New Aspects of the Mode Identification in the Eclipsing Binaries

Details New Aspects of the Mode Identification in the Eclipsing Binaries New Aspects of the Mode Identification in the Eclipsing Binaries

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jena.confq..18g&link_type=abstract

"JENAM-2007, "Our non-stable Universe", held 20-25 August 2007 in Yerevan, Armenia. Abstract book, p. 18-18"

Computer Science

Scientific paper

The mode identification is the most difficult problem in asteroseismology. Most of the identification techniques operate with the light integrated over the whole disk, while the spatial filtration method in eclipsing binaries with pulsating components (Gamarova et al., 2003, Rodriguez et al., 2004) gives a possibility to resolve the stellar disk. The attempts of the mode identification using this technique performed recently (Rodriguez et al., 2004) revealed the set of problems complicating the application (see Berger, 2005 and comments). Among them are: 1. the unknown orientation of the pulsational axis of the pulsating star; 2. possible multiperiodicity. We should note the case of the existence of “invisible” modes. For example, in the assumption that the pulsation axis coincides with the rotation axis which is perpendicular to the orbital plane axis the l+m=odd modes are not visible in the integrated light. But during the eclipse the growth of amplitude is expected for these modes and the pulsation light variations of the “visible” mode are violated; 3. the influence of the gas stream and non-stable gas envelope on the observed light curves on the case of semidetached eclipsing binary systems undergoing the mass-transfer. In our poster we present the modeled variations taking into account the possible inclination of the pulsation axis to the rotation one. The case of the “invisible” modes is modeled and the influence of the circumstellar structures on the observed pulsational characteristics is discussed.

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