The Detection of Gyrosynchrotron Emission from IRC+10216

Details The Detection of Gyrosynchrotron Emission from IRC+10216 The Detection of Gyrosynchrotron Emission from IRC+10216

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...203.5905w&link_type=abstract

American Astronomical Society Meeting 203, #59.05; Bulletin of the American Astronomical Society, Vol. 35, p.1305

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Scientific paper

We have used the NRAO Very Large Array (VLA) to search for OH and water maser emission from the late-type carbon star IRC+10216 (CW Leo). Although we did not detect maser emission from either OH or water, we detected continuum emission at 18 cm for the first time in this star. Based on a comparison with continuum emission at other frequencies and the time variability of the emission source, we conclude that synchrotron or gyrosynchrotron emission from the stellar magnetosphere is the current best explanation of the radio emission from this star.
The NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Part of this research was carried out under the auspices of the National Science Foundation's Research Experience for Teachers (RET) program at the NRAO, and we gratefully acknowledge the funding for this program.

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