X-rays from Young Massive Stars

Details X-rays from Young Massive Stars X-rays from Young Massive Stars

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21710403c&link_type=abstract

American Astronomical Society, AAS Meeting #217, #104.03; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

O stars are powerful sources of X-ray emission and are often the strongest X-ray sources in young clusters and SFRs. Massive stars are not magnetically active, even in the minority of cases where they have detectable magnetic fields. Rather, their X-ray emission is caused by one (or more) of three mechanisms: embedded wind shocks in all O stars, colliding wind shocks in close binaries, and magnetically channeled wind shocks in massive stars with strong dipole magnetic fields. I will discuss these mechanisms and their manifestations in three specific examples: the O2 supergiant HD 93129A in Trumpler 14, Kleinman's Anonymous Star in M17, and theta1 Ori C in the Orion Nebula Cluster.

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