cold Genesis Theory Regular Price $700.00 Sale Price $400.00 Excluding Sales Tax Quick View TphysicsLetters Detection of the large-scale tidal field with galaxy multiplet alignment in the Regular Price $1,900.00 Sale Price $950.00 Excluding Sales Tax Quick View Newly listed Tphysletters Violation of γ in Brans-Dicke gravity Regular Price $1,000.00 Sale Price $600.00 Excluding Sales Tax Quick View Astrophysics Observations and detectability of young Suns’ flaring and CME activity in optica Regular Price $1,000.00 Sale Price $450.00 Excluding Sales Tax Quick View TphysicsLetters Tunable structure-activity correlations of molybdenum dichalcogenides (MoX2; X=S Regular Price $2,000.00 Sale Price $400.00 Excluding Sales Tax Quick View New Thphysletters Bayesian and frequentist investigation of prior effects in EFTofLSS analyses of Regular Price $3,000.00 Sale Price $370.00 Excluding Sales Tax Quick View New Thphysletters A search for faint resolved galaxies beyond the Milky Way in DES Year 6: A new f Regular Price $1,900.00 Sale Price $750.00 Excluding Sales Tax Quick View New X-ray polarization properties of partially ionized equatorial obscurers around a Regular Price $800.00 Sale Price $350.00 Excluding Sales Tax Quick View New Unravelling multi-temperature dust populations in the dwarf galaxy Holmberg II Regular Price $1,200.00 Sale Price $400.00 Excluding Sales Tax Quick View New SpookyNet: Advancement in Quantum System Analysis through Convolutional Neural N Regular Price $1,500.00 Sale Price $500.00 Excluding Sales Tax Quick View New Rapid neutron star cooling triggered by accumulated dark matter Regular Price $1,500.00 Sale Price $500.00 Excluding Sales Tax Quick View Newly listed Tphysletters Searching for Radio Outflows from M31* with VLBI Observations Price $300.00 Excluding Sales Tax Quick View New Thphysletters Measurement of the scaling slope of compressible magnetohydrodynamic turbulence Regular Price $680.00 Sale Price $612.00 Excluding Sales Tax Quick View MAKE OPEN ACCESS New method to revisit the gravitational lensing analysis of the Bullet Cluster u Price $1,030.00 Excluding Sales Tax Quick View New Thphysletters New method to revisit the gravitational lensing analysis of the Bullet Cluster u Regular Price $599.00 Sale Price $359.40 Excluding Sales Tax Quick View New Nebular spectra from Type Ia supernova explosion models compared to JWST observa Regular Price $503.00 Sale Price $271.62 Excluding Sales Tax Quick View New Thphysletters The Nature of the 1 MeV-Gamma quantum in a Classic Interpretation of the Quantum Price $399.00 Excluding Sales Tax Quick View Exceptional Classifications of Non-Hermitian Systems Price $399.00 Excluding Sales Tax Quick View New Thphysletters On the occurrence of stellar fission in binary-driven hypernovae Price $399.00 Excluding Sales Tax Quick View New ApplSciLettersA AC frequency influence on pump temperature Price $399.00 Excluding Sales Tax Quick View New ApplSciLett. 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Theoretical Physics Letters HOME JOURNALS PRICING AND PLANS SUBMIT SPECIAL Tphysicsletters/vol-08/no-xx/Metabolic Potential versus Genome Size atanas.atanasov@univie.ac.at Monday, April 4, 2022 at 6:30:00 PM UTC Request Open Apply Now Locked 10.1490/8740064.780ptl Metabolic Potential versus Genome Size Atanas T. Atanasov1, Dimitar T. Valev2 ! Widget Didn’t Load Check your internet and refresh this page. If that doesn’t work, contact us. TOA Abstract Introduction Conclusion Unlock Only Changeover the Schrödinger Equation This option will drive you towards only the selected publication. If you want to save money then choose the full access plan from the right side. Unlock all Get access to entire database This option will unlock the entire database of us to you without any limitations for a specific time period. This offer is limited to 100000 clients if you make delay further, the offer slots will be booked soon. Afterwards, the prices will be 50% hiked. Buy Unlock us Newsletters ! 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Abstract Introduction Conclusion References All Products Quick View Newly listed Tphysletters A Unifying Bag Model of Composite Fermionic Structures in a Cold Genesis Theory Regular Price $700.00 Sale Price $400.00 Excluding Sales Tax Quick View TphysicsLetters Detection of the large-scale tidal field with galaxy multiplet alignment in the Regular Price $1,900.00 Sale Price $950.00 Excluding Sales Tax Quick View Newly listed Tphysletters Violation of γ in Brans-Dicke gravity Regular Price $1,000.00 Sale Price $600.00 Excluding Sales Tax Quick View Astrophysics Observations and detectability of young Suns’ flaring and CME activity in optica Regular Price $1,000.00 Sale Price $450.00 Excluding Sales Tax Quick View TphysicsLetters Tunable structure-activity correlations of molybdenum dichalcogenides (MoX2; X=S Regular Price $2,000.00 Sale Price $400.00 Excluding Sales Tax Quick View New Thphysletters Bayesian and frequentist investigation of prior effects in EFTofLSS analyses of Regular Price $3,000.00 Sale Price $370.00 Excluding Sales Tax Quick View New Thphysletters A search for faint resolved galaxies beyond the Milky Way in DES Year 6: A new f Regular Price $1,900.00 Sale Price $750.00 Excluding Sales Tax Quick View New X-ray polarization properties of partially ionized equatorial obscurers around a Regular Price $800.00 Sale Price $350.00 Excluding Sales Tax Quick View New Unravelling multi-temperature dust populations in the dwarf galaxy Holmberg II Regular Price $1,200.00 Sale Price $400.00 Excluding Sales Tax Quick View New SpookyNet: Advancement in Quantum System Analysis through Convolutional Neural N Regular Price $1,500.00 Sale Price $500.00 Excluding Sales Tax Quick View New Rapid neutron star cooling triggered by accumulated dark matter Regular Price $1,500.00 Sale Price $500.00 Excluding Sales Tax Quick View Newly listed Tphysletters Searching for Radio Outflows from M31* with VLBI Observations Price $300.00 Excluding Sales Tax Quick View New Thphysletters Measurement of the scaling slope of compressible magnetohydrodynamic turbulence Regular Price $680.00 Sale Price $612.00 Excluding Sales Tax Quick View MAKE OPEN ACCESS New method to revisit the gravitational lensing analysis of the Bullet Cluster u Price $1,030.00 Excluding Sales Tax Quick View New Thphysletters New method to revisit the gravitational lensing analysis of the Bullet Cluster u Regular Price $599.00 Sale Price $359.40 Excluding Sales Tax Quick View New Nebular spectra from Type Ia supernova explosion models compared to JWST observa Regular Price $503.00 Sale Price $271.62 Excluding Sales Tax Quick View New Thphysletters The Nature of the 1 MeV-Gamma quantum in a Classic Interpretation of the Quantum Price $399.00 Excluding Sales Tax Quick View Exceptional Classifications of Non-Hermitian Systems Price $399.00 Excluding Sales Tax Quick View New Thphysletters On the occurrence of stellar fission in binary-driven hypernovae Price $399.00 Excluding Sales Tax Quick View New ApplSciLettersA AC frequency influence on pump temperature Price $399.00 Excluding Sales Tax Quick View New ApplSciLett. 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Physics Tomorrow Material Science Letters publications. Download all open access papers form here. Share your feedback form the website about any published paper. Home PTL BOND Submission Central Browse Journals Program List More... Material Science Letters Publication archive Basic information Home Support About Email Submit your manucript Online submssion Email submission Impact factors Join as Editor Reviewer Extended indexing Science Citation (SCI) Scopus Submission is open Website is designed simply. Get anything from the search bar. PTL fellowship Best paper award Research sponsorship June submissions will be eligible for award and fellowship. Get is published earlier to apply for it later. Download Citation (0) © PTL OPEN April 17, 2021 at 6:20:33 AM Irreversible transformations of 3d lead(ii) coordination polymers via mechanochemistry; precursors for the preparation of lead(ii) chloride/bromide/sulfide nanoparticles Irreversible crystal-to-crystal transformations of 3D lead(II) coordination polymers with the ligand 1H-1,2,4- triazole-3-carboxylic acid (HL), from [Pb(L)(µ2-Cl)(H2O)]n (1) to [Pb(L)(µ2-Br)(H2O)]n (2) and [Pb(L)(µ1,1-NCS)(H2O)]n (3) by solid-state anion-replacement processes under mechanochemical reactions, have been studied. These irreversible solidstate structural transformations of compound 1 to compounds 2 and 3, have been verified by PXRD measurements. PbCl2, PbBr2 and PbS nanoparticles were obtained by thermal decomposition of compounds 1, 2 and 3 in oleic acid as surfactant at 200 °C under air atmosphere, respectively. Material Science Letters Keylines Introduction Coordination polymers are a class of materials composed of metals or metal clusters (the ‘‘node’’) coordinated to multi-functional organic ligands (the ‘‘linker’’) [1].During the last two decades, design and synthesis of novel metal–organic coordination polymers are attracting more attention, not only for their interesting molecular topologiesbut also for their potential applications as functional materials, ions exchange, catalysis, molecular recognition, nonlinear optics, molecular magnetic materials, electrical conductivity, separation and gas storage [2]. Solidstate crystal-to-crystal transformations involving coordination polymers induced by light, heat, guest removal, uptake or exchange, expansion of coordination numbers, oxidation of metal centers, condensation, or reactions between the ligands are very fascinating and one of the hot topics in solidstate chemistry [3]. Solid state reactions by manual or mechanical grinding solid reactants together with either no added solvent or only nominal amounts for molecular synthesis have triggered lots of attention.Mechanochemical synthesis, a burgeoning field in coordination polymers, has been utilized to synthesize various coordination polymers from the reactants without solvents [4]. Conclusion In summary, a3D lead(II) coordination polymer [Pb(L)(µ2- Cl)(H2O)]n (1) polymerize on grinding the solid with KBr and KSCN to form the 3D coordination polymers, [Pb(L)(µ2-Br)(H2O)]n (2) and [Pb(L)(µ1,1-NCS)(H2O)]n(3), respectively. PbCl2, PbBr2 and cubic-shaped PbS nanoparticles were obtained by thermolysis of compounds 1, 2 and 3 in oleic acid as surfactant at 200 °C under air atmosphere, respectively. References [1]. M.-L. Hu, A. Morsali and L. Aboutorabi, Coord. Chem. Rev. 255, 2821(2011) [2]. M. J. Zaworotko, New J. Chem.34,2355 (2010). [3]. M. Nagarathinam, A. Chanthapally, S. H. Lapidus, P. W. Stephens and J. J. Vittal, Chem. Commun. 48, 2585(2012). [4]. S. L. James, C. J. Adams, C. Bolm, D. Braga, P. Collier, T. Friscic, F. Grepioni, K. D. M. Harris, G. Hyett, W. Jones, A. Krebs, J. Mack, L. Maini, A. G. Orpen, I. P. Parkin, W. C. Shearouse, J. W. Steed and D. C. Waddell, Chem. Soc. Rev. 41, 413 (2012). Submit a manuscript

Physics Tomorrow Material Science Letters publications. Download all open access papers form here. Share your feedback form the website about any published paper. Home PTL BOND Submission Central Browse Journals Program List More... Material Science Letters Publication archive Basic information Home Support About Email Submit your manucript Online submssion Email submission Impact factors Join as Editor Reviewer Extended indexing Science Citation (SCI) Scopus Submission is open Website is designed simply. Get anything from the search bar. PTL fellowship Best paper award Research sponsorship June submissions will be eligible for award and fellowship. Get is published earlier to apply for it later. Download Citation (0) © PTL OPEN April 17, 2021 at 4:20:17 AM Design Analysis of Low-Pressure Acetylene Generators used in Chhattisgarh State The Low-Pressure Acetylene Generators used calcium carbide to generate Acetylene gas. The generated low-pressure Acetylene is used with an oxygen cylinder extensively by Gas welders in Chhattisgarh state for oxy acetylene welding. This low-pressure oxy acetylene welding is used mostly in automobile body repairing work. In this research paper mainly four types of popular generators are used to study for producing low-pressure Acetylene. The design construction and working of these lookalike generators are similar but their capacities and safety to hold the Acetylene gas are different. These generators are selected by the gas welders as per the experience and skill developed by them. The safety features in these low-pressure acetylene generators are rarely followed by the gas welders in the state. These Lowpressure Acetylene generators are preferred over the Acetylene cylinder due to low-cost Acetylene generation. In this research paper with help of CAD modeling these four popular Acetylene generators design and the capacity of each generator are calculated. In these four types of low-pressure acetylene generation, prefabricated generators are found safest to operate and the Top charged Acetylene Generator is found unsafe and required very high skill of operation. These design analysis study of these popular models will certainly help to standardize the dimensions of the Acetylene generators for their safe working. Material Science Letters Keylines Introduction The Acetylene generators are used along with oxygen cylinders to weld and repair automobiles quit extensively in Chhattisgarh state. These generators are used Calcium Carbide with water to produce the Acetylene gas. This type of welding is considered as low pressure welding where welding pressure is required only 0.1 bar [1]. This type of Acetylene generation is used with Oxygen in auto body minor repairing [2]. Other than automotive repair low pressure gas welding is also used for joining of thin ferrous and non ferrous materials, air craft industries and sheet metal, fabrication plant [3]. Generally 16 gauges to 22 gauges mild steel sheets are welded using theses generators [2]. The dimensions of all the popular generators are gathered from the 11 District of Chhattisgarh. They are Raipur, Durg, Rajnadgaon, Balod, Dhamtari, Kanker, Kondagaon, Jagadalpur, Sukma, Dantewada, Bijapur and Narayanpur. As per BIS (Bureau of Indian Standards) SP: 12-1975 Handbook of Gas Welders the Low pressure Acetylene generators are divided as Water to Carbide and Carbide to Water [4]. But these classification are little confusing to exactly naming the generators. These generators can be clearly classified further as [5]- 1. Pre-fabricated Acetylene generators. 2. Fabricated Acetylene generators. A) Open Dome type B) Submerged Dome type C) Top charging type There are few more popular models are used in these classification. But the Analysis is done on only those which can hold the maximum calcium carbide (CaC2). Almost all the generators are made with mild steel sheet of 16 gauges (1.5189 mm). Conclusion References Submit a manuscript

Theoretical Physics Letters HOME JOURNALS PRICING AND PLANS SUBMIT Locked Tphysicsletters/6981/11/1490/874831tpl/Probing supermassive black hole seed scenarios with gravitational wave measurements Citation (0) Wednesday, December 6, 2023 at 12:15:00 PM UTC Request Open Apply Now Article Rating by Publisher 10 Astrophysics Article Rating by Readers 10 https://doi.wikipt.org/11/1490/874831tpl Probing supermassive black hole seed scenarios with gravitational wave measurements John Ellis,1, 2, 3, ∗ Malcolm Fairbairn,1, † Juan Urrutia,3, 4, ‡ and Ville Vaskonen3, 5, 6, § 1King’s College London, Strand, London, WC2R 2LS, United Kingdom 2Theoretical Physics Department, CERN, Geneva, Switzerland 3Keemilise ja Bioloogilise F¨u¨usika Instituut, R¨avala pst. 10, 10143 Tallinn, Estonia 4Department of Cybernetics, Tallinn University of Technology, Akadeemia tee 21, 12618 Tallinn, Estonia 5Dipartimento di Fisica e Astronomia, Universit`a degli Studi di Padova, Via Marzolo 8, 35131 Padova, Italy 6Istituto Nazionale di Fisica Nucleare, Sezione di Padova, Via Marzolo 8, 35131 Padova, Italy Theoretical Physics Letters 2023 ° 18(06) ° 0631-3657 https://www.wikipt.org/tphysicsletters DOI : https://doi.wikipt.org/11/1490/874831tpl TOA Abstract Introduction Conclusion ACKNOWLEDGMENTS The work of J.E. was supported by the United Kingdom STFC Grants ST/X000753/1 and ST/T00679X/1, and that of M.F. was also supported by the United Kingdom STFC Grant ST/X000753/1. The work of J.U. and V.V. was supported by European Regional Development Fund through the CoE program grant TK133 and by the Estonian Research Council grant PRG803. The work of V.V. was also partially supported by the European Union’s Horizon Europe research and innovation program under the Marie Sk lodowska-Curie grant agreement No. 101065736. Unlock Only Changeover the Schrödinger Equation This option will drive you towards only the selected publication. If you want to save money then choose the full access plan from the right side. Unlock all Get access to entire database This option will unlock the entire database of us to you without any limitations for a specific time period. This offer is limited to 100000 clients if you make delay further, the offer slots will be booked soon. Afterwards, the prices will be 50% hiked. Buy Unlock us Newsletters Abstract The process whereby the supermassive black holes populating the centers of galaxies have been assembled remains to be established, with the relative importance of seeds provided by collapsed Population-III stars, black holes formed in nuclear star clusters via repeated mergers, or direct collapses of protogalactic disks yet to be determined. In this paper we study the prospects for casting light on this issue by future measurements of gravitational waves emitted during the inspirals and mergers of pairs of