X-rays from protostars

Details X-rays from protostars X-rays from protostars

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sfet.confe..14m&link_type=abstract

"Star Formation in the Era of Three Great Observatories, meeting abstracts from the conference held July 13-15, 2005 in Cambridg

Physics

Scientific paper

X-ray emission from young stars is most generally a proxy for their magnetic activity. In some cases, the X-rays come from magnetically channeled accretion shocks onto the stars, or from shocks between bipolar jets and the surrounding molecular clouds. In protostars, the X-ray emission may be more closely linked with magnetic interactions between the central, growing stars and their accretion disks, which play a central role in the accretion-ejection mechanism. The stage at which X-rays appear, which may regulate the coupling between the protostellar envelope and the magnetic fields, is however still debated. I will emphasize the importance of a multi-wavelength (X-IR-mm) approach to understand the evolution of protostars.

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