Magnetic flaring in pre-main sequence stars
| dc.creator | Feigelson, Eric D. | |
| dc.date | 2001-02-19 | |
| dc.date.accessioned | 2026-07-07T01:57:44Z | |
| dc.date.available | 2026-07-07T01:57:44Z | |
| dc.description | Observations of nearby star forming clouds with imaging X-ray telescopes have revealed that X-ray emission is elevated $10^1-10^4$ 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. | |
| dc.description | 10 pages, 2 figures. To appear in "Magnetic Fields Across the Hertzsprung-Russell Diagram" (G. Mathys et al. eds), ASP conf, in press | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0102326 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0102326 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/2507 | |
| dc.subject | Astrophysics | |
| dc.title | Magnetic flaring in pre-main sequence stars | |
| dc.type | text |