SDSS J142625.71+575218.3: A Prototype for a New Class of Variable White Dwarf

Montgomery, M. H.; Williams, Kurtis A.; Winget, D. E.; Dufour, Patrick; DeGennaro, Steven; Liebert, James

doi:10.1086/588286

Cited by 78 publications

(153 citation statements)

References 18 publications

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“…Also, the theoretical blue edge of DQVs is hotter for less massive models than for more massive ones (see Fig. 23), which is at odds with the results of and Montgomery et al (2008a). In addition, the blue edge for DQV stars is hotter for smaller amounts of He in the envelopes.…”

Section: Dqvsmentioning

confidence: 73%

“…They are white dwarfs with C-and Herich atmospheres. The analysis of the prototype of this class (SDSS J142625.71+575218.3) carried out by Green et al (2009) appeared to confirm the pulsating nature of this star, thus unequivocally ruling out the interacting binary hypothesis that was initially put forward by Montgomery et al (2008a) in the discovery paper. Table 2, adapted from O'Brien (2003), presents a summary of the main characteristics of each class of pulsating white dwarf stars.…”

Section: Stellar Pulsations and Variable White Dwarfsmentioning

confidence: 86%

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Evolutionary and pulsational properties of white dwarf stars

Althaus

Córsico

Isern

et al. 2010

Astron Astrophys Rev

369

372

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White dwarf stars are the final evolutionary stage of the vast majority of stars, including our Sun. Since the coolest white dwarfs are very old objects, the present population of white dwarfs contains a wealth of information on the evolution of stars from birth to death, and on the star formation rate throughout the history of our Galaxy. Thus, the study of white dwarfs has potential applications to different fields of astrophysics. In particular, white dwarfs can be used as independent reliable cosmic clocks, and can also provide valuable information about the fundamental parameters of a wide variety of stellar populations, like our Galaxy and open and globular clusters. In addition, the high densities and temperatures characterizing white dwarfs allow to use these stars as cosmic laboratories for studying physical processes under extreme conditions that cannot be achieved in terrestrial laboratories. Last but not least, since many white dwarf stars undergo pulsational instabilities, the study of their properties constitutes a powerful tool for applications beyond stellar astrophysics. In particular, white dwarfs can be used to constrain fundamental properties of elementary particles such as axions and neutrinos, and to study problems related to the variation of fundamental constants.These potential applications of white dwarfs have led to a renewed interest in the calculation of very detailed evolutionary and pulsational models for these stars. In this work, we review the essentials of the physics of white dwarf stars. We enumerate the reasons that make these stars excellent chronometers and we describe why white dwarfs provide tools for a wide variety of applications. Special emphasis is placed on the physical processes that lead to the formation of white dwarfs as well as on the different energy sources and processes responsible for chemical abundance changes that occur along their evolution. Moreover, in the course of their lives, white dwarfs cross different pulsational instability strips. The existence of these instability strips provides astronomers with an unique opportunity to peer into their internal structure that would otherwise remain hidden from observers. We will show that this allows to measure with unprecedented precision the stellar masses and to infer their envelope thicknesses, to probe the core chemical stratification, and to detect rotation rates and magnetic fields. Consequently, in this work, we also review the pulsational properties of white dwarfs and the most recent applications of white dwarf asteroseismology.

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Section: Dqvsmentioning

confidence: 73%

Section: Stellar Pulsations and Variable White Dwarfsmentioning

confidence: 86%

Evolutionary and pulsational properties of white dwarf stars

Althaus

Córsico

Isern

et al. 2010

Astron Astrophys Rev

369

372

View full text Add to dashboard Cite

show abstract

“…One such class is the hot DQ stars, discovered by Dufour et al [11], which have spectra that are C-dominated. Recently, IVIontgomery et al [10] discovered what are apparently gmode pulsations in one of these objects. Subsequently, two more such DQV stars have been found [53], establishing this as a class of pulsating stars, the first such new class of white dwarf pulsators in 25 years.…”

Section: The Dqvs: a New Class Of Wd Pulsatormentioning

confidence: 98%

“…Recently, Montgomery et al [10] discovered a fourth class of pulsating white dwarf: the DQVs. These stars have large amounts of C in their atmospheres [11] and, like the DAVs and DBVs, their pulsations seem to be tied to the partial ionization of their dominant surface element, C and/or He.…”

Section: Astrophysical Context 2 a Brief Historymentioning

confidence: 99%

White Dwarf and Pre-White Dwarf Pulsations

Montgomery¹

2009

AIP Conference Proceedings

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“…Two new classes of white dwarf pulsators were found, the DQVs (Montgomery et al 2008;Fontaine et al 2009;Williams et al 2013) and the ELMVs Hermes et al (2013a,b); Van Grootel et al (2012, 2013a; Córsico & Althaus (2014).…”

Section: Compact Oscillatorsmentioning

confidence: 99%