Thirty‐Five New Pulsating DA White Dwarf Stars

Mukadam, Anjum S.; Mullally, Fergal; Nather, R. E.; Winget, D. E.; Hippel, Ted von; Kleinman, S. J.; Nitta, A.; Krzesiński, Jurek; Kanaan, A.; Koester, D.; Sullivan, D. J.; Homeier, D.; Thompson, Susan E.; Reaves, D.; Cotter, Charles H.; Slaughter, D.; Brinkmann, J.

doi:10.1086/383083

Cited by 118 publications

(184 citation statements)

References 61 publications

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“…Employing high signal-tonoise spectra, Bergeron et al (1995Bergeron et al ( , 2004, and Gianninas et al (2005Gianninas et al ( , 2006 have found a pure instability strip for the brightest DAVs. On the other hand, there are about 20 DA stars located within the instability strip, for which pulsations are not detected (Mukadam et al 2004). These stars suffer from a poor determination of their surface parameters.…”

Section: Observations Of Davs: the Purity Of The Instability Stripmentioning

confidence: 99%

Evolutionary and pulsational properties of white dwarf stars

Althaus

Córsico

Isern

et al. 2010

Astron Astrophys Rev

379

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: Observations Of Davs: the Purity Of The Instability Stripmentioning

confidence: 99%

Evolutionary and pulsational properties of white dwarf stars

Althaus

Córsico

Isern

et al. 2010

Astron Astrophys Rev

379

372

View full text Add to dashboard Cite

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“…For compact pulsators, the Sloan Digital Sky Survey has been the tool to find and characterize new white dwarf and subdwarf stars, and led to the discovery of more than 200 new pulsators, mainly DAVs, also called ZZ Cetis (Mukadam et al 2004;Mullally et al 2005;Kepler et al 2005a;Castanheira et al 2006Castanheira et al , 2007, and their modelling (Castanheira & Kepler 2008, 2009Romero et al 2012Romero et al , 2013, but also DBVs Nitta et al (2009) and a few DOVs, also called variable PG 1159 or GW Vir stars (Quirion 2009a;Quirion, Fontaine & Brassard 2009b;Woudt, Warner,& Zietsman 2012;Kepler et al 2014). 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%

Triennial Report (2012-2015): The Legacy Issue

Pollard¹,

Jeffery²,

Handler³

et al. 2015

Proc. IAU

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“…For the DAVS, the number known has grown from a pre-SDSS number of about 35 to approximately 150 stars [64,65,66,67,68]. In addition, the number of known DBVs has increased from a pre-SDSS number of 9 to a current value of 18, doubling the sample of DBVs [69].…”

Section: Increased Numbers Of Known Pulsatorsmentioning

confidence: 99%

White Dwarf and Pre-White Dwarf Pulsations

Montgomery¹

2009

AIP Conference Proceedings

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Thirty‐Five New Pulsating DA White Dwarf Stars

Cited by 118 publications

References 61 publications

Evolutionary and pulsational properties of white dwarf stars

Evolutionary and pulsational properties of white dwarf stars

Triennial Report (2012-2015): The Legacy Issue

White Dwarf and Pre-White Dwarf Pulsations

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