2013
DOI: 10.1051/epjconf/20134305005
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Pulsations in white dwarfs: Selected topics

Abstract: Abstract. This paper presents a very brief overview of the observed properties of g-mode pulsations in variable white dwarfs. We then discuss a few selected topics: Excitation mechanisms (kappa-and convection-mechanisms), and briefly the effect of a strong magnetic field (∼ 1 MG) on g-modes as recently found in a hot DQ (carbon-rich atmosphere) white dwarf. In the discussion of excitation mechanisms, a simple interpretation for the convection mechanism is given.

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Cited by 19 publications
(17 citation statements)
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“…Our nonadiabatic computations rely on the frozen-convection (FC) approximation, in which the perturbation of the convective flux is neglected. While this approximation could not be strictly valid in the case of the longest-period g modes considered, we do not expect large variations of the nonadiabatic results if a time-dependent convection treatment is used (TDC; see, for instance, Van Grootel et al 2013;Saio 2013) instead, although we must keep in mind that this issue can constitute a source of uncertainties in the location of the blue edges of instability computed in this work. The Brunt-Väisälä frequency, N, is computed as in Tassoul et al (1990).…”
Section: Numerical Codesmentioning
confidence: 89%
“…Our nonadiabatic computations rely on the frozen-convection (FC) approximation, in which the perturbation of the convective flux is neglected. While this approximation could not be strictly valid in the case of the longest-period g modes considered, we do not expect large variations of the nonadiabatic results if a time-dependent convection treatment is used (TDC; see, for instance, Van Grootel et al 2013;Saio 2013) instead, although we must keep in mind that this issue can constitute a source of uncertainties in the location of the blue edges of instability computed in this work. The Brunt-Väisälä frequency, N, is computed as in Tassoul et al (1990).…”
Section: Numerical Codesmentioning
confidence: 89%
“…1 and Table 1). To highlight this mechanism, we follow the didactic approach proposed by Saio (2013). Note that an extensive review about the various type of pulsating white dwarf stars can be found in Winget and Kepler (2008).…”
Section: Convective Drivingmentioning
confidence: 99%
“…Our nonadiabatic computations rely on the frozen-convection (FC) approximation, in which the perturbation of the convective flux is neglected. While this approximation is known to give unrealistic locations of the g-mode red edge of the ZZ Ceti instability strip, it leads to satisfactory predictions for the location of the blue edge (Van Grootel et al 2012) (see also Saio 2013, for an enlightening discussion of this topic). et al (2013) derived realistic configurations for lowmass He-core WDs by mimicking the binary evolution of progenitor stars.…”
Section: Pulsation Codementioning
confidence: 99%