Titlebook: Stellar Pulsations; Impact of New Instru J.C. Suárez,R. Garrido,J. Christensen-Dalsgaard Book 2013 Springer-Verlag Berlin Heidelberg 2013 A

信條

1570-6591 s also discussed. These Proceedings are distinguished by?the format of the conference, which brings together a variety of related but different topics not found in other meetings of this nature..978-3-642-44326-8978-3-642-29630-7Series ISSN 1570-6591 Series E-ISSN 1570-6605

biosphere

Book 2013lsations (Granada, September 2011). These results are leading to a re-appraisal of our views on stellar pulsation in some stars and posing some new and unexpected challenges. The very important and exciting role played by innovative ground-based observational techniques, such as interferometric meas

Hemoptysis

Vibrational Instability of Metal-Poor Low-Mass Main-Sequence Starsthose of Pop I stars, the stars showing γ Dor-type pulsation are substantially less massive than in the case of Pop I stars. We demonstrate that those modes are unstable for about 1 .. stars in the metal-poor case.

咽下

Non-radial Pulsation and Magnetic Fields of OB Stars the large-scale structures in the stellar wind. Results of searching for the polarimetric line profile variability (pLPV) in the spectra of OB stars are also reported. We find that the pattern of LPV can differ for the left and right polarized components of stellar radiation.

晚間

Some Thoughts About the Blazhko Effect for RR Lyrae Variable Pulsationsmaterial opacity an its dependence on temperature and density. Current linear theory for pulsation calculations using my much improved pulsation code show that two beating modes (one radial and another nonradial) may exist for an explanation of those few pulsating RR Lyrae, amplitude varying variable stars.

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Minutes

Stellar Pulsations and Stellar Evolution: Conflict, Cohabitation, or Symbiosis?s of stellar physics are pointed out as well, for which it is hoped that seismology—or in general the analysis of stellar pulsations—will help to resolve them. The limits of this symbiosis will be discussed as well.

Bronchial-Tubes

冥界三河

Traditional Approximation for Low-Frequency Modes in Rotating Stars and A Working Hypothesis About Ere, we point out that very low frequency oscillations become leaky waves. A working hypothesis is then proposed to explain mass loss in Be stars as episodic wave leakage associated with gradual angular-momentum transport due to prograde modes.

FRET

Modelling Stellar Convection and Pulsation in Multidimensions Using the ANTARES Codesfer. We then present the basic parameters of the Cepheid we study more closely. For that star we provide a short discussion of patterns of the . and the . convection zones and the interaction with pulsation seen in the . work or atmospheric structures.