intermediate-mass black holes, discussing in particular the roles of prospective measurements by LISA and the proposed atom interferometers AION and AEDGE. We find that, the expected number of detectable IMBH binaries is O(100) for LISA and AEDGE and O(10) for AION in low-mass seeds scenarios and goes down to O(10) for LISA and below one for AEDGE and AION in high-mass seed scenarios. This allows all of these observatories to probe the parameters of the seed model, in particular if at least a fraction of the SMBHs arise from a low-mass seed population. We also show that the measurement accuracy of the binary parameters is, in general, best for AEDGE that sees very precisely the merger of the binary. Introduction Most galaxies contain supermassive black holes (SMBHs) heavier than 106M⊙ [1], and the existence of black holes (BHs) with masses between a few and ∼ 80M⊙ has been established by observations of X-ray binaries [2] and by the measurements of gravitational waves (GWs) with frequencies ∼ 100 Hz emitted during their mergers [3–5]. Various other observations point to the existence of intermediate-mass black holes (IMBHs) with masses in the range 104 − 106M⊙, but their mass function and redshift distribution is known only very poorly [6]. This lack of information about IMBHs impedes our understanding of how SMBHs have been assembled [7]. The main possibilities for seeding SMBH assembly include collapsed Population-III stars [8], BHs formed in nuclear star clusters via repeated mergers [9–11] or direct collapses of protogalactic disks in which fragmentation is suppressed [12–18]. All of these mechanisms are capable of reproducing the properties of the observed SMBH population for suitable values of assembly parameters such as accretion rates, but can differ significantly in their predictions for the spectrum of IMBH mergers at different redshifts, see [19] for an overview. Signatures of these mechanisms may include either light seeds, with masses ∼ 102 − 103M⊙ or heavy seeds, with masses ∼ 104 − 105M⊙, at z ≲ 10. These are currently unconstrained by data, but can in principle be probed by future GW and other measurements [20–26]. The purpose of this paper is to investigate what progress can be made in distinguishing between the SMBH assembly scenarios with planned future GW experiments in light of recent data on nHz GWs from pulsar timing array (PTA) experiments, highlighting the potential capabilities of atom interferometers. NANOGrav [27] and other PTA experiments [28–30] have recently reported the observation of a stochastic background of GWs at frequencies in the nHz range, for which the most conservative astrophysical interpretation is that binary systems of SMBHs are emitting them with masses ∼ 109M⊙ [31–34]. Naive extrapolation of binary merger models to lower BH masses suggests that GWs from IMBH binaries may be observable at higher frequencies between 10−5 Hz and 1 Hz, for example by the LISA space-borne laser interferometer experiment or atom interferometer experiments [35]. In principle, there are two regimes where the formation channels of the SMBHs may be distinguished. Either at z ≳ 7 when the seeds are assembling and scaling relations are not that strong [36, 37], or by observing the low mass occupation fraction of dwarf galaxies and dark matter halos at more recent times [19, 38]. The extrapolation to higher frequencies of a model that can fit the NANOGrav background [34] predicts that the majority of detectable binaries will be at z < 7, so the focus of this study is to constrain the latter. Our work complements analogous studies that have been performed with electromagnetic observations of active galactic nuclei (AGNs) [39–42]. Read more articles. Unravelling multi-temperature dust populations in the dwarf galaxy Holmberg II Buy Now Searching for Radio Outflows from M31* with VLBI Observations Buy Now A search for faint resolved galaxies beyond the Milky Way in DES Year 6: A new f Buy Now Conclusion We have described in this paper the capabilities of the planned space-borne laser interferometer LISA and the proposed atom interferometers AEDGE and AION-1km to observe mergers of intermediate-mass BHs, measure their parameters, and discriminate between different seed scenarios for the assembly of SMBHs. We have considered the extended Press-Schechter to model the coalescences of galactic halos and estimate a rate for mergers of SMBHs that is compatible with the PTA signals for GWs in the nHz range. We have extrapolated this model to different SMBH seed scenarios by parametrizing the low mass cutoff of the massive BH population. Using this parametrization, we have estimated the possible rates for IMBH mergers, and assessed their detectability and measurability. We have found that, although LISA has a high rate for observing the early infall stages of IMBH binaries for all the masses studied, this detector loses many binaries as the merger time approaches. Both AEDGE and AION-1km have higher rates than LISA for detections within one minute of the merger. We have shown that AEDGE has the best perspectives for detecting mergers of IMBHs weighing ≲ 104M⊙ whereas LISA has better perspectives for IMBHs weighing ≳ 105M⊙. The better detection rates translate into smaller uncertainties in the measurements by AEDGE of binary parameters for IMBHs weighing ≲ 105M⊙. We have estimated the accuracy with which a lower cutoff on the BH seed mass, mcut could be extracted from the prospective GW data. We find that both LISA and AEDGE could determine mcut with precision ≲ 20% if mcut ≲ 104M⊙, whereas LISA could determine mcut with better precision than AEDGE if mcut ≳ 104M⊙. We also find that both LISA and AEDGE have interesting capabilities for distinguishing between scenarios with different mixtures of seeds with 102 and 105M⊙. AION1km could also provide some information, particularly in scenarios with a population of low-mass seeds. Our results indicate that the space-borne laser interferometer LISA and atom interferometers AEDGE and AION-1km have interesting and complementary capabilities for measuring IMBH mergers and distinguishing between different seed scenarios for the assembly of SMBHs. We should emphasize that our study has been exploratory and should be complemented by an improved modelling of the SMBH seed scenarios and more detailed studies of the instrumental capabilities of GW interferometers. It would also be interesting to extend the analysis to assess the prospects for multimessenger observations and study the prospects for measuring higher-order multipoles of the GW signals that would allow for example for new probes of strong gravity. TOC (TphysicsLetters) TOC (TphysicsLetters) The Nature of the 1 MeV-Gamma Quantum in a Classic Interpretation of the Quantum Nebular spectra from Type Ia supernov Physics Tomorrow TOC HIGHLIGHTS 2023 TOC HIGHLIGHTS 2023 Theoretical Physics Letters Physics Tomorrow ZZ Ceti stars of the southern ecliptic hemisphere re-observed by TESS ZZ Ceti stars of the southern ecliptic hemisphere re-observed by TESS Physics Tomorrow References [1] J. Kormendy and L. C. Ho, Ann. Rev. Astron. Astrophys. 51, 511 (2013), arXiv:1304.7762 [ astro-ph.CO ]. [2] R. A. Remillard and J. E. McClintock, Ann. Rev. Astron. Astrophys. 44, 49 (2006), arXiv:astro-ph/0606352. [3] B. P. Abbott et al. (LIGO Scientific, Virgo), Phys. Rev. X 9, 031040 (2019), arXiv:1811.12907 [astro-ph.HE]. [4] R. Abbott et al. (LIGO Scientific, Virgo), Phys. Rev. X 11, 021053 (2021), arXiv:2010.14527 [gr-qc]. [5] R. Abbott et al. (LIGO Scientific, Virgo and KAGRA Collaborations), (2021), arXiv:2111.03634 [astroph.HE]. [6] J. E. Greene, J. Strader, and L. C. Ho, Ann. Rev. Astron. Astrophys. 58, 257 (2020), arXiv:1911.09678 [ astroph.GA ]. [7] A. E. Reines, Nature Astron. 6, 26 (2022), arXiv:2201.10569 [ astro-ph.GA ]. [8] V. Bromm and A. Loeb, Astrophys. J. 596, 34 (2003), arXiv:astro-ph/0212400. [9] S. F. Portegies Zwart, H. Baumgardt, P. Hut, J. Makino, and S. L. W. McMillan, Nature 428, 724 (2004), arXiv:astro-ph/0402622. [10] M. Atakan Gurkan, M. Freitag, and F. A. Rasio, Astrophys. J. 604, 632 (2004), arXiv:astro-ph/0308449. [11] P. Natarajan, Mon. Not. Roy. Astron. Soc. 501, 1413 (2021), arXiv:2009.09156 [ astro-ph.GA ]. [12] A. Sesana, F. Haardt, P. Madau, and M. Volonteri, Astrophys. J. 611, 623 (2004), arXiv:astro-ph/0401543. [13] M. C. Begelman, M. Volonteri, and M. J. Rees, Mon. Not. Roy. Astron. Soc. 370, 289 (2006), arXiv:astroph/0602363. [14] M. Volonteri, G. Lodato, and P. Natarajan, Mon. Not. Roy. Astron. Soc. 383, 1079 (2008), arXiv:0709.0529 [astro-ph]. [15] L. Mayer, S. Kazantzidis, P. Madau, M. Colpi, T. R. Quinn, and J. Wadsley, Science 316, 1874 (2007), arXiv:0706.1562 [astro-ph]. [16] T. L. Tanaka and M. Li, Mon. Not. Roy. Astron. Soc. 439, 1092 (2014), arXiv:1310.0859 [ astro-ph.CO ]. [17] K. Inayoshi, E. Visbal, and K. Kashiyama, Mon. Not. Roy. Astron. Soc. 453, 1692 (2015), arXiv:1504.00676 [ astro-ph.GA ]. [18] D. Izquierdo-Villalba, M. Colpi, M. Volonteri, D. Spinoso, S. Bonoli, and A. Sesana, Astron. Astrophys. 