Magnetic flaring in pre-main sequence stars
Abstract
Observations of nearby star forming clouds with imaging X-ray telescopes have revealed that X-ray emission is elevated above main sequence levels in low-mass pre-main sequence (PMS) stars. The variability and spectral X-ray evidence, together with circularly polarized radio continuum flares seen in a few cases, strongly argues for an origin in magnetic reconnection flares. These high levels of magnetic activity are present from the earliest protostellar phase to the main sequence. After a brief review of past observations, three astrophysical issues are raised: the location of the flaring magnetic fields, the origin of these fields, and the effects of flare high-energy photons and particles on the environs. New results from Chandra observations of a well-defined samples of PMS solar analogues are presented, giving an improved view of magnetic flaring in the early Sun.
Cite
@article{arxiv.astro-ph/0102326,
title = {Magnetic flaring in pre-main sequence stars},
author = {Eric D. Feigelson},
journal= {arXiv preprint arXiv:astro-ph/0102326},
year = {2007}
}
Comments
10 pages, 2 figures. To appear in "Magnetic Fields Across the Hertzsprung-Russell Diagram" (G. Mathys et al. eds), ASP conf, in press