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L.A. Lopez, H.L. Marshall, J.F. Kane, C.R. Canizares, N.S. Schulz (MIT CSR)
We test the physical model of the jets in SS 433 that was proposed by Marshall, Canizares and Schulz using additional observations with the Chandra High Energy Transmission Grating Spectrometer. The new observations sampled different precessional and orbital phases, offering different views of the jets through local material. Preliminary results indicate that the jet thermal structure has not changed drastically. The emission lines are broader than expected in one observation, so the jet opening angle has increased by a factor of two. In two observing periods, the low energy lines were substantially weaker, probably due to obscuration. These two observations were obtained at precession phases where the jets "cross over" so the obscuring region could be a very thick disk. The jets are not eclipsed at orbital phase 0, placing a stringent limit on the size of the companion because the orbital inclination is well known and the length of the jets are well determined from physical modelling using the X-ray spectrum.
This work was supported in part by the Smithsonian Astrophysical Observatory (SAO) contract SVI-61010 for the Chandra X-Ray Center (CXC) and NASA contract NAS8-39073.
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Bulletin of the American Astronomical Society, 35 #3
© 2003. The American Astronomical Soceity.