677, A123 (2023), arXiv:2305.16410 [ astro-ph.GA ]. [19] M. Volonteri, M. Habouzit, and M. Colpi, Nature Rev. Phys. 3, 732 (2021), arXiv:2110.10175 [ astro-ph.GA ]. [20] A. Sesana, J. Gair, E. Berti, and M. Volonteri, Phys. Rev. D 83, 044036 (2011), arXiv:1011.5893 [ astroph.CO ]. [21] T. Hartwig, M. Volonteri, V. Bromm, R. S. Klessen, E. Barausse, M. Magg, and A. Stacy, Mon. Not. Roy. Astron. Soc. 460, L74 (2016), arXiv:1603.05655 [ astroph.GA ]. [22] J. H. Krolik, M. Volonteri, Y. Dubois, and J. Devriendt, Astrophys. J. 879, 110 (2019), arXiv:1905.10450 [ astroph.GA ]. Buy this article to read full length. Abstract Introduction Conclusion References All Products Quick View Newly listed Tphysletters A Unifying Bag Model of Composite Fermionic Structures in a Cold Genesis Theory Regular Price $700.00 Sale Price $400.00 Excluding Sales Tax Quick View TphysicsLetters Detection of the large-scale tidal field with galaxy multiplet alignment in the Regular Price $1,900.00 Sale Price $950.00 Excluding Sales Tax Quick View Newly listed Tphysletters Violation of γ in Brans-Dicke gravity Regular Price $1,000.00 Sale Price $600.00 Excluding Sales Tax Quick View Astrophysics Observations and detectability of young Suns’ flaring and CME activity in optica Regular Price $1,000.00 Sale Price $450.00 Excluding Sales Tax Quick View TphysicsLetters Tunable structure-activity correlations of molybdenum dichalcogenides (MoX2; X=S Regular Price $2,000.00 Sale Price $400.00 Excluding Sales Tax Quick View New Thphysletters Bayesian and frequentist investigation of prior effects in EFTofLSS analyses of Regular Price $3,000.00 Sale Price $370.00 Excluding Sales Tax Quick View New Thphysletters A search for faint resolved galaxies beyond the Milky Way in DES Year 6: A new f Regular Price $1,900.00 Sale Price $750.00 Excluding Sales Tax Quick View New X-ray polarization properties of partially ionized equatorial obscurers around a Regular Price $800.00 Sale Price $350.00 Excluding Sales Tax Quick View New Unravelling multi-temperature dust populations in the dwarf galaxy Holmberg II Regular Price $1,200.00 Sale Price $400.00 Excluding Sales Tax Quick View New SpookyNet: Advancement in Quantum System Analysis through Convolutional Neural N Regular Price $1,500.00 Sale Price $500.00 Excluding Sales Tax Quick View New Rapid neutron star cooling triggered by accumulated dark matter Regular Price $1,500.00 Sale Price $500.00 Excluding Sales Tax Quick View Newly listed Tphysletters Searching for Radio Outflows from M31* with VLBI Observations Price $300.00 Excluding Sales Tax Quick View New Thphysletters Measurement of the scaling slope of compressible magnetohydrodynamic turbulence Regular Price $680.00 Sale Price $612.00 Excluding Sales Tax Quick View MAKE OPEN ACCESS New method to revisit the gravitational lensing analysis of the Bullet Cluster u Price $1,030.00 Excluding Sales Tax Quick View New Thphysletters New method to revisit the gravitational lensing analysis of the Bullet Cluster u Regular Price $599.00 Sale Price $359.40 Excluding Sales Tax Quick View New Nebular spectra from Type Ia supernova explosion models compared to JWST observa Regular Price $503.00 Sale Price $271.62 Excluding Sales Tax Quick View New Thphysletters The Nature of the 1 MeV-Gamma quantum in a Classic Interpretation of the Quantum Price $399.00 Excluding Sales Tax Quick View Exceptional Classifications of Non-Hermitian Systems Price $399.00 Excluding Sales Tax Quick View New Thphysletters On the occurrence of stellar fission in binary-driven hypernovae Price $399.00 Excluding Sales Tax Quick View New ApplSciLettersA AC frequency influence on pump temperature Price $399.00 Excluding Sales Tax Quick View New ApplSciLett. 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Theoretical Physics Letters HOME JOURNALS PRICING AND PLANS SUBMIT Premium Tphysicsletters/6981/11/1490/77009901.265tpl/A Unifying Bag Model of Composite Fermionic Structures in a Cold Genesis Theory of Particles Citation (0) Premium Thursday, November 28, 2024 at 6:30:00 AM UTC Request Open Apply Now Article Rating by Publisher 8.7 T. Physics Article Rating by Readers 10 Locked 10.1490/77009901.265tpl A Unifying Bag Model of Composite Fermionic Structures in a Cold Genesis Theory of Particles Arghirescu Marius Theoretical Physics Letters 2024 ° 28(11) ° 11-12 https://www.wikipt.org/tphysicsletters DOI: 10.1490/77009901.265tpl TOA Abstract Introduction Conclusion Unlock Only Changeover the Schrödinger Equation This option will drive you towards only the selected publication. If you want to save money then choose the full access plan from the right side. Unlock all Get access to entire database This option will unlock the entire database of us to you without any limitations for a specific time period. This offer is limited to 100000 clients if you make delay further, the offer slots will be booked soon. Afterwards, the prices will be 50% hiked. Buy Unlock us Newsletters Abstract The paper presents a better calculation of the constants and d of the CGT’s unifying bag model, previously published, which explains the strong interaction and the nuclear force without the concept of ‚color charge’ specific to the Standard Model. The recalculation indicates that the pressure of internal ‚naked’ photons on the bag’s surface of radius ai = 0.59, which explains the nucleon's quarks deconfining temperature (~2x1012 K), for a current quark's radius of ordinary nuclear temperature: rq = 0.2 fm, is: Psi0(ai) = 6.688x1033 N/m2, corresponding to a ,bag' constant: Bi l= 41.8 MeV/fm3, value which verify the CGT's model of strong ' interaction between quarks and that between nucleons considered in a vortical model, by a constant of the bag's field variation of value: d = 0.34 fm. The total potential of interaction between two nucleons results in the form of a modified Sombrero-type potential, with an attractive part Va(r) = Va0×e-r/h* and a repulsive part: Vr(r) = Vr0×e-7r/h*, (h* = 0.8 fm). The explanatory model indicates the existence of a bag pressure for each composite particle but also for quarks and the bag’s constant variation with the mass and the intrinsic temperature of the particle’s kernel. Introduction The necessity to explain unitary the strong interaction between quarks and their confining and the nuclear force, that generates the nucleons’ confining in quasi-liquid or solid nuclei, is obvious. In the Standard Model of particles, this aim is fulfilled by the concept of ‘color charge’ of current quarks and by the mechanism of interaction by intermediary ‘gluons’ formed as pairs of virtual current quarks and antiquarks, the nuclear force of interaction between nucleons being explained by an exchange of residual gluons (short lived mesons). But compared to the Electrodynamics- which evidenced a real existence of the electric charge, in the Quantum Chromodynamics the real existence of the considered ‘color charge’ is not proved or strongly argued. In a Cold genesis theory of particles [1] , [2] , based on the Galilean relativity, the strong force of quarks confining and the nuclear force were explained by a (multi)vortical model of nucleon, considered as cluster of an even number Np = 1836/0.8095 = 2268 quasielectrons, (integer number of degenerate “gammons”, g*(e*- e*+)), i.e. electrons with degenerate charge (e* = ±(2/3)e), magnetic moment m* and mass: me* = 0.8095 me, resulting by a degeneration of the magnetic moment’s quantum vortex Gm = GA +GB , given by ‘heavy’ etherons of mass ms » 10-60kg and ‘quantons’ of mass mh = h×1/c2 = 7.37x10-51 kg. The considered “gammons” were experimentally observed in the form of quanta of “un-matter” plasma, [3] . The me* -value results in CGT by the conclusion that the difference between the masses of neutron and proton: (mn -mp » 2.62 me) is given by an incorporate electron with degenerate magnetic moment and a linking ‘gammon’ se (g*) = 2me* » 1.62 me , forming a ‘weson’, w- = (se (g*) + e-), which explains the neutron in a dynamide model of Lenard- Radulescu type [1] , [2] , ( protonic center and a negatron revolving around it by the Gm -vortex with the speed ve* << c, at a distance re* » 1.36 fm [2] - close to the value of the nucleon’s scalar radius: r0 »1.25 fm used by the formula of nuclear radius: Rn » r0×A1/3), at which it has a degenerate meS -magnetic moment and Sen –spin. The used electron model [1] supposes an exponential variation of its density: re(r) =re0e-r/h, (re0 = 22.24x1013 kg/m3) given by photons of inertial mass mf , vortically attracted around a dense kernel m0 and confined in a volume of classic radius a = 1.41 fm, (the e-charge in electron’s surface), the superposition of the (Np+1) quantonic vortices Gm* of the protonic quasielectrons, generating a total dynamic