The high energy X-ray spectrum of 4U 1700-37 observed from OSO 8
The most intense hard X-ray source in the confused region in Scorpius has been identified as 4U 1700-37 (=HD 153919). Observations extending over three binary periods in 1978 September were carried out with the high-energy X-ray spectrometer on OSO 8. The 3.4 day modulation is seen above 20 keV with...
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| Veröffentlicht in: | Astrophys. J.; (United States) 1980-05, Vol.238, p.238 |
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| container_title | Astrophys. J.; (United States) |
| container_volume | 238 |
| creator | Dolan, J. F. Coe, M. J. Crannell, C. J. Dennis, B. R. Frost, K. J. Orwig, L. E. Maurer, G. S. |
| description | The most intense hard X-ray source in the confused region in Scorpius has been identified as 4U 1700-37 (=HD 153919). Observations extending over three binary periods in 1978 September were carried out with the high-energy X-ray spectrometer on OSO 8. The 3.4 day modulation is seen above 20 keV with the intensity during eclipse being consistent with zero flux. The photon-number spectrum from 20 to 150 keV is well represented by a single power law with a photon-number spectral index of -2.77 +- 0.35 or by a thermal bremsstrahlung spectrum with kT=27 (+15, -7) keV. The counting rate above 20 keV outside of eclipse shows no evidence for the 96.8 minute X-ray modulation previously reported at lower energies. Despite the difficulties that exist in reconciling both the lack of periodic modulation in the emitted X-radiation and the orbital dynamics of the system with our currently accepted theories of the evolution and physical properties of neutron stars, the observed properties of 4U 1700-37 are all consistent with the source being a spherically accreting neutron star rather than a black hole. |
| doi_str_mv | 10.1086/157980 |
| format | Article |
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The counting rate above 20 keV outside of eclipse shows no evidence for the 96.8 minute X-ray modulation previously reported at lower energies. Despite the difficulties that exist in reconciling both the lack of periodic modulation in the emitted X-radiation and the orbital dynamics of the system with our currently accepted theories of the evolution and physical properties of neutron stars, the observed properties of 4U 1700-37 are all consistent with the source being a spherically accreting neutron star rather than a black hole.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1086/157980</identifier><language>eng</language><publisher>United States</publisher><subject>640102 - Astrophysics & Cosmology- Stars & Quasi-Stellar, Radio & X-Ray Sources ; BINARY STARS ; CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS ; COSMIC RAY SOURCES ; COSMIC X-RAY SOURCES ; ECLIPSE ; NEUTRON STARS ; ORBITS ; SPECTRA ; STAR ACCRETION ; STAR EVOLUTION ; STARS ; STELLAR WINDS ; X-RAY SPECTRA</subject><ispartof>Astrophys. 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S.</creatorcontrib><creatorcontrib>NASA Goddard Space Flight Center, Laboratory for Astronomy and Solar Physics</creatorcontrib><title>The high energy X-ray spectrum of 4U 1700-37 observed from OSO 8</title><title>Astrophys. J.; (United States)</title><description>The most intense hard X-ray source in the confused region in Scorpius has been identified as 4U 1700-37 (=HD 153919). Observations extending over three binary periods in 1978 September were carried out with the high-energy X-ray spectrometer on OSO 8. The 3.4 day modulation is seen above 20 keV with the intensity during eclipse being consistent with zero flux. The photon-number spectrum from 20 to 150 keV is well represented by a single power law with a photon-number spectral index of -2.77 +- 0.35 or by a thermal bremsstrahlung spectrum with kT=27 (+15, -7) keV. The counting rate above 20 keV outside of eclipse shows no evidence for the 96.8 minute X-ray modulation previously reported at lower energies. Despite the difficulties that exist in reconciling both the lack of periodic modulation in the emitted X-radiation and the orbital dynamics of the system with our currently accepted theories of the evolution and physical properties of neutron stars, the observed properties of 4U 1700-37 are all consistent with the source being a spherically accreting neutron star rather than a black hole.</description><subject>640102 - Astrophysics & Cosmology- Stars & Quasi-Stellar, Radio & X-Ray Sources</subject><subject>BINARY STARS</subject><subject>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</subject><subject>COSMIC RAY SOURCES</subject><subject>COSMIC X-RAY SOURCES</subject><subject>ECLIPSE</subject><subject>NEUTRON STARS</subject><subject>ORBITS</subject><subject>SPECTRA</subject><subject>STAR ACCRETION</subject><subject>STAR EVOLUTION</subject><subject>STARS</subject><subject>STELLAR WINDS</subject><subject>X-RAY SPECTRA</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1980</creationdate><recordtype>article</recordtype><recordid>eNotkF1LwzAYhYMoWKf-huCFd9F8NumdMvyCQS_cYHclSd-sFduMpAr7927Uq8OBh8PhQeiW0QdGTfnIlK4MPUMFU8IQKZQ-RwWlVJJS6O0lusr561R5VRXoad0B7vpdh2GEtDvgLUn2gPMe_JR-BhwDlhvMNKVEaBxdhvQLLQ4pDrj-rLG5RhfBfme4-c8F2ry-rJfvZFW_fSyfV8RzxicinZRMSKeVlcILyUPpShug9LIE56QD41lrjdHOsaA8r8AyaVvPjXA6aLFAd_NuzFPfZN9P4Dsfx_F4tFGMa67oEbqfIZ9izglCs0_9YNOhYbQ5yWlmOeIPFhVTKA</recordid><startdate>19800515</startdate><enddate>19800515</enddate><creator>Dolan, J. 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R.</creatorcontrib><creatorcontrib>Frost, K. J.</creatorcontrib><creatorcontrib>Orwig, L. E.</creatorcontrib><creatorcontrib>Maurer, G. S.</creatorcontrib><creatorcontrib>NASA Goddard Space Flight Center, Laboratory for Astronomy and Solar Physics</creatorcontrib><collection>CrossRef</collection><collection>OSTI.GOV</collection><jtitle>Astrophys. J.; (United States)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Dolan, J. F.</au><au>Coe, M. J.</au><au>Crannell, C. J.</au><au>Dennis, B. R.</au><au>Frost, K. J.</au><au>Orwig, L. E.</au><au>Maurer, G. S.</au><aucorp>NASA Goddard Space Flight Center, Laboratory for Astronomy and Solar Physics</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The high energy X-ray spectrum of 4U 1700-37 observed from OSO 8</atitle><jtitle>Astrophys. 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Despite the difficulties that exist in reconciling both the lack of periodic modulation in the emitted X-radiation and the orbital dynamics of the system with our currently accepted theories of the evolution and physical properties of neutron stars, the observed properties of 4U 1700-37 are all consistent with the source being a spherically accreting neutron star rather than a black hole.</abstract><cop>United States</cop><doi>10.1086/157980</doi><oa>free_for_read</oa></addata></record> |
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| language | eng |
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| source | Alma/SFX Local Collection |
| subjects | 640102 - Astrophysics & Cosmology- Stars & Quasi-Stellar, Radio & X-Ray Sources BINARY STARS CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS COSMIC RAY SOURCES COSMIC X-RAY SOURCES ECLIPSE NEUTRON STARS ORBITS SPECTRA STAR ACCRETION STAR EVOLUTION STARS STELLAR WINDS X-RAY SPECTRA |
| title | The high energy X-ray spectrum of 4U 1700-37 observed from OSO 8 |
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