Toward Self-consistent Angular Momentum Transport in Pulsating Massive Stars

Details Toward Self-consistent Angular Momentum Transport in Pulsating Massive Stars Toward Self-consistent Angular Momentum Transport in Pulsating Massive Stars

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1170..355t&link_type=abstract

STELLAR PULSATION: CHALLENGES FOR THEORY AND OBSERVATION: Proceedings of the International Conference. AIP Conference Proceedin

Physics

2

Cepheids, Hydrodynamics, Pulsations, Oscillations, And Stellar Seismology

Scientific paper

I report on preliminary results from an ongoing project that explores angular momentum transport by unstable pulsation modes in massive stars. After briefly reviewing the underlying formalism for this transport, and describing a numerical code that implements it, I present an example simulation for a 5 Msolar model star. I show that prograde = m = 2 g modes, unstable due to the iron-bump κ mechanism, can spin down the surface layers of the star by 25% over a short (~100-year) timescale. The resulting shear layer separating the surface from interior acts to switch off the κ-mechanism instability, providing a natural way of limiting mode amplitudes. This process may have a role to play in the mode selection mechanism of pulsating massive stars.

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