pressure: Pµ(r) = (1/2)rµ(r)×c2 £ (1/2)rn(r)×c2= Pn(r), inside a volume with radius: da = 2.1 fm, (conform to the superposition principle of quantum mechanics) which gives an exponential nuclear potential: Vn(r) = -uiPµ(r) of eulerian form, conform to : Vn(r) = uiPµ(r) = Vn0×e-r/h* ; Vn0 = -uiPµ0 , (1) with: h* = 0.8 fm (equal to the root-mean-square radius of the magnetic moment’s density variation inside a neutron, experimentally determined) and ui(rpi =0.586fm) » 0.843fm3 - the ‘impenetrable’ volume of nuclear interaction [1] , [2] , the proton resulting as formed by Np » 2268 paired quasi-electrons which give a proton’s apparent density in its center (by the sum rule), of value: rno » fc×Np×reo = 4.54x1017kg/m3, (re0 = 22.24 x1013 kg/m3 ), and an attached positron with degenerate magnetic moment, in the CGT’s model, the density of the Gm -vortex of a free electron having approximately the same density’ variation as the density of photons of its classic volume (of radius a = 1.41 fm), f ≈ 0.9 being a coefficient of mass’ and Gm -vortex’s density reducing in the center of the (quasi)electron at its mass degeneration, its value resulting by the gauge relation of CGT: e = 4pa2/k1 and by the integral of nucleon’s mass –considered as given by confined photons, with a density variation: rn(r) = rn0(0).e-r/h’ with h’ = 0.87 fm, (equal to the proton’s root-mean square charge radius, experimentally determined: 0.84 ¸0.87 fm). The variation of rµ(r) is similar to that of rn(r) because it is given mainly by the vorticity of the photons with mass mf >> mh = h1/c2 which give the main part of the nucleon’s mass, (the mass of the bosonic shell of nucleon’s kerneloid), conform to CGT. The radius rpi of the ‘impenetrable’ quantum volume ui corresponding to the nuclear interaction results in CGT as quasi-equal to the radius of the proton’s magnetic moment: rpi » rmp = 0.586 fm, given by the relation mp = 2.79mN = ½ecrm , (Þrmp/rme = mp/me , with: rme = (h/2pmec) » 386fm; mN- the nuclear magneton) and corresponding in CGT to the maximal speed, c, of the quantons in the Gm -vortex of the magnetic moment mp, without the photonic shell of the nucleon’s kerneloid Read more related articles Dirac-Majorana neutrino type conversion induced by an oscillating scalar dark ma Buy Now Solve the Maxwell’s equations and Schrodinger’s equation but avoiding the Sommer Buy Now X-ray polarization properties of partially ionized equatorial obscurers around a Buy Now Conclusion The paper shows that the recalculation of the constants Psi0 and d of the CGT’s bag model, previously published, which for a ‚bag’s radius: ai » 0.59 fm gives: Psi0(ai) = 6.688x1033 N/m2, corresponding to a ‚bag’ constant: Bi » 41.8 MeV/fm3, verify the both CGT’s models: of strong interaction between quarks and the interaction between nucleons, based on the (multi)vortical model of nucleon, by a constant of the bag’s field variation of value: d » 0.34 fm, the explanatory model resulting as unitary, without the need of (semi)formal concepts such as the concept of ‚color charge’ used by the Standard Model of Quantum Mechanics. The resulting explanatory model of CGT is important because –in a Galilean relativity, the mechanism of paired quarks forming from relativist jets of negatron and positron, experimentally evidenced [21] , is explained by the forming of compact clusters of degenerated negatron-positron pairs, (of paired quasi-electrons), corresponding to z0-preons, in CGT [1] , and not by the total energy 2me(v)c2 of a single pair of relativist electrons entered in mutual collision, as in the Standard Model, so in this case the forming of the supposed ‘color charges’ of the formed quarks is not explained. Compared to the value B » 58MeV/fm3 = 9.28x1033 N/m2 obtained by the MIT bag model [6] , the lower value Bi » 41.8 MeV/fm3 » 6.69x1033 N/m2 obtained in CGT indicates –by the static equilibrium relation of stellar structures which- in a classic (non-relativist) case, is given by: dP(r)/dr=-r(r)×g(r); (g(r)=G×m(r)/r2), (28) and by an equation of state (EoS) of the internal pressure: P(r) = (SPf –B) with Pf -–pressure due to each quark flavor (u; d; s ), that the TOV limit ’ (Tolman–Oppenheimer–Volkoff, [22] ; [23] ) of the neutron stars’ mass is higher than the superior limit of ~3 solar masses [24] obtained by the B-constant of the MIT’ bag model (~58 MeV/fm3 ). The fact that the shell of the valence (current) quarks is given in CGT by thermalized ‘naked’ photons –instead of gluons as in the S.M., is argued by the possibility to obtain paired quarks from relativist jets of negatrons and positrons (i.e. by the CGT’s model of meson and of baryon) and by the fact that when the internal quark structure of the proton is revealed by deeply virtual Compton scattering [25] (a process in which electrons are scattered off quarks inside the protons), the internal quarks subsequently emit high-energy photons, which are detected in coincidence with the scattered electrons and with the recoil protons. Even if it was concluded –by the Standard Model of particles, that although the basic bag model does not provide a pion-mediated interaction it describes excellently the nucleon–nucleon forces through the 6 quark bag s-channel mechanism using the P-matrix [26] , it results –conform to the observations presented in Chpt. 2, that the value of the current u/d-quark’s radius: rq· = 0.43x10-3 fm –actually considered by the S.M. , is not compatible with the possibility to explain the quarks’ confining without the concept of ‘color charge’ used in Quantum Chromodynamics. Also, it is recognized that a consistent theory of the nuclear force, based upon the interaction of quarks and gluons, does not yet exist [27] , [28] , [29] , [30] . The total potential of interaction between two nucleons results in the form of a modified Sombrero-type potential, with an attractive part and a repulsive part: Vr(r) = Vr0×e-7r/h* -explained in CGT by intrinsic vibrations of the particle’s kernel produced by its current quarks, without the hypothesis of a mediating quantum- considered in the Standard Model as being an isoscalar vector meson omega [31] . The explanatory model indicates the existence of a bag pressure (and a bag constant) for each composite particle but also for quarks and the bag’s constant variation with the intrinsic temperature of the particle’s kernel. The possible implications in astrophysics are related to the structure and the density of the quark stars and of the cold stars of ‚black hole’ type. TOC (TphysicsLetters) TOC (TphysicsLetters) The Nature of the 1 MeV-Gamma Quantum in a Classic Interpretation of the Quantum Nebular spectra from Type Ia supernov Physics Tomorrow TOC HIGHLIGHTS 2023 TOC HIGHLIGHTS 2023 Theoretical Physics Letters Physics Tomorrow ZZ Ceti stars of the southern ecliptic hemisphere re-observed by TESS ZZ Ceti stars of the southern ecliptic hemisphere re-observed by TESS Physics Tomorrow References [1] Arghirescu, M., “The Cold Genesis of Matter and Fields”, Science PG, (2015). viXra:1104.0043 [2] Arghirescu M., “A preonic quasi-crystal quark model based on a cold genesis theory and on the experimentally evidenced neutral boson of 34 me”, Global J. of Phys., 5 (1): (2016) 496-504 [3] Sarri G., Poder K., Cole J., et al., „Generation of neutral and high-density electron– positron pair plasmas in the laboratory”, Nature Comm. , 6:6747, 23 April (2015). [4] Islam, M. M., Luddy R. J. (2013) „High Energy Elastic Scattering in Condensate Enclosed Chiral Bag Model and TOTEM Elastic Measurements at LHC at 7 TeV”, Talk presented at the EDS Blois, Sept. 9-13, 2013 [5] Harsha, S., "The tightly bound nuclei in the liquid drop model". European Journal of Physics. 39 (3): (2018) 035802. arXiv : 1709.01386 [6] A. Chodos, R.L. Jaffe, K. Johnson, C. B. Thorn, V. F. Weisskopf, New extended model of hadrons, Phys. Rev. D9 (1974) 3471 [7] Arghirescu M. “The nuclear force explaining by a bag model resulted from a vortexial, cold genesis model of nucleon”, Phys. Astron. Int. J. 2(4): (2018) 349‒358 [8] R. Jastrow, Phys. Review, 81 (1951) 165. [9] Yan, Y., Tegen, R.‚ ‟N-N Scattering and Nucleon Quark core‟, Science Asia, 27 (2001) 251 [10] F. Karsch, E. Laermann, A. Peikert, Nucl. Phys. B 605, (2001) 579 [11] Arghirescu, M., ‚The Density and the Structure of a Bare Quark Star in a Cold Genesis Theory of Particles’,J. of High Energy Phys., Gravitation & Cosmology, Vol.10, No.4 (2024) [12] Johnson, K. ‘The M.I.T. Bag Model’, Acta Phys. Polonica Vol. B6 No.6 (1975) 865-893, [13] Milonni P.W., “The Quantum Vacuum-An Introduction to Quantum Electrodynamics”, Ed. Academic, N. Y. (1994) [14] P. W. Higgs, “Broken Symmetries and the Masses of Gauge Bosons”, Phys. Rev. Lett. 13, (1964) 508-509 [15] Flügge S. ‚Practical Quantum Mechanics’, Ed. Springer-Verlag, New York, 1 (1974) 180-181 [16] Reid, R. V., "Local phenomenological nucleon–nucleon potentials". Annals of Physics. 