The evolution of x‐ray emission of SS433 over its precessional period gave an evidence to the existence of an alternative harder x‐ray emission region apart from the jets. The spectral fits with a two continuum component model involving such a hard x‐ray component gave further support to this scenario.
{"title":"The precessional phase dependent x‐ray emission of SS433","authors":"W. Yuan, N. Kawai, M. Matsuoka","doi":"10.1063/1.46037","DOIUrl":"https://doi.org/10.1063/1.46037","url":null,"abstract":"The evolution of x‐ray emission of SS433 over its precessional period gave an evidence to the existence of an alternative harder x‐ray emission region apart from the jets. The spectral fits with a two continuum component model involving such a hard x‐ray component gave further support to this scenario.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"82 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2008-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134055570","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Several evolutionary scenarios have been proposed for the origin of low‐mass x‐ray binaries, including accretion‐induced collapse, common envelope evolution of a massive binary with an extreme mass ratio, black hole formation in Wolf‐Rayet binaries with extreme mass ratios, triple star evolution, and (in globular clusters) tidal capture. In this brief review, we examine some of the factors which determine whether a primordial binary may survive to become a neutron star‐ or black hole‐binary with a low‐mass nondegenerate component, and what structural criteria it must satisfy, having reached that state, in order to appear as an x‐ray binary. These constraints include: survival of common envelope evolution, survival of the supernova or core‐collapse event, duration of the non‐interactive phase following formation of the compact component and evolutionary state of the donor star, and finally the critical mass ratios which dictate the time scale for mass transfer in the x‐ray state. A population synthesis mod...
{"title":"On the origin of low‐mass x‐ray binaries","authors":"R. Webbink, V. Kalogera","doi":"10.1063/1.45966","DOIUrl":"https://doi.org/10.1063/1.45966","url":null,"abstract":"Several evolutionary scenarios have been proposed for the origin of low‐mass x‐ray binaries, including accretion‐induced collapse, common envelope evolution of a massive binary with an extreme mass ratio, black hole formation in Wolf‐Rayet binaries with extreme mass ratios, triple star evolution, and (in globular clusters) tidal capture. In this brief review, we examine some of the factors which determine whether a primordial binary may survive to become a neutron star‐ or black hole‐binary with a low‐mass nondegenerate component, and what structural criteria it must satisfy, having reached that state, in order to appear as an x‐ray binary. These constraints include: survival of common envelope evolution, survival of the supernova or core‐collapse event, duration of the non‐interactive phase following formation of the compact component and evolutionary state of the donor star, and finally the critical mass ratios which dictate the time scale for mass transfer in the x‐ray state. A population synthesis mod...","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"18 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2008-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121384098","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Single neutron stars were thought of more than 30 years before they were observed (and even then were not instantly recognized). Binary neutron stars, on the other hand, were observed before they had been thought of as a separate, interesting class, and were also not immediately recognized for what they were. The traditional apportionments of credit for the various ideas are not fully supported by contemporaneous publications.
{"title":"Creator’s records: The pre‐history of single and binary neutron stars","authors":"V. Trimble","doi":"10.1063/1.45954","DOIUrl":"https://doi.org/10.1063/1.45954","url":null,"abstract":"Single neutron stars were thought of more than 30 years before they were observed (and even then were not instantly recognized). Binary neutron stars, on the other hand, were observed before they had been thought of as a separate, interesting class, and were also not immediately recognized for what they were. The traditional apportionments of credit for the various ideas are not fully supported by contemporaneous publications.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"96 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2008-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"115941167","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
We consider collisions between dynamically‐evolved primordial binaries consisting of main‐sequence stars, white dwarfs, and neutron stars in globular clusters. In our four‐body binary‐binary scattering experiments, we allow stars to ‘‘stick’’ if they pass close enough to each other, which leads to the formation of a wide variety of exotic objects. Most of these objects have binary companions. Also, relatively clean exchange interactions can produce binaries containing neutron stars that eventually receive material from their companions. Such systems will be observable as x‐ray binaries.
