Magnetized Rotating Isothermal Winds
Solar and Stellar Astrophysics
2023-11-01 v2 High Energy Astrophysical Phenomena
Abstract
We consider the general problem of a Parker-type non-relativistic isothermal wind from a rotating and magnetic star. Using the magnetohydrodynamics (MHD) code athena++, we construct an array of simulations in the stellar rotation rate and the isothermal sound speed , and calculate the mass, angular momentum, and energy loss rates across this parameter space. We also briefly consider the three dimensional case, with misaligned magnetic and rotation axes. We discuss applications of our results to the spindown of normal stars, highly-irradiated exoplanets, and to nascent highly-magnetic and rapidly-rotating neutron stars born in massive star core collapse.8
Cite
@article{arxiv.2302.05462,
title = {Magnetized Rotating Isothermal Winds},
author = {Matthias J. Raives and Matthew S. B. Coleman and Todd A. Thompson},
journal= {arXiv preprint arXiv:2302.05462},
year = {2023}
}
Comments
19 pages, 13 figures; v2: published version after minor revisions