50 (3): (1968) 411–448 [17] Yndurain, F., "Limits on the mass of the gluon". Phys. Lett. B . 345 (4): (1995) 524 [18] Plekhanov,V.G., „Hadron - Lepton Strong Interaction”, Services for Science and Education Stockport, Cheshire, SK4 2BT, U. K., (2020) p. 25; [19] Iancu, E., Venugopalan, R., in QGP3, Eds. R.C. Hwa, X.N.Wang , World Scientific (2003). arXiv:hep-ph/0303204; [20] McLerran, L., A Brief Introduction to the Color Glass Condensate and the Glasma’, Int. Symp. of Multiparticle Dynamics , Sep. 15-20, DESY, Hamburg, (2008). [21] Marshall, R. “The Pair Production of Quarks”, Phys. Bl. 53 No. 7/8, (1997), p.685-688 [22] Tolman, R. C. „Static Solutions of Einstein's Field Equations for Spheres of Fluid”, Phys. Rev. 55: (1939) 364 [23] Oppenheimer, J.R., Volkoff, G.M. "On Massive Neutron Cores". Phys. Rev. 55 (4): (1939) 374–381. [24] Bombaci, I. The Maximum Mass of a Neutron Star. Astron.& Astrophys . 305: (1996) 871–877 [25] Ji, X. D., Deeply virtual Compton scattering. Phys. Rev. D 55, (1997) 7114–7125 [26] Simonov, Yu. A. The quark compound bag model and the Jaffe-Low P-matrix. Phys. Lett. B . 107 (1981) 1–2. [27] E.M. Henley and A. Garcia, Subatomic Physics, 3rd Edn., World Scientific, Singapore, (2007). [28] K.S. Krane, Introductory Nuclear Physics, Ed. Wiley, New York - Chichester, (1988). [29] B.R. Martin, Nuclear and Particle Physics, Ed. J. Wiley & Sons, Weinheim, Chichester, (2006). [30] V.G. Plekhanov, ‘Modern View of the Origin of Isotope Effect , LAP, LAMBERT 35 Academic Publishing, Saarbrücken, Germany, (2018). [31] Reinhard, A., Reinhardt , H., Weigel , H., Zuckert, U., The Isoscalar vector meson omega in the Nambu-Jona-Lasinio soliton, Phys.Lett.B 298 (1992) 132-140 Abstract Introduction Conclusion References All Products Quick View Newly listed Tphysletters A Unifying Bag Model of Composite Fermionic Structures in a Cold Genesis Theory Regular Price $700.00 Sale Price $400.00 Excluding Sales Tax Quick View TphysicsLetters Detection of the large-scale tidal field with galaxy multiplet alignment in the Regular Price $1,900.00 Sale Price $950.00 Excluding Sales Tax Quick View Newly listed Tphysletters Violation of γ in Brans-Dicke gravity Regular Price $1,000.00 Sale Price $600.00 Excluding Sales Tax Quick View Astrophysics Observations and detectability of young Suns’ flaring and CME activity in optica Regular Price $1,000.00 Sale Price $450.00 Excluding Sales Tax Quick View TphysicsLetters Tunable structure-activity correlations of molybdenum dichalcogenides (MoX2; X=S Regular Price $2,000.00 Sale Price $400.00 Excluding Sales Tax Quick View New Thphysletters Bayesian and frequentist investigation of prior effects in EFTofLSS analyses of Regular Price $3,000.00 Sale Price $370.00 Excluding Sales Tax Quick View New Thphysletters A search for faint resolved galaxies beyond the Milky Way in DES Year 6: A new f Regular Price $1,900.00 Sale Price $750.00 Excluding Sales Tax Quick View New X-ray polarization properties of partially ionized equatorial obscurers around a Regular Price $800.00 Sale Price $350.00 Excluding Sales Tax Quick View New Unravelling multi-temperature dust populations in the dwarf galaxy Holmberg II Regular Price $1,200.00 Sale Price $400.00 Excluding Sales Tax Quick View New SpookyNet: Advancement in Quantum System Analysis through Convolutional Neural N Regular Price $1,500.00 Sale Price $500.00 Excluding Sales Tax Quick View New Rapid neutron star cooling triggered by accumulated dark matter Regular Price $1,500.00 Sale Price $500.00 Excluding Sales Tax Quick View Newly listed Tphysletters Searching for Radio Outflows from M31* with VLBI Observations Price $300.00 Excluding Sales Tax Quick View New Thphysletters Measurement of the scaling slope of compressible magnetohydrodynamic turbulence Regular Price $680.00 Sale Price $612.00 Excluding Sales Tax Quick View MAKE OPEN ACCESS New method to revisit the gravitational lensing analysis of the Bullet Cluster u Price $1,030.00 Excluding Sales Tax Quick View New Thphysletters New method to revisit the gravitational lensing analysis of the Bullet Cluster u Regular Price $599.00 Sale Price $359.40 Excluding Sales Tax Quick View New Nebular spectra from Type Ia supernova explosion models compared to JWST observa Regular Price $503.00 Sale Price $271.62 Excluding Sales Tax Quick View New Thphysletters The Nature of the 1 MeV-Gamma quantum in a Classic Interpretation of the Quantum Price $399.00 Excluding Sales Tax Quick View Exceptional Classifications of Non-Hermitian Systems Price $399.00 Excluding Sales Tax Quick View New Thphysletters On the occurrence of stellar fission in binary-driven hypernovae Price $399.00 Excluding Sales Tax Quick View New ApplSciLettersA AC frequency influence on pump temperature Price $399.00 Excluding Sales Tax Quick View New ApplSciLett. 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Theoretical Physics Letters HOME JOURNALS PRICING AND PLANS SUBMIT Locked Tphysicsletters/6879/10/1490/3486tpl/Protoplanetary disks in Ks-band total intensity and polarized light Citation (36) Received 14 August 2023, Revised 28 September, Accepted 04 October 2023 Friday, October 13, 2023 at 12:15:00 PM UTC Request Open Apply Now Article Rating by Publisher 10 Exp. Astrophysics Article Rating by Readers 10 Premium doi.wikipt.org/10/1490/3486tpl Protoplanetary disks in Ks-band total intensity and polarized light Bin B. Ren (任彬) iD ⋆⋆1, 2, 3 Myriam Benisty iD 1, 2 Christian Ginski iD 4 Ryo Tazaki iD 2 Nicole L. Wallack iD 5 Julien Milli iD 2 Antonio Garufi iD 6 Jaehan Bae iD 7 Stefano Facchini iD 8 François Ménard iD 2 Paola Pinilla iD 9 C. Swastik iD 10, Richard Teague iD 11, and Zahed Wahhaj iD 12 _________________________________________________________________ 1 Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Bd de l’Observatoire, CS 34229, 06304 Nice cedex 4, France; bin.ren@oca.eu 2 Université Grenoble Alpes, CNRS, Institut de Planétologie et d’Astrophysique (IPAG), F-38000 Grenoble, France 3 Department of Astronomy, California Institute of Technology, MC 249-17, 1200 E California Blvd, Pasadena, CA 91125, USA 4 School of Natural Sciences, University of Galway, University Road, H91 TK33 Galway, Ireland 5 Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA 6 INAF, Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, I-50125 Firenze, Italy 7 Department of Astronomy, University of Florida, Gainesville, FL 32611, USA 8 Dipartimento di Fisica, Universitá degli Studi di Milano, via Celoria 16, I-20133 Milano, Italy 9 Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, UK 10 Indian Institute of Astrophysics, Koramangala 2nd Block, Bangalore 560034, India 11 Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 12 European Southern Observatory, Alonso de Córdova 3107, Vitacura Casilla 19001, Santiago, Chile Theoretical Physics Letters 2023 ° 03(10) ° 0631-3486 https://www.wikipt.org/tphysicsletters Total citation received before and after publication. Citation data TOA Abstract Introduction Conclusion We thank the anonymous referee for their prompt and constructive comments. We thank Valentin Christiaens for comments on the manuscript. B.B.R. thanks Yinzi Xin for discussions on wavefront sensing in high-contrast imaging, Jie Ma on convolution effects, and Laurent Pueyo for support. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programs 0103.C0470 , 105.209E , 105.20HV , 105.20JB , 106.21HJ , and 108.22EE . For the archival data in Sect. 5.3, based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programs 60.A-9389 , 60.A-9800 , 095.C-0273 , 096.C-0248 , 096.C-0523 , 097.C0523 , 097.C-0702 , 097.C-0902 , 297.C-5023 , 198.C-0209 , 098.C-0486 , 098.C-0760 , 099.C-0147 , 0100.C-0452 , 0100.C-0647 , 0101.C-0464 , 0101.C0867 , 0102.C-0162 , 0102.C-0453 , 0102.C-0778 , 1104.C-0415 , 0104.C-0472 , 0104.C-0850 , 109.23BC , and 111.24GG . This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (PROTOPLANETS, grant agreement No. 101002188). This project has received funding from the European Union’s Horizon Europe research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 101103114. This work has made use of the High Contrast Data Centre, jointly operated by OSUG/IPAG (Grenoble), PYTHEAS/LAM/CeSAM (Marseille), OCA/Lagrange (Nice), Observatoire de Paris/LESIA (Paris), and Observatoire de Lyon/CRAL, and supported by a grant from Labex OSUG@2020 (Investissements d’avenir – ANR10 LABX56). This research has made use of the SIMBAD database (Wenger et al. 2000), operated at CDS, Strasbourg, France. