S. Matz, D. Grabelsky, W. Purcell, M. Ulmer, W. Johnson, R. Kinzer, J. Kurfess, M. Strickman
{"title":"天鹅座x - 3的硬x射线变异性","authors":"S. Matz, D. Grabelsky, W. Purcell, M. Ulmer, W. Johnson, R. Kinzer, J. Kurfess, M. Strickman","doi":"10.1063/1.46020","DOIUrl":null,"url":null,"abstract":"The OSSE instrument on the Compton Gamma‐Ray Observatory (GRO) made 4 observations of Cygnus X–3 between May 1991 and December 1992. OSSE observed a substantial change in the average hard x‐ray flux, which has previously been observed to be stable (variations <20%). Over a 2–3 day period the flux above ∼50 keV decreased by roughly a factor of 3. This occurred about 15 days prior to a large radio flare from this source. OSSE detected by 4.8 hr period and observed significant orbital modulation of the hard x‐ray (≳50 keV) flux, in conflict with some extrapolations from lower energies. The spectrum in the high state is consistent with a power law, ∝E−3.0.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"13 1","pages":"0"},"PeriodicalIF":0.0000,"publicationDate":"2008-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"Hard x‐ray variability of Cygnus X–3\",\"authors\":\"S. Matz, D. Grabelsky, W. Purcell, M. Ulmer, W. Johnson, R. Kinzer, J. Kurfess, M. Strickman\",\"doi\":\"10.1063/1.46020\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"The OSSE instrument on the Compton Gamma‐Ray Observatory (GRO) made 4 observations of Cygnus X–3 between May 1991 and December 1992. OSSE observed a substantial change in the average hard x‐ray flux, which has previously been observed to be stable (variations <20%). Over a 2–3 day period the flux above ∼50 keV decreased by roughly a factor of 3. This occurred about 15 days prior to a large radio flare from this source. OSSE detected by 4.8 hr period and observed significant orbital modulation of the hard x‐ray (≳50 keV) flux, in conflict with some extrapolations from lower energies. The spectrum in the high state is consistent with a power law, ∝E−3.0.\",\"PeriodicalId\":101857,\"journal\":{\"name\":\"The evolution of X‐ray binaries\",\"volume\":\"13 1\",\"pages\":\"0\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2008-05-12\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"The evolution of X‐ray binaries\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.1063/1.46020\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"The evolution of X‐ray binaries","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1063/1.46020","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
The OSSE instrument on the Compton Gamma‐Ray Observatory (GRO) made 4 observations of Cygnus X–3 between May 1991 and December 1992. OSSE observed a substantial change in the average hard x‐ray flux, which has previously been observed to be stable (variations <20%). Over a 2–3 day period the flux above ∼50 keV decreased by roughly a factor of 3. This occurred about 15 days prior to a large radio flare from this source. OSSE detected by 4.8 hr period and observed significant orbital modulation of the hard x‐ray (≳50 keV) flux, in conflict with some extrapolations from lower energies. The spectrum in the high state is consistent with a power law, ∝E−3.0.
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