Mathematics – Logic
Scientific paper
Jan 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004esasp.538..117g&link_type=abstract
In: Second Eddington Workshop: Stellar structure and habitable planet finding, 9 - 11 April 2003, Palermo, Italy. Edited by F. F
Mathematics
Logic
1
Stars: Structure, Pulsation, Photometry
Scientific paper
Colour information in asteroseismology has proved to be very useful not only for mode identification but also to supply other physical information which is not contained in the frequencies themselves. Solar and solar-like asteroseismology is based on the regular patterns shown by the oscillation frequencies in the asymptotic regime. The "avoided crossing" phenomenon can destroy this regular pattern and make useless the asteroseismological techniques based on large and small differences and on the so called "echelle" diagrams. Rotation, even at intermediate (and common) velocities, introduces some degree of asymmetry and coupling which complicate even more any expected regular pattern. A method for mode identification is then required for such cases and, in practice, for most of the κ-driven non-radial pulsating stars. Colour can supply this method through the linearization of the photometric variations of a non-radially pulsating star. The formula contains terms which require a deep understanding of the stellar atmosphere (limb darkening coefficients, first derivatives of photometric colours, local temperature and gravity variations and phase lags) but contains also information on the degree of the associated spherical harmonic, l, which is the clue for the mode identification. The physical observables, amplitude ratios and phase differences for different photometric bands, can then be used to constrain not only model atmospheres but also non-adiabatic pulsation codes. This contribution aims to present the last results on the field and to motivate the inclusion of colour information in the Eddington capabilities. Some examples are given where it is shown that colours, properly defined, are able to discriminate the l-values of a non-radially pulsating star.
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