Atmospheric Temperature Inversions and He ι 5876 Core Profile Structure in White Dwarfs

Here we report distinctive core profiles in the strongest optical helium line, He ι λ5876, from high-resolution high-sensitivity observations of spectral type DB white dwarfs. By analyzing a sample of 40 stars from Keck/HIRES and VLT/UVES, we find the core appearance to be related to the degree of h...

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Bibliographic Details
Published in:The Astrophysical journal 2020-08, Vol.900 (1)
Main Authors: Klein, Beth, Blouin, Simon, Romani, Diego, Zuckerman, Benjamin, Melis, Carl, Xu, Siyi, Dufour, Patrick, Genest-Beaulieu, Cynthia, Bédard, Antoine, Jura, Michael
Format: Article
Language:English
Subjects:
ASTRONOMY AND ASTROPHYSICS
DB stars
extrasolar rocky planets
high resolution spectroscopy
stellar atmospheres
stellar atmospheric opacity
stellar effective temperatures
upper atmosphere
white dwarf stars
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Summary:Here we report distinctive core profiles in the strongest optical helium line, He ι λ5876, from high-resolution high-sensitivity observations of spectral type DB white dwarfs. By analyzing a sample of 40 stars from Keck/HIRES and VLT/UVES, we find the core appearance to be related to the degree of hydrogen and heavy element content in the atmosphere. New Ca K-line measurements or upper limits are reported for about half the sample stars. He ι λ5876 emission cores with a self-reversed central component are present for those stars with relatively low hydrogen abundance, as well as relatively low atmospheric heavy element pollution. This self-reversed structure disappears for stars with higher degrees of pollution and/or hydrogen abundance, giving way to a single absorption core. From our model atmospheres, we show that the self-reversed emission cores can be explained by temperature inversions in the upper atmosphere. We propose that the transition to a single absorption core is due to the additional opacity from hydrogen and heavy elements that inhibits the temperature inversions. Our current models do not exactly match the effective temperature range of the phenomenon or the amplitude of the self-reversed structure, which is possibly a result of missing physics such as 3D treatment, convective overshoot, and/or non-LTE effects. The He ι λ5876 line structure may prove to be a useful new diagnostic for calibrating temperature profiles in DB atmosphere models.
ISSN:1538-4357
1538-4357