X-ray Observations of AGB Stars with XMM-Newton

Details X-ray Observations of AGB Stars with XMM-Newton X-ray Observations of AGB Stars with XMM-Newton

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...203.3101k&link_type=abstract

American Astronomical Society Meeting 203, #31.01; Bulletin of the American Astronomical Society, Vol. 35, p.1253

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We report the preliminary results of an XMM-Newton observing program to determine the X-ray emission properties of a sample of well-studied AGB stars. Our goal is to set constraints on magnetic (dynamo) activity during mass-losing AGB evolutionary stages, and thereby test models wherein AGB star magnetic fields influence mass loss geometry and shape planetary nebulae. We detected X-ray emission from the Mira system, with a total EPIC count rate of ˜0.11 s-1. This emission may be due to accretion or magnetic activity associated with Mira B, a companion of uncertain nature located only 0.6" from the mass-losing AGB star. The X-ray spectrum of the Mira system displays emission from highly ionized Ne, and initial (single-component) spectral fits suggest a characteristic emission region temperature ˜10 MK, intervening absorbing column ˜3×1021 cm-2, and an intrinsic X-ray luminosity of ˜2×1029 ergs s-1. The (apparently single) star T Cas is undetected in X-rays. At the meeting, we will also report on results from observations of TX Cam, an AGB star for which the presence of relatively strong (5-10 G at ˜3 R⋆ ) magnetic fields has been inferred from maser polarization measurements in the radio.
This research is partly supported via NASA/GSFC grant NAG5--13158 (XMM-Newton Guest Observer program) to the Center for Imaging Science at Rochester Institute of Technology.

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