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France (DOI: 10.26093/cds/vizier). The original description of the VizieR service was published in A&AS 143, 23 (Ochsenbein et al. 2000). The VizieR photometry tool is developed by Anne-Camille Simon and Thomas Boch. This research has made use of the Jean-Marie Mariotti Center SearchCal service4 co-developed by LAGRANGE and IPAG. Unlock Only Changeover the Schrödinger Equation This option will drive you towards only the selected publication. If you want to save money then choose the full access plan from the right side. Unlock all Get access to entire database This option will unlock the entire database of us to you without any limitations for a specific time period. This offer is limited to 100000 clients if you make delay further, the offer slots will be booked soon. Afterwards, the prices will be 50% hiked. Buy Unlock us Newsletters Abstract Diverse morphology in protoplanetary disks can result from planet-disk interaction, suggesting the presence of forming planets. Characterizing disks can inform the formation environments of planets. To date, most imaging campaigns have probed the polarized light from disks, which is only a fraction of the total scattered light and not very sensitive to planetary emission. Aims. We aim to observe and characterize protoplanetary disk systems in the near-infrared in both polarized and total intensity light, to carry out an unprecedented study of the dust scattering properties of disks, as well as of any possible planetary companions. Methods. Using the star-hopping mode of the SPHERE instrument at the Very Large Telescope, we observed 29 young stars hosting protoplanetary disks and their reference stars in the Ks-band polarized light. We extracted disk signals in total intensity by removing stellar light using the corresponding reference star observations, by adopting the data imputation concept with sequential non-negative matrix factorization (DI-sNMF). For well-recovered disks in both polarized and total intensity light, we parameterized the polarization fraction phase functions using scaled beta distribution. We investigated the empirical DI-sNMF detectability of disks using logistic regression. For systems with SPHERE data in Y-/J-/H-band, we summarized their polarized color at ≈90◦ scattering angle. Results. We obtained high-quality disk images in total intensity for 15 systems and in polarized light for 23 systems. Total intensity detectability of disks primarily depends on host star brightness, which determines adaptive-optics control ring imagery and thus stellar signals capture using DI-sNMF. The peak of polarization fraction tentatively correlates with the peak scattering angle, which could be reproduced using certain composition for compact dust, yet more detailed modeling studies are needed. Most of disks are blue in polarized J − Ks color, and the fact that they are relatively redder as stellar luminosity increases indicates larger scatterers. Conclusions. High-quality disk imagery in both total intensity and polarized light allows for disk characterization in polarization fraction. The combination of them reduces the confusion between disk and planetary signals. Introduction In the past 10 years, the advent of high angular resolution facilities enabled the detection of numerous disk substructures, such as rings, spirals, dust-depleted cavities, in the near-infrared scattered light (e.g., Benisty et al. 2015, 2023; Wagner et al. 2018; Shuai et al. 2022) and in the (sub-)millimeter/mm regime (e.g., Francis & van der Marel 2020; Long et al. 2022), indicating the ubiquity of substructures in large, bright disks (Bae et al. 2023). These substructures can be interpreted as evidence of planetdisk interactions, suggesting the presence of an underlying yetundetected population of young exoplanets (e.g., Dong et al. 2012). Additional support for this interpretation recently came from the detection of local velocity deviations in the gaseous outer disk velocity field probed with ALMA (e.g., Pinte et al. 2018; Teague et al. 2018; Pinte et al. 2020; Wölfer et al. 2023; Stadler et al. 2023). Scattered light surveys also pointed out a large fraction of infrared-faint disks, that appear more compact and featureless in scattered light because of self-shadowing effects (e.g., Garufi et al. 2022). These disks however often host substructures in the sub-millimeter (e.g., Long et al. 2018) that could be due to planets. The presence of massive planets inside cavities was also suggested in transition disks (disks with depleted inner cavities; Bae et al. 2019) and confirmed in at least one system, PDS 70, with the detection of two protoplanets (Keppler et al. 2018; Haffert et al. 2019). The range of plausible mass for the companion(s) in these disks is however quite large, as eccentric stellar companion could be sculpting the cavity (e.g., Calcino et al. 2019) as found in the HD 142527 system (Balmer et al. 2022). In that specific case, the companion is also leading to a misaligned inner disk, which casts a shadow on the outer disk (Price et al. 2018). Such misalignments were found in at least 6 transition disks (Bohn et al. 2022). Whether these features are of planetary or stellar nature, the search for the perturbers, which are responsible for all the observed disk substructures (e.g., Asensio-Torres et al. 2021; Cugno et al. 2023), is of prime importance to understand the formation and evolution of planetary systems. The detection of these perturbers would offer crucial observational evidence to test planet-disk interaction theories (e.g., Dong et al. 2015) and constrain the overall evolution of a planetary system (Bae et al. 2019). However, directly imaging planets embedded in bright and highly structured disks is very challenging with current instruments. Until now, all claims but PDS 70 still require confirmation (e.g., Kraus & Ireland 2012; Sallum et al. 2015; Quanz et al. 2015; Reggiani et al. 2018; Wagner et al. 2019; Boccaletti et al. 2020; Uyama et al. 2020; Currie et al. 2022; Hammond et al. 2023; Law et al. 2023; Wagner et al. 2023). To observe exoplanetary systems with high-contrast imaging, observation strategies including angular differential imaging (ADI; Marois et al. 2006, where parallactic angle diversity of observations is used to remove star light) have enabled the detection of prototypical planetary systems (e.g., HR 8799; Marois et al. 2008). Nevertheless, ADI detections are still limited by self-subtraction at close-in regions from the stars (e.g., Milli et al. 2012; Wahhaj et al. 2021), yet these regions are where giant planets are expected to have the most occurrence (1– 10 au; from a combination of radial velocity and high-contrast imaging surveys, e.g., Nielsen et al. 2019; Fulton et al. 2021). To overcome this limitation, on the one hand, better optimized post-processing methods for ADI datasets were developed (e.g., Pairet et al. 2021; Flasseur et al. 2021; Juillard et al. 2022, 2023). On the other hand, the diversity in archival observational data can enable the usage of other stars as the templates to remove star light and speckles with the reference differential imaging (RDI) data reduction strategy (e.g., Ruane et al. 2019; Xie et al. 2022). Moving forward along the direction of RDI, the Spectro-Polarimetic High contrast imager for Exoplanets REsearch (SPHERE; Beuzit et al. 2019) at the Very Large Telescope (VLT) from European Southern Observatory (ESO) initiated the star-hopping mode (Wahhaj et al. 2021), which offers quasi-simultaneous observations of a science star and its reference star, unleashing the full potential in exoplanet imaging in close-in regions for SPHERE. Determining dust properties is of fundamental importance for the early stage of grain growth and planetesimal formation, as they will determine the efficiency of grain sticking and fragmentation (Birnstiel et al. 2012). In addition to the planet imaging capabilities with SPHERE, the star-hopping mode enables optimized extraction of disks in scattered light in total intensity. This goes beyond the polarimetric surveys that have been routinely carried out in the near-infrared (e.g., Avenhaus et al. 2018; Garufi et al. 2020; Ginski et al. 2020), and allows us to better study spatial distribution and properties of dust in the disk (e.g., Olofsson et al. 2023). With the observations taken in dualpolarimetry imaging (DPI: Langlois et al. 2010) mode, which probes polarized signals in the scattered light, star-hopping can also offer total intensity imaging from RDI. The combination of both can yield an estimate of the polarization fraction, and thus to better constrain dust properties (e.g., shape, composition: Ginski et al. 2023; Tazaki et al. 2023). In this study, we present the first large survey of protoplanetary disks in total intensity from the ground. As many as 29 young stars are surveyed in Ks-band with VLT/SPHERE in the star-hopping mode. Our target sample consists of both transition disk systems to search for protoplanets that can potentially reside in the close-in regions with star-hopping that are otherwise unachievable (Wahhaj et al. 2021), and non-transition disk sample of faint disks in the infrared to search for planets in their outer disk regions. We also aim to derive the