High Resolution Spectra of Stellar Winds in Very Young Massive Stars

Details High Resolution Spectra of Stellar Winds in Very Young Massive Stars High Resolution Spectra of Stellar Winds in Very Young Massive Stars

Jan 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003rmxac..15..220s&link_type=abstract

Winds, Bubbles, and Explosions: a conference to honor John Dyson, Pátzcuaro, Michoacán, México, September 9-13, 2002 (Eds. S. J.

Astronomy and Astrophysics

Astronomy

3

Stars: Early Type, Stars: Clusters, Stars: Formation, Techniques: Spectroscopic, X-Rays: Stars

Scientific paper

We present a series of spectra from hot stars obtained with the high energy transmission grating spectrometer (HETGS) onboard the Chandra X-ray Observatory. Most of the selected stars are located at or near the centers of young star-forming regions, which include IC 1396, NGC 2362, and Orion. The median ages of these clusters range from 0.3 to 12 Myr. The X-ray properties of these young, hot stars are then compared to a highly resolved X-ray spectrum of the more evolved field star zeta Pup. Cluster stars with ages larger than 3 Myr show moderate temperatures and broad asymmetric lines. These properties are quite similar to what has been observed in zeta Pup and are consistent with X-rays produced by shock instabilities in a radiation-driven wind. Stars with ages significantly less than 1 Myr, as found in the Orion Trapezium, show completely different characteristics. Here most of the X-ray flux shows very high temperatures and the X-ray lines are narrow and unresolved. This strongly indicates that the X-ray properties are dominated by magnetic field effects.

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