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The stellar structure is usually assumed to be spherically symmetric, so the horizontal (i.e. non-radial) component of the oscillations is described by spherical harmonics, indexed by an angular degree and azimuthal order . In non-rotating stars, modes with the same angular degree must all have the same frequency because there is no preferred axis.
Stellar dynamics is the branch of astrophysics which describes in a statistical way the collective motions of stars subject to their mutual gravity. The essential difference from celestial mechanics is that the number of body N ≫ 10. {\displaystyle N\gg 10.}
He has made significant contributions to both fields, including predicting the oscillation of Sun-like stars in 1983. [1] He is the head of "Rumudvalget" (the committee of space of the Danish Ministry of Science, Technology and Innovation) [ 2 ] and the Stellar Astrophysics Centre (SAC) supported by the Danish National Research Foundation.
Timothy R. Bedding FAA (born 21 July 1966) is an Australian astronomer known for his work on asteroseismology, the study of stellar oscillations.In particular, he contributed to the first detections of solar-like oscillations in stars such as eta Bootis, beta Hydri and alpha Centauri. [1]
Paul Ledoux (8 August 1914 – 6 October 1988 [2]) was a Belgian astrophysicist best known for his work on stellar stability and variability. With Theodore Walraven, he co-authored a seminal work on stellar oscillations. [3]
The following shows a similar visualization of the period doubling cascade to chaos for a sequence of stellar models that differ by their average surface temperature T. The graph shows triplets of values of the stellar radius (R i, R i+1, R i+2) where the indices i, i+1, i+2 indicate successive time intervals.
Buzasi's research interests include computational astrophysics, helioseismology, asteroseismology, oscillations in massive stars, characterization of solar analogs, gyrochronology and binary systems, stellar magnetic field structures and interactions in active stars, and astronomical instrumentation. [9]
They suggested that the most plausible explanation for the variability of Arcturus is stellar oscillations. [30] Asteroseismological measurements allow direct calculation of the mass and radius, giving values of 0.8 ± 0.2 M ☉ and 27.9 ± 3.4 R ☉. This form of modelling is still relatively inaccurate, but a useful check on other models. [31]