The First Evidence for Multiple Pulsation Axes: A New roAp Star in the Kepler Field, KIC 10195926

D. W. Kurtz, M. S. Cunha, H. Saio, L. Bigot, L. A. Balona, V. G. Elkin, H. Shibahashi, I. M. Brandão, K. Uytterhoeven, S. Frandsen, S. Frimann, A. Hatzes, T. Lüftinger, M. Gruberbauer, H. Kjeldsen, J. Christensen-Dalsgaard, S. D. Kawaler

Resumo
This conference talk introduced the characteristics of the rapidly oscillating Ap stars, then discussed a new rapidly oscillating Ap star discovered and published by Working Group 5 of the Kepler Asteroseismic Science Consortium, KIC 10195926. This star shows two pulsation modes with periods that are amongst the longest known for roAp stars at 17.1 min and 18.1 min, indicating that the star is near the terminal-age main-sequence. The principal pulsation mode is an oblique dipole mode that shows a rotationally split frequency septuplet that provides information on the geometry of the mode. The secondary mode also appears to be a dipole mode with a rotationally split triplet, but within the improved oblique pulsator model these two modes cannot have the same axis of pulsation. This is the first time for any pulsating star that evidence has been found for separate pulsation axes for different modes.

Progress in Solar/Stellar Physics with Helio- and Asteroseismology.
(Eds.) H. Shibahashi, M. Takata, A.E. Lynas-Gray

Astronomical Society of the Pacific
Vol. 462, Página 180
2012

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