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Asteroseismology of DAV white dwarf stars [PDF]
Open Astronomy, 1998 Following the recent mode identification by Clemens suggesting the hydrogen layer mass of the DAV (ZZ Ceti) stars is nearly the same, I make the extreme assumption that models with a single composition profile with a hydrogen layer mass of 1.5 × 10−4M* may be able to fit the observed pulsation periods.
Bradley P. A.
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Comparing the asteroseismic properties of pulsating extremely low-mass pre-white dwarf stars and δ Scuti stars [PDF]
EPJ Web of Conferences, 2017 We present the first results of a detailed comparison between the pulsation properties of pulsating Extremely Low-Mass pre-white dwarf stars (the pre-ELMV variable stars) and δ Scuti stars.
Arias J.P.Sánchez +3 more
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An overview of white dwarf stars [PDF]
EPJ Web of Conferences, 2013 We present a brief summary of what is currently known about white dwarf stars, with an emphasis on their evolutionary and internal properties. As is well known, white dwarfs represent the end products of stellar evolution for the vast majority of stars ...
Charpinet S. +4 more
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White-Dwarf Asteroseismology With the Kepler Space Telescope
Frontiers in Astronomy and Space Sciences, 2020 In the course of their evolution, white-dwarf stars go through at least one phase of variability in which the global pulsations they undergo allow astronomers to peer into their interiors, making it possible to shed light on their deep inner structure ...
Alejandro H. Córsico +1 more
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A Chondritic Solar Neighborhood
The Planetary Science Journal, 2023 A persistent question in exoplanet demographics is whether exoplanetary systems form from similar compositional building blocks to our own. Polluted white dwarf stars offer a unique way to address this question, as they provide measurements of the bulk ...
Isabella L. Trierweiler +2 more
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Catalog of Magnetic White Dwarfs with Hydrogen Dominated Atmospheres
The Astrophysical Journal, 2023 White dwarfs are excellent research laboratories as they reach temperatures, pressures, and magnetic fields that are unattainable on Earth. To better understand how these three physical parameters interact with each other and with other stellar features,
L. L. Amorim +4 more
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The Astrophysical Journal Letters, 2023 ASASSN-V J205543.90+240033.5 (ASJ2055) is a possible post-common-envelope binary system. Its optical photometric data show an orbital variation of about 0.52 days and a fast period modulation of P _0 ∼ 9.77 minutes, whose origin is unknown.
J. Takata +9 more
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Diffusion of neon in white dwarf stars [PDF]
Physical Review E, 2010 Sedimentation of the neutron rich isotope $^{22}$Ne may be an important source of gravitational energy during the cooling of white dwarf stars. This depends on the diffusion constant for $^{22}$Ne in strongly coupled plasma mixtures. We calculate self-diffusion constants $D_i$ from molecular dynamics simulations of carbon, oxygen, and neon mixtures. We
Horowitz, C. J. +3 more
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Asteroseismology of White Dwarf Stars [PDF]
Symposium - International Astronomical Union, 1997 The theoretical potential of white dwarf asteroseismology is summarized. It is shown how one can derive fundamental parameters on the internal structure and evolution of these stars. The analysis of the non-radial g-modes permits in principle to determine the total mass, the rotation rate, the magnetic field strength. The mass of the outer layers, left
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Maximum mass ratio of AM CVn-type binary systems and maximum white dwarf mass in ultra-compact X-ray binaries [PDF]
Serbian Astronomical Journal, 2011 AM CVn-type stars and ultra-compact X-ray binaries are extremely interesting semi-detached close binary systems in which the Roche lobe filling component is a white dwarf transferring mass to another white dwarf, neutron star or a black hole ...
Arbutina Bojan
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