Colors in Eddington: implications for mode identification

Details Colors in Eddington: implications for mode identification Colors in Eddington: implications for mode identification

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.485..103g&link_type=abstract

In: Proceedings of the First Eddington Workshop on Stellar Structure and Habitable Planet Finding, 11 - 15 June 2001, Córdoba, S

Physics

2

Stars: Pulsations, Stars: Photometry, Stars: Delta Scuti

Scientific paper

Theoretical radial and non-radial modes of low n orders in main sequence stars, like δ Scuti and β Cephei, do not show regular pattern in their power spectra. Although Barban et al. (2001) have shown that assuming an amplitude distribution certain patterns could be recovered, a method to identify the mode is needed in order to perform real asteroseismology of these objects. Examples are given in the literature where for several stars showing many periods: FG Vir (24): Breger et al. (1999), XX Pyx (22): Handler et al. (2000), 4 CVn (30): Breger et al. (1999) and BI CMi (20): Breger et al. (2002), a physical modeling was not successful, the reason being the mode identification. Multicolor photometry, as well as line profile spectroscopy, have been the usual methods to identify modes. In this work we will focus on the capabilities of color information to discriminate the different angular degrees l of the spherical harmonic associated to a radial or non-radial mode excited in a given δ Scuti pulsating star. Some numerical simulations are also presented for the exoplanetary camera in the space mission COROT where it is shown that, under some physical assumptions, color can be very important in order to identify the angular degree l. Furthermore colors can give relevant information of the non-adiabatic properties of some pulsating stars which, in the case of the δ Scuti stars, are related with the treatment of the convection. Arguments are also given to support the inclusion of color information in Eddington.

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