2022MNRAS.510..858R -
Mon. Not. R. Astron. Soc., 510, 858-869 (2022/February-2)
Uncovering the chemical structure of the pulsating low-mass white dwarf SDSS J115219.99+024814.4.
ROMERO A.D., LAUFFER G.R., ISTRATE A.G. and PARSONS S.G.
Abstract (from CDS):
Pulsating low-mass white dwarf (WD) stars are WDs with stellar masses between 0.30 and 0.45 M☉ that show photometric variability due to gravity-mode pulsations. Within this mass range, they can harbour both a helium core and hybrid core, depending if the progenitor experienced helium-core burning during the pre-WD evolution. SDSS J115219.99+024814.4 is an eclipsing binary system where both components are low-mass WDs, with stellar masses of 0.362 ± 0.014 M☉ and 0.325 ± 0.013 M☉. In particular, the less-massive component is a pulsating star, showing at least three pulsation periods of ∼1314, ∼1069, and ∼582.9 s. This opens the way to use asteroseismology as a tool to uncover its inner chemical structure, in combination with the information obtained using the light-curve modelling of the eclipses. To this end, using binary evolutionary models leading to helium- and hybrid-core WDs, we compute adiabatic pulsations for l = 1 and l = 2 gravity modes with Gyre. We found that the pulsating component of the SDSS J115219.99+024814.4 system must have a hydrogen envelope thinner than the value obtained from binary evolution computations, independently of the inner composition. Finally, from our asteroseismological study, we find a best-fitting model characterized by Teff=10917 K, M = 0.338 M☉, and MH = 10–6 M☉ with the inner composition of a hybrid WD.
Abstract Copyright:
© 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society
Journal keyword(s):
asteroseismology - binaries: eclipsing - white dwarfs
Simbad objects:
2
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