Ultrashort-Period Stellar Oscillations. III. Power-Spectrum Analysis of Photometric Observations of White Dwarfs

Hesser, J. E.; Ostriker, Jeremiah P.; Lawrence, G. M.

doi:10.1086/149922

Cited by 13 publications

(2 citation statements)

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“…Our data-collection and analytical techniques closely resemble those previously discribed (Hesser, Ostriker and Lawrence 1969; hereinafter referenced as HOL); only departures from those procedures are discussed further here. The observations were obtained with the 60-, 36-and No.…”

Section: Observationsmentioning

confidence: 88%

8. High Frequency Stellar Oscillations: IV: Photoelectric Monitoring of Southern White Dwarfs

Hesser

Lasker²

1971

Symp. - Int. Astron. Union

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Section: Observationsmentioning

confidence: 88%

8. High Frequency Stellar Oscillations: IV: Photoelectric Monitoring of Southern White Dwarfs

Hesser

Lasker²

1971

Symp. - Int. Astron. Union

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“…Other Non-variables; Lists of non-variable white dwarfs which were observed during surveys for variable white dwarfs can be found in Lasker (1971, 1972), Hesser et al (1969), Lawrence et al (1967), McGraw (1976, 1977, Robinson and McGraw (1976), Robinson et al (1978), andRicher andUlrych (1974). Care must be exercised when using these lists because a star may appear -occasionally disguised by an alias -in more than one of them.…”

Section: The Census Of the Zz Ceti Starsmentioning

confidence: 99%

The Observational Properties of the ZZ Ceti Stars

Robinson

1979

International Astronomical Union Colloquium

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The ZZ Ceti stars are the pulsating white dwarfs lying within a narrow instability strip, extending in temperature from 13,500 to 10,500 K, on the white dwarf cooling sequence. That white dwarfs should be pulsationally unstable cannot be considered surprising, since theoretical investigations of white dwarf pulsations began at least as early as 1949 (Sauvenier-Goffin 1949). As the predicted pulsation periods demonstrate, however, the nature of the pulsations was not correctly foreseen. With very few exceptions (e.g. Harper and Rose 1970) the early investigations assumed that the most likely pulsations to be excited were radial pulsations. Thus, the calculated periods were quite short, typically 2-10 seconds. The first of the pulsating white dwarfs actually to be observed was HL Tau-76 (Landolt 1968). A portion of its light curve is shown in Figure 1. The typical interval between successive pulses is about 750 seconds, not 2-10 seconds. This is a serious discrepancy, and one that exists for all of the ZZ Ceti stars discovered since HL Tau-76. Clearly, then, the observational data requires us to modify our understanding of pulsating white dwarfs. A considerable body of this observational data now exists. The purpose of the present paper is to present the data, and to show that it provides a reasonably coherent picture of the pulsating white dwarfs.

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The observational properties of the ZZ Ceti stars

Robinson

Nonradial and Nonlinear Stellar Pulsation

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Ultrashort-Period Stellar Oscillations. III. Power-Spectrum Analysis of Photometric Observations of White Dwarfs

Cited by 13 publications

References 0 publications

8. High Frequency Stellar Oscillations: IV: Photoelectric Monitoring of Southern White Dwarfs

8. High Frequency Stellar Oscillations: IV: Photoelectric Monitoring of Southern White Dwarfs

The Observational Properties of the ZZ Ceti Stars

The observational properties of the ZZ Ceti stars

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