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Populations of accreting white dwarfs

Published online by Cambridge University Press:  30 December 2019

Hai-Liang Chen ,
Tyrone E. Woods ,
Lev Yungelson ,
Marat Gilfanov  and
Zhanwen Han
Hai-Liang Chen
Affiliation:
Yunnan Observatories, CAS, Kunming, 650011, China email: [email protected] Key Laboratory for the Structure and Evolution of Celestial Objects, CAS, Kunming 650011, China Center for Astronomical Mega-Science, Chinese Academy of Science, Beijing 100012, China
Tyrone E. Woods
Affiliation:
Institute of Gravitational Wave Astronomy and School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, UK
Lev Yungelson
Affiliation:
Institute of Astronomy, RAS, 48 Pyatnitskaya Str., 119017 Moscow, Russia
Marat Gilfanov
Affiliation:
Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str. 1, Garching b. München 85741, Germany Space Research Institute of Russian Academy of Sciences, Profsoyuznaya 84/32, 117997 Moscow, Russia
Zhanwen Han
Affiliation:
Yunnan Observatories, CAS, Kunming, 650011, China email: [email protected] Key Laboratory for the Structure and Evolution of Celestial Objects, CAS, Kunming 650011, China Center for Astronomical Mega-Science, Chinese Academy of Science, Beijing 100012, China
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Abstract

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Using a hybrid binary population synthesis approach, we modelled the formation and evolution of populations of accreting white dwarfs (WDs) for differing star formation histories. We found that the delay time distribution of SNe Ia in the single degenerate scenario is inconsistent with observations. Additionally, we found that our predicted X-ray and UV emission of populations of accreting WDs are consistent with the X-ray luminosities of early-type galaxies observed by Chandra and the HeII 4686 Å/Hβ line ratio measured in stacked SDSS spectra of passively evolving galaxies. Moreover, we found that the majority of current novae in elliptical-like galaxies have low-mass WDs, long decay times, long recurrence periods and are relatively faint. In contrast, the majority of current novae in spiral-like galaxies have massive WDs, short decay times, short recurrence periods and are relatively bright. Our predicted distribution of mass-loss timescales in an M31-like galaxy is consistent with observations for Andromeda.

Keywords

stars:novaecataclysmic variableswhite dwarfs
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S343: Why Galaxies Care About AGB Stars: A Continuing Challenge through Cosmic Time , August 2018 , pp. 371 - 372
Copyright
© International Astronomical Union 2019 

References

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