Hot Gas at 10^7 K, Fe K Reflection, Ongoing Non-thermal Outbursts, Jet Formation and 10^6 K Shocks in the Symbiotic Binary R Aqr.

Details Hot Gas at 10^7 K, Fe K Reflection, Ongoing Non-thermal Outbursts, Jet Formation and 10^6 K Shocks in the Symbiotic Binary R Aqr. Hot Gas at 10^7 K, Fe K Reflection, Ongoing Non-thermal Outbursts, Jet Formation and 10^6 K Shocks in the Symbiotic Binary R Aqr.

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...1e..45k&link_type=abstract

Cosmic Particle Acceleration, 26th meeting of the IAU, Joint Discussion 1, 16-17 August, 2006, Prague, Czech Republic, JD01, #45

Computer Science

Scientific paper

X-ray and VLA radio observations of the evolved binary system R Aqr over the past several years have revealed a rich variety of phenomena, in addition to observations spanning decades in radio, optical and IR. These observations argue more and more strongly for a binary system with a compact companion, with an accretion disk, producing jets along the symmetry axis of the compact object or accretion disk. Chandra observations at epochs 2000.7, 2004.0 and 2005.8 show bright regions of 10^6 K thermal x-ray emission 1400-5000 AU moving out from the central binary at ~600 km s^-1, aligned with a bipolar axis extending from the star at PA ~35°/215°. These are quite similar to the Herbig-Haro emission associated with young stellar objects. There is also cool Fe line emission from an unresolved point source at the star. In the latter epochs new synchrotron inner jets at ~600 AU are being ejected, appearing in radio and x-rays at the same PA. A second component in the unresolved central source has a spectrum that indicates hot gas at ~7 x 10^7 K, heavily absorbed with a column density of ~4 x 10^23 cm^-2. We also show results of a 2005.5 XMM-Newton observation that add high resolution grating spectroscopy improve our understanding of the outer 10^6 K emitting regions. Taken together, the observations reveal the source of the energy that has been ejecting material observed for decades in the IR, optical and UV, a compact object, an accretion disk, and material ejected at high speeds along the axis of rotation. All this from a nearby (200 pc) low mass star system.

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