USING ASTEROSEISMOLOGY TO INVESTIGATE THE PULSATING HYDROGEN-RICH WHITE DWARFS HL TAU 76 AND EC14012-1446
Date
2025-05
Authors
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Publisher
University of Delaware
Abstract
White dwarfs (WDs) are the final stage of stellar evolution for approximately
98% of stars, including the Sun. WD evolution is dominated by cooling. As they cool,
they pass through specific temperature ranges, or instability strips, where pulsations
are initiated. We are able to gain valuable insight into stellar parameters of these
fascinating objects using asteroseismology. Asteroseismology is the study of a star’s
internal structure through the analysis of its pulsations. In particular, it’s important to
study hydrogen-atmosphere white dwarfs (DAs), as they comprise approximately 80%
of the WD population. The pulsation behavior of these pulsating DA white dwarfs
(DAVs) has broader implications for our comprehension of stellar evolution and the
formation of white dwarfs, which play a vital role in the evolution of our Solar System
and of the Universe. In this work, we will present our findings on two DAVs, HL Tau
76 and EC 14012-1446. There is a significant amount of observational data for both
DAVs. This amassed data is a result of both ground-based telescopes and space-based
observations. The DAV population has similar physical properties, so the study of
these two DAVs allows for a more comprehensive understanding of the general DA
population. This is the first time a comprehensive analysis of these two stars has been
undertaken.