Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21811001g&link_type=abstract
American Astronomical Society, AAS Meeting #218, #110.01; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
X-rays accompany most phases of star formation and stellar evolution, revealing unexpected diversity and offering unequaled access to high-energy physical mechanisms in stellar environments. X-ray radiation is a foremost diagnostic for magnetic fields and hot, coronal plasma in cool and pre-main sequence stars; X-ray spectroscopy has been used to study composition and compositional anomalies in cool stars as well as densities of coronal sources, including giant flares. However, Chandra has also contributed to the discovery and characterization of X-ray sources related to accretion and outflow processes in young stars. Specifically, magnetospheric accretion is held responsible for an excess of cool plasma and dense X-ray sources probably related to shock heating in the accretion streams. X-ray sources have also been found both in Herbig-Haro objects and in jets very close to T Tauri stars and protostars. In both cases, shocks developing at the interface with the interstellar medium or within the jet flows, perhaps even in the acceleration and collimation region, may be at the origin of the efficient heating although magnetic heating processes may be a viable alternative. Moving toward more massive pre-main sequence stars, energetic processes could also be related to magnetically confined wind shocks. I will discuss these subjects in the context of Chandra findings, concentrating on low- and intermediate mass stars.
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