NATURE OF THE EXTREME ULTRALUMINOUS X-RAY SOURCES
In this proof-of-concept study we demonstrate that in a binary system mass can be transferred toward an accreting compact object at an extremely high rate. If the transferred mass is efficiently converted to X-ray luminosity (with disregard of the classical Eddington limit) or if the X-rays are focu...
| المؤلفون الرئيسيون: | , , , |
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| مؤلفون آخرون: | |
| التنسيق: | مقال |
| اللغة: | en_US |
| منشور في: |
IOP Publishing
2015
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| الوصول للمادة أونلاين: | http://hdl.handle.net/1721.1/100049 https://orcid.org/0000-0001-9147-1841 |
| _version_ | 1826203291315339264 |
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| author | Wiktorowicz, Grzegorz Belczynski, Krzysztof Sobolewska, Malgorzata Sadowski, Aleksander B |
| author2 | MIT Kavli Institute for Astrophysics and Space Research |
| author_facet | MIT Kavli Institute for Astrophysics and Space Research Wiktorowicz, Grzegorz Belczynski, Krzysztof Sobolewska, Malgorzata Sadowski, Aleksander B |
| author_sort | Wiktorowicz, Grzegorz |
| collection | MIT |
| description | In this proof-of-concept study we demonstrate that in a binary system mass can be transferred toward an accreting compact object at an extremely high rate. If the transferred mass is efficiently converted to X-ray luminosity (with disregard of the classical Eddington limit) or if the X-rays are focused into a narrow beam, then binaries can form extreme ultraluminous X-ray (ULX) sources with an X-ray luminosity of L[subscript X] ≳ 10[superscript 42] erg s[superscript -1]. For example, Lasota and King argued that the brightest known ULX (HLX-1) is a regular binary system with a rather low-mass compact object (a stellar-origin black hole (BH) or a neutron star (NS)). The predicted formation efficiencies and lifetimes of binaries with the very high mass transfer rates are large enough to explain all observed systems with extreme X-ray luminosities. These systems are not only limited to binaries with stellar-origin BH accretors. Notably, we have also identified such objects with NSs. Typically, a 10 M[subscript ʘ] BH is fed by a massive (~10 M[subscript ʘ]) Hertzsprung gap donor with Roche lobe overflow (RLOF) rate of ~10[superscript -3] M[subscript ʘ] yr[superscript -1] (≈2600[. over M][subscript Edd]). For NS systems the typical donors are evolved low-mass (~2 M[subscript ʘ]) helium stars with RLOF rate of ~10[superscript -2] MM[subscript ʘ] yr[superscript -1]. Our study does not prove that any particular extreme ULX is a regular binary system, but it demonstrates that any ULX, including the most luminous ones, may potentially be a short-lived phase in the life of a binary star. |
| first_indexed | 2024-09-23T12:34:19Z |
| format | Article |
| id | mit-1721.1/100049 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T12:34:19Z |
| publishDate | 2015 |
| publisher | IOP Publishing |
| record_format | dspace |
| spelling | mit-1721.1/1000492022-10-01T09:51:01Z NATURE OF THE EXTREME ULTRALUMINOUS X-RAY SOURCES Wiktorowicz, Grzegorz Belczynski, Krzysztof Sobolewska, Malgorzata Sadowski, Aleksander B MIT Kavli Institute for Astrophysics and Space Research Sadowski, Aleksander In this proof-of-concept study we demonstrate that in a binary system mass can be transferred toward an accreting compact object at an extremely high rate. If the transferred mass is efficiently converted to X-ray luminosity (with disregard of the classical Eddington limit) or if the X-rays are focused into a narrow beam, then binaries can form extreme ultraluminous X-ray (ULX) sources with an X-ray luminosity of L[subscript X] ≳ 10[superscript 42] erg s[superscript -1]. For example, Lasota and King argued that the brightest known ULX (HLX-1) is a regular binary system with a rather low-mass compact object (a stellar-origin black hole (BH) or a neutron star (NS)). The predicted formation efficiencies and lifetimes of binaries with the very high mass transfer rates are large enough to explain all observed systems with extreme X-ray luminosities. These systems are not only limited to binaries with stellar-origin BH accretors. Notably, we have also identified such objects with NSs. Typically, a 10 M[subscript ʘ] BH is fed by a massive (~10 M[subscript ʘ]) Hertzsprung gap donor with Roche lobe overflow (RLOF) rate of ~10[superscript -3] M[subscript ʘ] yr[superscript -1] (≈2600[. over M][subscript Edd]). For NS systems the typical donors are evolved low-mass (~2 M[subscript ʘ]) helium stars with RLOF rate of ~10[superscript -2] MM[subscript ʘ] yr[superscript -1]. Our study does not prove that any particular extreme ULX is a regular binary system, but it demonstrates that any ULX, including the most luminous ones, may potentially be a short-lived phase in the life of a binary star. 2015-11-24T20:44:52Z 2015-11-24T20:44:52Z 2015-08 2015-03 Article http://purl.org/eprint/type/JournalArticle 1538-4357 0004-637X http://hdl.handle.net/1721.1/100049 Wiktorowicz, Grzegorz, Małgorzata Sobolewska, Aleksander Sadowski, and Krzysztof Belczynski. “NATURE OF THE EXTREME ULTRALUMINOUS X-RAY SOURCES.” The Astrophysical Journal 810, no. 1 (August 25, 2015): 20. © 2015 The American Astronomical Society https://orcid.org/0000-0001-9147-1841 en_US http://dx.doi.org/10.1088/0004-637x/810/1/20 The 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 IOP Publishing |
| spellingShingle | Wiktorowicz, Grzegorz Belczynski, Krzysztof Sobolewska, Malgorzata Sadowski, Aleksander B NATURE OF THE EXTREME ULTRALUMINOUS X-RAY SOURCES |
| title | NATURE OF THE EXTREME ULTRALUMINOUS X-RAY SOURCES |
| title_full | NATURE OF THE EXTREME ULTRALUMINOUS X-RAY SOURCES |
| title_fullStr | NATURE OF THE EXTREME ULTRALUMINOUS X-RAY SOURCES |
| title_full_unstemmed | NATURE OF THE EXTREME ULTRALUMINOUS X-RAY SOURCES |
| title_short | NATURE OF THE EXTREME ULTRALUMINOUS X-RAY SOURCES |
| title_sort | nature of the extreme ultraluminous x ray sources |
| url | http://hdl.handle.net/1721.1/100049 https://orcid.org/0000-0001-9147-1841 |
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