Magnetized Rotating Isothermal Winds
Matthias J. Raives, Matthew S. B. Coleman, Todd A. Thompson
TL;DR
This study models magnetized, rotating, isothermal stellar winds using MHD simulations to analyze mass, angular momentum, and energy loss, with applications to star spindown, exoplanets, and neutron stars.
Contribution
It provides a comprehensive set of MHD simulations exploring the effects of rotation and magnetic fields on stellar winds, including 3D misaligned cases, advancing understanding of stellar and planetary wind dynamics.
Findings
Quantified mass, angular momentum, and energy loss rates across parameter space.
Demonstrated effects of magnetic and rotational axes misalignment in 3D.
Applied results to stellar spindown, exoplanetary atmospheres, and neutron star evolution.
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
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Taxonomy
TopicsSolar and Space Plasma Dynamics · Pulsars and Gravitational Waves Research · Stellar, planetary, and galactic studies