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dc.contributor.authorLopez, Laura A.
dc.contributor.authorMarshall, Herman Lee
dc.contributor.authorCanizares, Claude R.
dc.contributor.authorSchulz, Norbert S.
dc.contributor.authorKane, Julie F.
dc.date.accessioned2012-08-17T20:09:42Z
dc.date.available2012-08-17T20:09:42Z
dc.date.issued2006-05
dc.date.submitted2006-01
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://hdl.handle.net/1721.1/72202
dc.description.abstractWe test the physical model of the relativistic jets in the Galactic X-ray binary SS 433 proposed in our previous paper using additional observations from the Chandra High Energy Transmission Grating Spectrometer. These observations sample two new orbital/precessional phase combinations. In the observation near orbital phase zero, the H- and He-like Fe lines from both receding and approaching jets are comparably strong and unocculted while the He-like Si line of the receding jet is significantly weaker than that of the approaching jet. This condition may imply that the cooler parts of the receding jet are eclipsed by the companion. The X-ray spectrum from this observation has broader emission lines than obtained in Paper I that may arise from the divergence of a conical outflow or from Doppler shift variations during the observation. Using recent optical results, along with the length of the unobscured portion of the receding jet assuming adiabatic cooling, we calculate the radius of the companion to be 9.6 ± 1.0 R[subscript ☉], about one-third of the Roche lobe radius. For a main-sequence star, this corresponds to a companion mass of 35 ± 7 M[subscript ☉], giving a primary source mass of 20 ± 5 M[subscript ☉]. If our model is correct, this calculation indicates that the compact object is a black hole, and accretion occurs through a wind process. In a subsequent paper, we will examine the validity of the adiabatic cooling model of the jets and test the mode of line broadening.en_US
dc.description.sponsorshipUnited States. National Aeronautics and Space Administration. (Contract Number NAS8- 38249)en_US
dc.description.sponsorshipSmithsonian Astrophysical Observatory (Chandra X-ray Center (U.S.)) (Contract SV3- 73016)en_US
dc.description.sponsorshipNational Science Foundation (U.S.). Graduate Research Fellowship Programen_US
dc.language.isoen_US
dc.publisherIOP Publishingen_US
dc.relation.isversionofhttp://dx.doi.org/10.1086/506174en_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.sourcearVixen_US
dc.titleDetermining the Nature of the SS 433 Binary from an X-ray Spectrum During Eclipseen_US
dc.typeArticleen_US
dc.identifier.citationLopez, Laura A. et al. “Determining the Nature of the SS 433 Binary from an X‐Ray Spectrum During Eclipse.” The Astrophysical Journal 650.1 (2006): 338–349.en_US
dc.contributor.departmentdeleteen_US
dc.contributor.departmentKavli Institute for Astrophysics and Space Researchen_US
dc.contributor.departmentMassachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciencesen_US
dc.contributor.departmentMassachusetts Institute of Technology. Department of Physicsen_US
dc.contributor.approverCanizares, Claude C.
dc.contributor.mitauthorMarshall, Herman Lee
dc.contributor.mitauthorCanizares, Claude R.
dc.contributor.mitauthorSchulz, Norbert S.
dc.contributor.mitauthorKane, Julie F.
dc.relation.journalAstrophysical Journalen_US
dc.eprint.versionAuthor's final manuscripten_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dspace.orderedauthorsLopez, Laura A.; Marshall, Herman L.; Canizares, Claude R.; Schulz, Norbert S.; Kane, Julie F.en
dc.identifier.orcidhttps://orcid.org/0000-0002-5769-8441
mit.licensePUBLISHER_POLICYen_US


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