{"title":"Binary-binary collisions involving main-sequence stars, white dwarfs and neutron stars in globular clusters","authors":"P. Leonard, M. Davies","doi":"10.1063/1.45965","DOIUrl":"https://doi.org/10.1063/1.45965","url":null,"abstract":"We consider collisions between dynamically‐evolved primordial binaries consisting of main‐sequence stars, white dwarfs, and neutron stars in globular clusters. In our four‐body binary‐binary scattering experiments, we allow stars to ‘‘stick’’ if they pass close enough to each other, which leads to the formation of a wide variety of exotic objects. Most of these objects have binary companions. Also, relatively clean exchange interactions can produce binaries containing neutron stars that eventually receive material from their companions. Such systems will be observable as x‐ray binaries.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"88 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2008-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"126199790","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
M. Finger, L. Cominsky, R. Wilson, B. A. Harmon, G. Fishman
Three outbursts of the x‐ray binary system A 0535+262 have been detected in the 20–120 keV energy range by the BATSE instrument onboard the Compton Gamma Ray Observatory. The system orbital parameters have been determined by a pulse timing analysis during data from these outbursts.
{"title":"Hard x‐ray observations of A 0535+262","authors":"M. Finger, L. Cominsky, R. Wilson, B. A. Harmon, G. Fishman","doi":"10.1063/1.46032","DOIUrl":"https://doi.org/10.1063/1.46032","url":null,"abstract":"Three outbursts of the x‐ray binary system A 0535+262 have been detected in the 20–120 keV energy range by the BATSE instrument onboard the Compton Gamma Ray Observatory. The system orbital parameters have been determined by a pulse timing analysis during data from these outbursts.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"11 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2008-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"126399917","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
V. Kaspi, S. Johnston, R. Manchester, M. Bailes, J. Bell, M. Bessell, A. Lyne, N. D'Amico
We report the discovery of regular Doppler shifts of the pulse period of PSR J0045−7319, the only known pulsar in the Small Magellanic Cloud. The pulsar is in a highly concentric 51‐day orbit with a companion star of mass greater than 4M⊙. Optical observations in the direction of the pulsar reveal a 16th magnitude B star companion. The PSR J0045−7319 system is likely an x‐ray binary progenitor.
{"title":"A radio pulsar‐B star binary in the small magellanic cloud","authors":"V. Kaspi, S. Johnston, R. Manchester, M. Bailes, J. Bell, M. Bessell, A. Lyne, N. D'Amico","doi":"10.1063/1.45960","DOIUrl":"https://doi.org/10.1063/1.45960","url":null,"abstract":"We report the discovery of regular Doppler shifts of the pulse period of PSR J0045−7319, the only known pulsar in the Small Magellanic Cloud. The pulsar is in a highly concentric 51‐day orbit with a companion star of mass greater than 4M⊙. Optical observations in the direction of the pulsar reveal a 16th magnitude B star companion. The PSR J0045−7319 system is likely an x‐ray binary progenitor.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"82 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2008-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132999481","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
R. Wilson, B. A. Harmon, G. Fishman, M. Finger, M. Stollberg, G. Pendleton, Michael H. Briggs, B. Rubin, N. Zhang
BATSE detection of a new hard x‐ray pulsar is reported. The source was first observed on 14 Jul 1993, reached a maximum intensity on 25 Jul 1993, then declined smoothly until it became undetectable on 16 Aug 1993. The BATSE location was adequate to permit OSSE, ASCA, and ROSAT observations, leading to an improved source location. The observed period at the solar system barycenter was 93.548±0.002s, 93.5665±0.0005s, and 93.541±0.004 on 15 Jul 1993, 23 Jul 1993, and 10 Aug 1993, respectively. The source is detected between ∼20 keV and 160 keV, with a spectrum fit by an optically thin thermal bremsstrahlung form, having a kT of 25.4±2.1 keV during the rise to maximum intensity, decreasing monotonically during the remainder of the outburst to 17.1±2.5 keV on 5 Aug 1993. The pulse profile in this energy range has a single broad peak, with the maximum occurring later at higher energies. The pulse profile, intensity history, and spectral behavior observed by BATSE are reported.
