The outbursts of R Aquarii - a symbiotic star, an X-ray binary, or a nanoquasar?

Details The outbursts of R Aquarii - a symbiotic star, an X-ray binary, or a nanoquasar? The outbursts of R Aquarii - a symbiotic star, an X-ray binary, or a nanoquasar?

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009cfdd.confe.129k&link_type=abstract

Chandra's First Decade of Discovery, Proceedings of the conference held 22-25 September, 2009 in Boston, MA. Edited by Scott Wo

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Stellar Spectroscopy

Scientific paper

Chandra is an unparalleled facility for resolving the behavior of R Aquarii. Chandra's sub arc second angular resolution allow us to resolve the X-ray jets and lobes, and its energy resolution lets us delineate regions of thermal and nonthermal emission from this variegated system. Chandra and other major observatories have observed R Aquarii over the Chandra decade, recording outbursts across the spectrum from radio to X-rays. We review the observations and discuss thermal and non thermal emission mechanisms in the jets, lobes and central source. The central engine is known to contain a Mira-type variable red giant star and a putative white dwarf. R Aquarii has refused so far to yield information on its binary period, or compelling evidence for an accretion disk. There is tantalizing evidence for a rotation period in the central source of 29 min on one observing occasion, that tempts us to believe the WD is magnetic. The many facets of R Aquarii's emission invite comparisons with extragalactic quasars and galactic microquasars, with the difference that observed velocities in the R Aquarii system are generally nonrelativistic, even comparable to Solar wind speeds in some cases. All in all, R Aquarii is a very versatile laboratory for study of a wide range of high energy phenomena, and being only 200 pc distant can be studied in great detail.

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