Results 261 to 270 of about 501 (275)
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Polarimetric observations of pulsating variable stars
Astrophysics, 1996Results are presented for polarimetric observations of 17 red giants and supergiants, of which nine are long-period Mira variables, five are semiregular variables (SR), and three are slowly fluctuating variables (Lb). Light polarization is detected for eight stars, seven of them for the first time.
N. D. Melikian, M. A. Eritsian
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The Pulsation Theory of Variable Stars
Nature, 1949CEPHEID (variable stars—the name given to stars which behave like δ Cephei—have played a distinguished part in modern astronomy. Their most characteristic feature—that there is a definite relation between period and median absolute luminosity—was discovered by Miss Leavitt in 1912 when investigating the Lesser Magellanic Cloud.
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Pulsating variable white dwarf (Helium) stars and solitons
Astrophysics and Space Science, 1991Photometric emissions from pulsating variable white dwarf (GD 358) stars having helium atmosphere provide optical imprints of the intermediate phase of some of the dying stars and thus establishes a direct link with the evolutionary history and compositional structure of variable stars.
J. G. Negi, K. N. N. Rao
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2003
Of all the variable stars, pulsating stars, especially the Mira (M) and semiregular (SR) stars, are probably the most observed by amateur astronomers. This claim is easily understood when you consider that well over 22,000 pulsating variable stars are cataloged within the GCVS and several million pulsating stars probably exist within the Milky Way.
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Of all the variable stars, pulsating stars, especially the Mira (M) and semiregular (SR) stars, are probably the most observed by amateur astronomers. This claim is easily understood when you consider that well over 22,000 pulsating variable stars are cataloged within the GCVS and several million pulsating stars probably exist within the Milky Way.
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C. The Continuous Spectrum of Pulsating Variable Stars
Symposium - International Astronomical Union, 1967Pecker:The topic to be considered today is the continuous spectrum of certain stars, whose variability we attribute to a pulsation of some part of their structure. Obviously, this continuous spectrum provides a test of the pulsation theory to the extent that the continuum is completely and accurately observed and that we can analyse it to infer the ...
J. B. Oke, C. A. Whitney
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Construction of the Database for Pulsating Variable Stars
Chinese Astronomy and Astrophysics, 2012Abstract A database for pulsating variable stars is constructed to favor the study of variable stars in China. The database includes about 230,000 variable stars in the Galactic bulge, LMC and SMC observed in an about 10 yr period by the MACHO(MAssive Compact Halo Objects) and OGLE(Optical Gravitational Lensing Experiment) projects. The software used
Bing-Qiu Chen, Ming Yang, Bi-Wei Jiang
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Pulsation Modes in Small‐Amplitude Red Variable Stars
Publications of the Astronomical Society of the Pacific, 1998We have investigated the pulsation modes of small‐amplitude red variables with well‐determined periods and accurate Hipparcos parallaxes by comparing observational and theoretical Q‐values. In our sample of 13 stars, one appears to be pulsating in the third overtone, nine in the first or second overtone, and three in the fundamental or first overtone ...
John R. Percy, Michael Parkes
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Variability, Pulsations and Mass Loss of Evolved Stars
Proceedings of the International Astronomical Union, 2017AbstractEvolved low- and intermediate-mass stars that have reached the Asymptotic Giant Branch (AGB) phase tend to show pronounced long-period variability due to large-amplitude pulsations. Those pulsations are considered to play a key role in triggering mass loss through massive dusty winds.
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Variability of long-period pulsating stars. II. Additional parameters for classifying stars
Astrophysics, 2006Results are presented from an analysis of observations in a sample of 53 long-period pulsating stars (44 of which are Mira-type and 9 are semiregular variables). A catalog of the characteristics of the individual pulsation cycles of the light curves is obtained for these stars.
V. I. Marsakova, I. L. Andronov
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D. The Line Spectrum of Pulsating Variable Stars
Symposium - International Astronomical Union, 1967(Ed. note:Encouraged by the success of the more informal approach in Christy's presentation, we tried an even more extreme experiment in this session, I-D. In essence, Kraft held the floor continuously all morning, and for the hour and a half afternoon session, serving as a combined Summary-Introductory speaker and a marathon-moderator of a running ...
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