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Tphysicsletters/6879/10/1490/584587tpl/Rapid neutron star cooling triggered by accumulated dark matter
Sunday, September 10, 2023 at 12:45:00 PM UTC
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Rapid neutron star cooling triggered by accumulated dark matter
Afonso Avila ´ 1
∗ Edoardo Giangrandi1,2
† Violetta Sagun1
‡ Oleksii Ivanytskyi3
§ and Constan¸ca Providˆencia 1¶
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1CFisUC, Department of Physics, University of Coimbra, Rua Larga P-3004-516, Coimbra, Portugal
2
Institut f¨ur Physik und Astronomie, Universit¨at Potsdam,
Karl-Liebknecht-Str.24-25, Potsdam, Germany and
3
Incubator of Scientific Excellence—Centre for Simulations of Superdense Fluids,
University of Wroc law, 50-204, Wroclaw, Poland
Acknowledgement
The work is supported by the FCT – Funda¸c˜ao para a Ciˆencia e a Tecnologia, within the project No. EXPL/FIS-AST/0735/2021. A.A., E.G., V.S., and ´ C.P. acknowledge the support from FCT within the projects No. UIDB/04564/2020, UIDP/04564/2020. E.G. also acknowledges the support from Project No. PRT/BD/152267/2021. C.P. is supported by project No. PTDC/FIS-AST/28920/2017. The work of O.I. was supported by the program Excellence Initiative–Research University of the University of Wroc law of the Ministry of Education and Science.
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Abstract
We study the effect of asymmetric fermionic dark matter (DM) on the thermal evolution of neutron stars (NSs). No interaction between DM and baryonic matter is assumed, except the gravitational one. Using the two-fluid formalism, we show that DM accumulated in the core of a star pulls inwards the outer baryonic layers of the star, increasing the baryonic density in the NS core. As a result, it significantly affects the star’s thermal evolution by triggering an early onset of the dir ect Urca process and modifying the photon emission from the surface caused by the decrease of the radius. Thus, due to the gravitational pull of DM, the direct Urca process becomes kinematically allowed for stars with lower masses. Based on these results, we discuss the importance of NS observations at different distances from the Galactic center. Since the DM distribution peaks towards the Galactic center, NSs in this region are expected to contain higher DM fractions that could lead to a different cooling behavior.