Periodic motions around pulsating stars

Details Periodic motions around pulsating stars Periodic motions around pulsating stars

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ap%26ss.202...11s&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 202, no. 1, p. 11-19.

Astronomy and Astrophysics

Astrophysics

6

Orbit Perturbation, Periodic Variations, Stellar Motions, Stellar Orbits, Stellar Oscillations, Orbital Elements, Stellar Luminosity

Scientific paper

The periodic motion of a test particle (dust, grain, or a larger body) around a pulsating star with a luminosity oscillation of small amplitude (featured by a small parameter B) is studied. The perturbations of all orbital elements are determined to first order in B, by using Delaunay-type canonical variables and a method whose bases were put forth by von Zeipel. According to the value of the ratio oscillation frequency/dynamic frequency, three possible situations are pointed out: nonresonant (NR), quasi-resonant (QR), and resonant (R). The solution of motion equations shows that only in the QR and R cases there are orbital parameters (argument of periastron and mean anomaly) affected by secular perturbations. These solutions (which indicate a secularly stable motion in a first approximation) are valid over prediction times of order B exp -1 in the NR case and B exp -1/2 in the QR and R cases. The theory may be applied to various astronomical situations.

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