منابع مشابه
PG 1541 + 650 : A new ZZ Ceti white dwarf ?
We report the discovery of a new pulsating DA white dwarf, or ZZ Ceti, from the list of the Palomar-Green survey, rediscovered in the ongoing Hamburg Quasar survey (HQS). PG1541+650 is one of the ZZ Ceti candidates listed in the analysis of 80 DA white dwarfs from the HQS. With an effective temperature of 12000 K, for a surface gravity logg=7.79, it lies in the ZZ Ceti instability strip. It is ...
متن کاملBPM 24754 : A new Southern ZZ Ceti star ?
We report the discovery of a new long–period ZZ Ceti star through the analysis of photometric time series gathered on 7 nights between 1995 and 1996. The light curve displays a periodic variation with a period of ∼ 18 min in white light and the frequency analysis reveals a low frequency peak at ∼ 0.92 mHz with an amplitude varying from 0.007 to 0.025 mag present every night. BPM 24754 is the 28...
متن کاملFar Ultraviolet Study of the Hot White Dwarf in the Dwarf Nova WW Ceti
We present a synthetic spectral analysis of IUE archival and FUSE FUV spectra of the peculiar dwarf nova WW Ceti. During the quiescence of WW Ceti, a white dwarf with Twd ∼ 26, 000K ±1000K can account for the FUV flux and yields the proper distance. However, the best agreement with the observations is provided by a twotemperature white dwarf model with a cooler white dwarf at Twd = 25, 000K pro...
متن کاملDiscovery of seven ZZ Ceti stars using a new photometric selection method
We report the detection of non-radial g-mode oscillations in seven relatively bright (14.4 < B < 16.5) DA white dwarf stars from time-series photometry collected at the Nordic Optical Telescope (NOT) at Roque de Los Muchachos Observatory, Spain. The candidate variable stars were selected from preparatory photometric observations of objects from the Hamburg Quasar Survey (HQS) and from spectrosc...
متن کاملGravity Modes in Zz Ceti Stars. Ii. Eigenvalues and Eigenfunctions
We report on numerical calculations of nonadiabatic eigenvalues and eigenfunctions for g-modes in ZZ Ceti variables. The spectrum of overstable l \ 1 modes delineates the instability strip. Its blue edge occurs where for the n \ 1 mode. Here u is radian frequency and is about 4 times the uq c B 1 q c thermal time at the bottom of the surface convection zone. As a ZZ Ceti cools, its convection z...
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ژورنال
عنوان ژورنال: The Astrophysical Journal
سال: 2002
ISSN: 0004-637X,1538-4357
DOI: 10.1086/343085