What can we learn from WET about how to make white dwarfs?

Kawaler, Steven D.

doi:10.1515/astro-1998-0107

Cited by 2 publications

(2 citation statements)

References 8 publications

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“…It became clear that the detailed core C/O profile and a double-step helium were the most important features for quantitative asteroseismology of the DBV white dwarfs (Dehner & Kawaler, 1995). The seismic study of the interiors of white dwarfs fed back into the theory of stellar evolution (Kawaler, 1998). Hot white dwarfs were also mature examples of active asteroseismology with such a great importance that in their interiors their prior evolutionary history, especially the story of their last nuclear evolutionary stage had been locked.…”

Section: Results Between 1970-1980mentioning

confidence: 99%

“…Kawaler & Bradley (1994) derived that the constant period spacing was primarily determined by the mass of the star, which allowed mass determination. Regular departures from uniformity could have been regarded as a result of mode trapping by a surface composition discontinuity (Kawaler, 1998) allowing the determination of the mass of the H and He layers. Rotation could be deduced by identifying the equal frequency split in the pulsation spectrum.…”

Section: Results Between 1970-1980mentioning

confidence: 99%

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An Observer's View on the Future of Asteroseismology

Paparó

2019

Front. Astron. Space Sci.

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Scientific research is a continuous process, and the speed of future progress can be estimated by the pace of finding explanations for previous research questions. In this observers based view of stellar pulsation and asteroseismology, we start with the earliest observations of variable stars and the techniques used to observe them. The earliest variable stars were large amplitude, radial pulsators but were followed by other classes of pulsating stars. As the field matured, we outline some cornerstones of research into pulsating star research with an emphasis on changes in observational techniques. Improvements from photographs, to photometry, CCDs, and space telescopes allowed researchers to separate out pulsating stars from other stars with light variations, recognize radial and nonradial pulsation courtesy of increased measurement precision, and then use nonradial pulsations to look inside the stars, which cannot be done any other way. We follow several highlighted problems to show that even with excellent space data, there still may not be quick theoretical explanations. As the result of technical changes, the structure of international organizations devoted to pulsating stars has changed, and an increasing number of conferences specialized to space missions or themes are held. Although there are still many unsolved problems, such as mode identification in non-asymptotic pulsating stars, the large amount of data with unprecedented precision provided by space missions (MOST, CoRoT, Kepler) and upcoming missions allow us to use asteroseismology to its full potential. However, the enormous flow of data will require new techniques to extract the science before the next missions. The future of asteroseismology will be successful if we learn from the past and improve with improved techniques, space missions, and a properly educated new generation.

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Section: Results Between 1970-1980mentioning

confidence: 99%

Section: Results Between 1970-1980mentioning

confidence: 99%

An Observer's View on the Future of Asteroseismology

Paparó

2019

Front. Astron. Space Sci.

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The gravitational wave radiation of pulsating white dwarfs revisited: the case of BPM 37093 and PG 1159-035

Garcı́a–Berro

Lorén–Aguilar

Córsico

et al. 2006

A&A

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We compute the emission of gravitational radiation from pulsating white dwarfs. This is done by using an up-to-date stellar evolutionary code coupled with a state-of-the-art pulsational code. The emission of gravitational waves is computed for a standard 0.6 M white dwarf with a liquid carbon-oxygen core and a hydrogen-rich envelope, for a massive DA white dwarf with a partially crystallized core for which various = 2 modes have been observed (BPM 37093) and for PG 1159-035, the prototype of the GW Vir class of variable stars, for which several quadrupole modes have been observed as well. We find that these stars do not radiate sizeable amounts of gravitational waves through their observed pulsation g-modes, in line with previous studies. We also explore the possibility of detecting gravitational waves radiated by the f -mode and the p-modes. We find that in this case the gravitational wave signal is very large and, hence, the modes decay very rapidly. We also discuss the possible implications of our calculations for the detection of gravitational waves from pulsating white dwarfs within the framework of future space-borne interferometers like LISA.

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What can we learn from WET about how to make white dwarfs?

Cited by 2 publications

References 8 publications

An Observer's View on the Future of Asteroseismology

An Observer's View on the Future of Asteroseismology

The gravitational wave radiation of pulsating white dwarfs revisited: the case of BPM 37093 and PG 1159-035

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