Asteroseismological Observations of the Central Star of the Planetary Nebula NGC 1501

Bond, H. E.; Kawaler, S. D.; Ciardullo, Robin; Stover, R. J.; Kuroda, T.; Ishida, Toru; Ono, Tomoko; Tamura, Shinichi; Malasan, Hakim L.; Yamasaki, A.; Hashimoto, Osamu; Kambe, Eiji; Takeuti, M.; Kato, T.; Kato, M.; Chen, J.-S.; Leibowitz, E. M.; Roth, M.; Soffner, T.; Mitsch, Wolfgang

doi:10.1086/118214

Cited by 34 publications

(43 citation statements)

References 12 publications

(26 reference statements)

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“…Table 6 summarizes the asteroseismological masses obtained for each star, along with the associated values of the spectroscopic mass. A graphical representation of these results Bond et al (1996).…”

Section: Asteroseismological Inferences On Gw Vir Starsmentioning

confidence: 99%

Evolutionary and pulsational properties of white dwarf stars

Althaus

Córsico

Isern

et al. 2010

Astron Astrophys Rev

359

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: Asteroseismological Inferences On Gw Vir Starsmentioning

confidence: 99%

Evolutionary and pulsational properties of white dwarf stars

Althaus

Córsico

Isern

et al. 2010

Astron Astrophys Rev

359

372

View full text Add to dashboard Cite

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“…Two stars have their modes clearly identified by the period distribution method: PG 1159-035 (Winget et al 1991) and GD 358 . The stars PG 2131+066 , PG 1707+427 (Kawaler et al 2004) and RX J2117 (Bond et al 1996) have modes identified as = 1 from their period spacings and/or the presence of triplets.…”

Section: Observations With Hstmentioning

confidence: 99%

HST observations of the pulsating white dwarf GD 358

Castanheira¹,

Nitta²,

Winget

et al. 2005

A&A

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Abstract. We used time-resolved ultraviolet spectroscopy obtained with the FOS and STIS spectrographs of the Hubble Space Telescope (HST), together with archival IUE observations to measure the effective temperature (T eff ), surface gravity (log g) and distance (d) of the pulsating DB white dwarf GD 358 with unprecedented accuracy, and to show that the temperature did not change during the 1996 sforzando, when the star changed basically to a single mode pulsator. We also measured for the first time for a DBV the spherical harmonic degree ( ) for two modes, with k = 8 and k = 9, which was only possible because the stellar light curve was dominated by a single mode in 1996. The independent spectra provide the following values: T eff = 24 100 ± 400 K, log g = 7.91 ± 0.26 and d = 42.7 ± 2.5 pc. The ultraviolet spectroscopic distance is in better agreement with the seismological value, than the one derived by parallax.

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“…This is difficult spectroscopy -high resolution spectra are needed, and accurate and reliable NLTE model atmospheres are essential for the analysis. Bond et al (1996) …”

Section: Spectroscopic Measurements Of V Sin I In White Dwarfsmentioning

confidence: 99%

White Dwarf Rotation: Observations and Theory

Kawaler¹

2004

Symp. - Int. Astron. Union

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Abstract. White dwarfs rotate. The angular momentum in single white dwarfs must originate early in the life of the star, but also must be modified (and perhaps severely modified) during the many stages of evolution between birth as a mainsequence star and final appearance as a white dwarf. Observational constraints on the rotation of single white dwarf stars come from traditional spectroscopy and from asteroseismology, with the latter providing hints of angular velocity with depth. Results of these observational determinations, that white dwarfs rotate with periods ranging from hours to days (or longer), tells us that the processes by which angular momentum is deposited and/or drained from the cores of AGB stars are complex. Still, one can place strong limits on these processes by considering relatively simple limiting cases for angular momentum evolution in prior stages, and on subsequent angular momentum evolution in the white dwarfs. These limiting-case constraints will be reviewed in the context of the available observations.

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Asteroseismological Observations of the Central Star of the Planetary Nebula NGC 1501

Cited by 34 publications

References 12 publications

Evolutionary and pulsational properties of white dwarf stars

Evolutionary and pulsational properties of white dwarf stars

HST observations of the pulsating white dwarf GD 358

White Dwarf Rotation: Observations and Theory

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