Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21710405g&link_type=abstract
American Astronomical Society, AAS Meeting #217, #104.05; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
1
Scientific paper
The environment of young stars is shaped by a complex interplay between stellar radiation, circumstellar material such as disks or envelopes, mass accretion flows onto the star, mass outflows from the star or the stellar disk, and jets accelerated near the star. High-energy radiation and particles are especially important in ionizing and heating the circumstellar gas and to drive chemical networks. Radio and soft X-ray radiation provide the best evidence for high-energy processes in young stars, and relevant observations suggest that much of the high-energy output is the consequence of frequent flaring. This concept predicts high-energy output not yet accessible to observations, such as non-thermal hard X-ray radiation beyond 10 keV, frequent coronal mass ejections, and high-energy particles in the stellar winds. On larger scales, outflows and jets produce high-energy radiation as well, although the heating mechanism is not entirely clear. Jet X-rays add to the circumstellar radiation field On the largest scales, one finds extended plasma bubbles in star-forming regions that contribute further X-ray emission to the stellar environment. I will discuss the above issues and present new observations that suggest an important role for high-energy processes in young stellar environments.
No associations
LandOfFree
The High-Energy Environment of Young Stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The High-Energy Environment of Young Stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The High-Energy Environment of Young Stars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1393210