Determining the Nature of the SS 433 Binary from an X-ray Spectrum During Eclipse
We 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 obser...
| Main Authors: | , , , , |
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| Other Authors: | |
| Format: | Article |
| Language: | en_US |
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IOP Publishing
2012
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| Online Access: | http://hdl.handle.net/1721.1/72202 https://orcid.org/0000-0002-5769-8441 |
| _version_ | 1810991166549655552 |
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| author | Lopez, Laura A. Canizares, Claude R. Schulz, Norbert S. Kane, Julie F. Marshall, Herman |
| author2 | Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences |
| author_facet | Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences Lopez, Laura A. Canizares, Claude R. Schulz, Norbert S. Kane, Julie F. Marshall, Herman |
| author_sort | Lopez, Laura A. |
| collection | MIT |
| description | We 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. |
| first_indexed | 2024-09-23T12:49:22Z |
| format | Article |
| id | mit-1721.1/72202 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T12:49:22Z |
| publishDate | 2012 |
| publisher | IOP Publishing |
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| spelling | mit-1721.1/722022022-10-01T11:18:21Z Determining the Nature of the SS 433 Binary from an X-ray Spectrum During Eclipse Lopez, Laura A. Canizares, Claude R. Schulz, Norbert S. Kane, Julie F. Marshall, Herman Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research Canizares, Claude C. Marshall, Herman Lee Canizares, Claude R. Schulz, Norbert S. Kane, Julie F. We 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. United States. National Aeronautics and Space Administration. (Contract Number NAS8- 38249) Smithsonian Astrophysical Observatory (Chandra X-ray Center (U.S.)) (Contract SV3- 73016) National Science Foundation (U.S.). Graduate Research Fellowship Program 2012-08-17T20:09:42Z 2012-08-17T20:09:42Z 2006-05 2006-01 Article http://purl.org/eprint/type/JournalArticle 0004-637X 1538-4357 http://hdl.handle.net/1721.1/72202 Lopez, 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. https://orcid.org/0000-0002-5769-8441 en_US http://dx.doi.org/10.1086/506174 Astrophysical Journal Article 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. application/pdf IOP Publishing arVix |
| spellingShingle | Lopez, Laura A. Canizares, Claude R. Schulz, Norbert S. Kane, Julie F. Marshall, Herman Determining the Nature of the SS 433 Binary from an X-ray Spectrum During Eclipse |
| title | Determining the Nature of the SS 433 Binary from an X-ray Spectrum During Eclipse |
| title_full | Determining the Nature of the SS 433 Binary from an X-ray Spectrum During Eclipse |
| title_fullStr | Determining the Nature of the SS 433 Binary from an X-ray Spectrum During Eclipse |
| title_full_unstemmed | Determining the Nature of the SS 433 Binary from an X-ray Spectrum During Eclipse |
| title_short | Determining the Nature of the SS 433 Binary from an X-ray Spectrum During Eclipse |
| title_sort | determining the nature of the ss 433 binary from an x ray spectrum during eclipse |
| url | http://hdl.handle.net/1721.1/72202 https://orcid.org/0000-0002-5769-8441 |
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