Comparative analysis of mass determination methods for pulsating white dwarfs

ALEJANDRO H. CÓRSICO; LEILA M. CALCAFERRO; MURAT UZUNDAG; LEANDRO G. ALTHAUS; S. O. KEPLER; WERNER, KLAUS

Porto

Workshop; 8th TESS/15th Kepler Asteroseismic Science Consortium Workshop; 2024

Instituto de Astrofísica e Ciências do Espaço, Faculdade de Ciências da Universidade do Porto

Stellar mass determination poses a central challenge in stellar astrophysics. This study delves into the mass assessment of isolated pulsating white dwarf (WD) stars through spectroscopy, asteroseismology, and astrometry. Focusing on a sample of DAVs (pulsating H-rich atmosphere WDs), DBVs (pulsating He-rich atmosphere WDs), and GW Vir variables (pulsating hot C-, O-, and He-rich atmosphere WDs and pre-WDs), we carefully compare the mass values derived from these diverse methods. Employing consistent WD models and evolutionary tracks, our preliminary analysis reveals that: (1) There is a broad agreement among methods for DAV stars, particularly for those with masses below 0.75 M⊙. However, significant discrepancies emerge for certain massive stars; (2) Astrometric masses tend to surpass seismic and spectroscopic masses for DBV stars; (3) Marked differences are evident in the mass of GW Vir stars, indicating methodological disparities in mass determination. In brief, we plan to include the accurate photometric technique to assess the photometric mass and compare the results with the other techniques.