Shock Heating by the SS 433 Relativistic Jets

Details Shock Heating by the SS 433 Relativistic Jets Shock Heating by the SS 433 Relativistic Jets

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009cfdd.confe.149m&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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We examine the hypothesis that the X-ray emission from the SS 433 jets results from shock heating by relativistic jets. The main body of evidence comes from high resolution X-ray spectra using the Chandra HETGS. The X-ray spectra show many signatures of shock heating, by analogy to other systems where lower velocity shocks are involved. From density and temperature estimates from the X-ray spectra, the X-ray emission must originate very close to these shocks and the hot gas is advected downstream, cooling significantly via radiative and adiabatic losses. Comparing spectra taken during primary eclipse, it is clear that only the highest temperature portion of the X-ray emitting regions are blocked, placing an additional constraint on the location of the shocks. By relating contemporaneous X-ray and optical observations, we demonstrate that the optical emission originates much further downstream, past the point where the jet starts to clump.

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