polarization fraction whenever possible. The paper is structured as follows: Sect. 2 provides the description of the observations and data reduction procedure, Sect. 3 presents the polarized light and total intensity maps, Sect. 4 shows the detection limits of companions, and in Sect. 5 we present the polarization fraction maps. We summarize and conclude the study in Sect. 6. Read more related articles. On the occurrence of stellar fission in binary-driven hypernovae Buy Now Searching for Radio Outflows from M31* with VLBI Observations Buy Now A search for faint resolved galaxies beyond the Milky Way in DES Year 6: A new f Buy Now Self – Regulated Thermal Process Taking Place during Hardening of Materials ... Buy Now Conclusion We obtained Ks-band imaging of protoplanetary disks in scattered light using SPHERE/IRDIS on VLT for 29 systems in starhopping mode. In the DPI setup of IRDIS imaging, we can obtain both polarized light observations and total intensity observations simultaneously. By modeling the interior regions of the IRDIS Ks-band control ring using the information on the control ring with DI-sNMF, we have identified 15 systems in total intensity light with unprecedented data quality. For the RDI results from DI-sNMF, we calculated the companion detection limits for these observations with high-quality disk recovery: the existence of disks do raise the Ks-band detection limits in comparison to the exploration in K1-/K2-band in Wahhaj et al. (2021). Nevertheless, an actual detection is a tradeoff between contrast and band-integrated companion luminosity, and thus narrower bands do not necessarily always provide better detections. Given that star-hopping observation has no dependence on sky rotation in the pupil-tracking mode, and that it can reach similar mass detection limits as ADI observations, it should be preferred to ADI observations in terms of observational schedulability. Together with the IRDIS Qϕ data, we obtained the polarization fraction maps for these systems. With these polarization fraction maps, we can reduce the confusion by blob structures resembling planetary signals, since signals from giant protoplanets are not expected to be polarized. For the polarization fraction maps, we described the polarization fraction curves using analytical beta distributions. The polarization fractions peak between ∼20% and ∼50%, yet they could be smaller than the actual values due to convolution effects from instrumentation. Assuming these polarization fraction curves are a credible representation of the actual polarization fractions, or if they undergo similar convolution effects, then we observe a tentative trend: the peak polarization fraction increases with the peak scattering angle. Using the Tazaki & Dominik (2022) and Tazaki et al. (2023) dust models from the AggScatVIR database, we could reproduce such a trend using absorptive materials for GRS dust; nevertheless, such models do not produce the individual polarization fraction curves. In addition, there can be alternative explanations with different dust parameters, and more future analysis and dust modeling are needed to interpret the observed polarization fraction curves. Moving forward, more comprehensive extraction of the polarization fraction curves – including modeling the disk components separately – can better help in comparing the scattering properties within each disk. In addition, lab measurements (e.g., Muñoz et al. 2021; Frattin et al. 2022) may provide important dust information for the observed polarization fraction curves. For the 26 systems that have existing IRDIS observations in shorter wavelengths (Y-, J-, or H-band), we obtained the color of these systems at ∼90◦ scattering angle in polarized light. For Jpol − Ks pol and Hpol − Ks pol color in polarized light, we observe trends that the color is relatively redder when stellar luminosity increases. Such a trend indicates that the scatterers are larger for more luminous stars (e.g., Ren et al. 2023; Crotts et al. 2023). In addition, while the polarized H − Ks color here has a marginal trend of being relatively redder as stellar luminosity increases, the color ranges from red to blue for systems similar stellar luminosity, demonstrating the diversity of scatterers in different systems. In order to obtain the properties of the scatterers (e.g., mineralogy, morphology, porosity, size), detailed radiative transfer modeling efforts adopting realistic models (e.g., Tazaki & Dominik 2022; Tazaki et al. 2023) are needed. Using the SPHERE/IRDIS control ring for RDI data reduction with DI-sNMF, we cannot yet recover the disks in total intensity for systems with Gaia DR3 Rp ≳ 11 or 2MASS K ≳ 8. For the sample with high selection bias here, our logistic regression results indicate that brighter hosts, redder references, and brighter references in observational wavelengths could aid in detecting disks. Given that there is no clear evidence that closer-in references can provide better RDI imagery for the hosts, starhopping users can attribute a lower priority to on-sky proximity in reference selection. TOC (TphysicsLetters) TOC (TphysicsLetters) The Nature of the 1 MeV-Gamma Quantum in a Classic Interpretation of the Quantum Nebular spectra from Type Ia supernov Physics Tomorrow TOC HIGHLIGHTS 2023 TOC HIGHLIGHTS 2023 Theoretical Physics Letters Physics Tomorrow ZZ Ceti stars of the southern ecliptic hemisphere re-observed by TESS ZZ Ceti stars of the southern ecliptic hemisphere re-observed by TESS Physics Tomorrow References Adams Redai, J. I., Follette, K. B., Wang, J., et al. 2023, AJ, 165, 57 Allard, F., Homeier, D., Freytag, B., & Sharp, C. 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P., Yang, H., et al. 2023, arXiv, arXiv:2308.16223 Abstract Introduction Conclusion References All Products Quick View Newly listed Tphysletters A Unifying Bag Model of Composite Fermionic Structures in a Cold Genesis Theory Regular Price $700.00 Sale Price $400.00 Excluding Sales Tax Quick View TphysicsLetters Detection of the large-scale tidal field with galaxy multiplet alignment in the Regular Price $1,900.00 Sale Price $950.00 Excluding Sales Tax Quick View Newly listed Tphysletters Violation of γ in Brans-Dicke gravity Regular Price $1,000.00 Sale Price $600.00 Excluding Sales Tax Quick View Astrophysics Observations and detectability of young Suns’ flaring and CME activity in optica Regular Price $1,000.00 Sale Price $450.00 Excluding Sales Tax Quick View TphysicsLetters Tunable structure-activity correlations of molybdenum dichalcogenides (MoX2; X=S Regular Price $2,000.00 Sale Price $400.00 Excluding Sales Tax Quick View New Thphysletters Bayesian and frequentist investigation of prior effects in EFTofLSS analyses of Regular Price $3,000.00 Sale Price $370.00 Excluding Sales Tax Quick View New Thphysletters A search for faint resolved galaxies beyond the Milky Way in DES Year 6: A new f Regular Price $1,900.00 Sale Price $750.00 Excluding Sales Tax Quick View New X-ray polarization properties of partially ionized equatorial obscurers around a Regular Price $800.00 Sale Price $350.00 Excluding Sales Tax Quick View New Unravelling multi-temperature dust populations in the dwarf galaxy Holmberg II Regular Price $1,200.00 Sale Price $400.00 Excluding Sales Tax Quick View New SpookyNet: Advancement in Quantum System Analysis through Convolutional Neural N Regular Price $1,500.00 Sale Price $500.00 Excluding Sales Tax Quick View New Rapid neutron star cooling triggered by accumulated dark matter Regular Price $1,500.00 Sale Price $500.00 Excluding Sales Tax Quick View Newly listed Tphysletters Searching for Radio Outflows from M31* with VLBI Observations Price $300.00 Excluding Sales Tax Quick View New Thphysletters Measurement of the scaling slope of compressible magnetohydrodynamic turbulence Regular Price $680.00 Sale Price $612.00 Excluding Sales Tax Quick View MAKE OPEN ACCESS New method to revisit the gravitational lensing analysis of the Bullet Cluster u Price $1,030.00 Excluding Sales Tax Quick View New Thphysletters New method to revisit the gravitational lensing analysis of the Bullet Cluster u Regular Price $599.00 Sale Price $359.40 Excluding Sales Tax Quick View New Nebular spectra from Type Ia supernova explosion models compared to JWST observa Regular Price $503.00 Sale Price $271.62 Excluding Sales Tax Quick View New Thphysletters The Nature of the 1 MeV-Gamma quantum in a Classic Interpretation of the Quantum Price $399.00 Excluding Sales Tax Quick View Exceptional Classifications of Non-Hermitian Systems Price $399.00 Excluding Sales Tax Quick View New Thphysletters On the occurrence of stellar fission in binary-driven hypernovae Price $399.00 Excluding Sales Tax Quick View New ApplSciLettersA AC frequency influence on pump temperature Price $399.00 Excluding Sales Tax Quick View New ApplSciLett. 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