2013/09/13 by William M. Wolf, Lars Bildsten, Jared Brooks +1 · 7 citations
Physics and Astronomy · #Accretion (finance) #Accretion disc #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Astrophysics and Star Formation Studies #Hydrogen #Instability #Phase (matter) #Solar mass #White dwarf #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.1088/0004-637x/777/2/136
12 pages, 14 figures. Submitted to the Astrophysical Journal
arxiv created 2013/09/13 · openalex publication_date 2013/10/22 · arxiv updated 2015/06/17 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
We examine the properties of white dwarfs (WDs) accreting hydrogen-rich matter in and near the stable burning regime of accretion rates as modeled by time-dependent calculations done with Modules for Experiments in Stellar Astrophysics (MESA). We report the stability boundary for WDs of masses between 0.51 M ☉ and 1.34 M ☉ as found via time-dependent calculations. We also examine recurrent novae that are accreting at rates close to, but below, the stable burning limit and report their recurrence times. Our dense grid in accretion rates finds the expected minimum possible recurrence times as a function of the WD mass. This enables inferences to be made about the minimum WD mass possible to reach a specific recurrence time. We compare our computational models of post-outburst novae to the stably burning WDs and explicitly calculate the duration and effective temperature ( T eff ) of the post-nova WD in the supersoft phase. We agree with the measured turnoff time– T eff relation in M31 by Henze and collaborators, infer WD masses in the 1.0–1.3 M ☉ range, and predict ejection masses consistent with those observed. We close by commenting on the importance of the hot helium layer generated by stable or unstable hydrogen burning for the short- and long-term evolution of accreting WDs.