{"title":"Discovery of the hard x‐ray pulsar GRO J1008‐57 by BATSE","authors":"R. Wilson, B. A. Harmon, G. Fishman, M. Finger, M. Stollberg, G. Pendleton, Michael H. Briggs, B. Rubin, N. Zhang","doi":"10.1063/1.45985","DOIUrl":"https://doi.org/10.1063/1.45985","url":null,"abstract":"BATSE detection of a new hard x‐ray pulsar is reported. The source was first observed on 14 Jul 1993, reached a maximum intensity on 25 Jul 1993, then declined smoothly until it became undetectable on 16 Aug 1993. The BATSE location was adequate to permit OSSE, ASCA, and ROSAT observations, leading to an improved source location. The observed period at the solar system barycenter was 93.548±0.002s, 93.5665±0.0005s, and 93.541±0.004 on 15 Jul 1993, 23 Jul 1993, and 10 Aug 1993, respectively. The source is detected between ∼20 keV and 160 keV, with a spectrum fit by an optically thin thermal bremsstrahlung form, having a kT of 25.4±2.1 keV during the rise to maximum intensity, decreasing monotonically during the remainder of the outburst to 17.1±2.5 keV on 5 Aug 1993. The pulse profile in this energy range has a single broad peak, with the maximum occurring later at higher energies. The pulse profile, intensity history, and spectral behavior observed by BATSE are reported.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"308 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2008-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"130404155","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
This article reports on the analysis of the first M31 survey with the ROSAT PSPC performed in July 1991. The spectral characteristics of the 396 individual x‐ray sources detected will be discussed as well as their positional correlation with the 108 individual x‐ray sources detected by the Einstein observatory. The optical identifications of the ROSAT x‐ray sources are the result of a MIT‐MPE‐UvA collaboration. A detailed analysis of the integral flux distribution shows that just two thirds of the detected x‐ray sources in the field of M31 must be background objects. The discovery of a significant absorption of background radiation is discussed, as well as an upper limit for the luminosity of a diffuse emission component. Finally a comparison of the luminosity function of 29 globular clusters sources with the one in our own galaxy reveals a good agreement.
{"title":"ROSAT PSPC observation of M31","authors":"R. Supper","doi":"10.1063/1.45950","DOIUrl":"https://doi.org/10.1063/1.45950","url":null,"abstract":"This article reports on the analysis of the first M31 survey with the ROSAT PSPC performed in July 1991. The spectral characteristics of the 396 individual x‐ray sources detected will be discussed as well as their positional correlation with the 108 individual x‐ray sources detected by the Einstein observatory. The optical identifications of the ROSAT x‐ray sources are the result of a MIT‐MPE‐UvA collaboration. A detailed analysis of the integral flux distribution shows that just two thirds of the detected x‐ray sources in the field of M31 must be background objects. The discovery of a significant absorption of background radiation is discussed, as well as an upper limit for the luminosity of a diffuse emission component. Finally a comparison of the luminosity function of 29 globular clusters sources with the one in our own galaxy reveals a good agreement.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"1 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2008-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"130969840","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
J. Ballet, P. Laurent, F. Lebrun, J. Paul, J. Roques, P. Mandrou, I. Malet, M. Schmitz-Fraysse, E. Churazov, M. Gilfanov, R. Sunyaev, A. Vikhlinin, A. Finoguenov, A. Dyachkov, N. Khavenson, A. Sheikhet
X‐ray binaries form the bulk of hard x‐ray sources, in the 30–300 keV range. More than twenty of them have been detected by SIGMA. Suspected black hole systems seem to be particularly numerous among the sources emitting above 100 keV, and their spectra appear harder than those of neutron star systems. This amounts to a spectral distinction between the two classes of x‐ray binaries. The nature of the companion (high mass or low mass) does not affect this conclusion.
{"title":"Black holes vs neutron stars among SIGMA sources","authors":"J. Ballet, P. Laurent, F. Lebrun, J. Paul, J. Roques, P. Mandrou, I. Malet, M. Schmitz-Fraysse, E. Churazov, M. Gilfanov, R. Sunyaev, A. Vikhlinin, A. Finoguenov, A. Dyachkov, N. Khavenson, A. Sheikhet","doi":"10.1063/1.45998","DOIUrl":"https://doi.org/10.1063/1.45998","url":null,"abstract":"X‐ray binaries form the bulk of hard x‐ray sources, in the 30–300 keV range. More than twenty of them have been detected by SIGMA. Suspected black hole systems seem to be particularly numerous among the sources emitting above 100 keV, and their spectra appear harder than those of neutron star systems. This amounts to a spectral distinction between the two classes of x‐ray binaries. The nature of the companion (high mass or low mass) does not affect this conclusion.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"40 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2008-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"123859023","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"HST/FOS observations of hot gas during the total eclipse of the neutron star in HZ Her/Her X‐1","authors":"S. Wachter, S. Anderson, B. Margon, R. Downes","doi":"10.1063/1.45924","DOIUrl":"https://doi.org/10.1063/1.45924","url":null,"abstract":"","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"4 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2008-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"122256528","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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