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The evolution of X‐ray binaries最新文献

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The mass of the black hole in GS2023+338/V404 Cygni 天鹅座GS2023+338/V404黑洞的质量
The evolution of X‐ray binaries Pub Date : 2008-05-12 DOI: 10.1063/1.46026
J. Cesares, P. Charles
{"title":"The mass of the black hole in GS2023+338/V404 Cygni","authors":"J. Cesares, P. Charles","doi":"10.1063/1.46026","DOIUrl":"https://doi.org/10.1063/1.46026","url":null,"abstract":"New high resolution (0.8 A) Hα spectroscopy provides further constraints on the orbital parameters of the black hole candidate V404 Cyg. Our updated mass function is now 6.08±0.06 M⊙ which confirms V404 Cyg as the most important black hole candidate yet found. We also resolve the rotational broadening of the secondary star which yields the lowest mass ratio ever measured (q=Mc/Mx=0.050). The mass of the black hole is now restricted to the range 7–29 M⊙.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"7 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":"128734351","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}
引用次数: 3
Recent observations of EXO 2030+375 with BATSE 用BATSE对EXO 2030+375的最新观测
The evolution of X‐ray binaries Pub Date : 2008-05-12 DOI: 10.1063/1.46018
M. Stollberg, W. Paciesas, M. Finger, G. Fishman, R. Wilson, B. A. Harmon, C. Wilson
{"title":"Recent observations of EXO 2030+375 with BATSE","authors":"M. Stollberg, W. Paciesas, M. Finger, G. Fishman, R. Wilson, B. A. Harmon, C. Wilson","doi":"10.1063/1.46018","DOIUrl":"https://doi.org/10.1063/1.46018","url":null,"abstract":"The transient x‐ray pulsar EXO 2030+375 has been detected in the Large Area Detectors (LADs) of BATSE during twelve outbursts from February 1992 to July 1993. These data have been fit to a model of the pulsar’s rotational phase which assumes an independent torque for each outburst. An intensity history, a pulse period history, a pulsed fraction, and the latest orbit parameters resulting from this fit are presented.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"52 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":"115981280","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}
引用次数: 0
Optical behavior of the Be‐X binary V635 CAS=4U0115+63 before and during a transient phase Be‐X双星V635 CAS=4U0115+63瞬态前和瞬态期间的光学行为
The evolution of X‐ray binaries Pub Date : 2008-05-12 DOI: 10.1063/1.46023
A. Guarnieri, C. Bartolini, M. Teodorani, R. Silingardi, A. Piccioni
{"title":"Optical behavior of the Be‐X binary V635 CAS=4U0115+63 before and during a transient phase","authors":"A. Guarnieri, C. Bartolini, M. Teodorani, R. Silingardi, A. Piccioni","doi":"10.1063/1.46023","DOIUrl":"https://doi.org/10.1063/1.46023","url":null,"abstract":"The main results of the observations of the optical component of the Be‐X binary system V635 Cas, carried out at the Bologna Observatory in the period 1985–1990 are presented. Three kinds of variable features were prominent: i) photometric variations on a time‐scale of several days; ii) a strong increase in luminosity on a time‐scale of about one year; iii) an episodic inversion of the ratio of the equivalent widths of Hα and Fe ii 6153.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"90 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":"124240717","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}
引用次数: 0
Precession and long‐term cyclic behavior 岁差和长期周期行为
The evolution of X‐ray binaries Pub Date : 2008-05-12 DOI: 10.1063/1.45933
A. Smale
{"title":"Precession and long‐term cyclic behavior","authors":"A. Smale","doi":"10.1063/1.45933","DOIUrl":"https://doi.org/10.1063/1.45933","url":null,"abstract":"In this paper I review the observational evidence for long‐term superorbital periodicities and quasi‐periodic phenomena in x‐ray binaries with time scales of ∼30 days to ∼10 years, and discuss their physical interpretation. Superorbital periods may be directly measured from long‐term x‐ray monitoring, inferred by spectroscopic or ‘‘circumstantial’’ evidence, or (perhaps) deduced from changes in the binary orbital period. Possible causes of these periods are: precision processes within the binary; irradiation of the companion by the compact object and/or stellar activity in the companion star; or the presence in the system of a third body, making the source a hierarchical triple. Each of these processes has its own implications for binary evolution.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"3 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":"133275950","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}
引用次数: 0
Spin evolution of neutron stars in accretion powered pulsars 吸积动力脉冲星中子星的自旋演化
The evolution of X‐ray binaries Pub Date : 2008-05-12 DOI: 10.1063/1.45984
P. Ghosh
{"title":"Spin evolution of neutron stars in accretion powered pulsars","authors":"P. Ghosh","doi":"10.1063/1.45984","DOIUrl":"https://doi.org/10.1063/1.45984","url":null,"abstract":"This is a review of our understanding of the evolution of the spin periods of neutron stars in accretion‐powered binary x‐ray pulsars during the course of evolution of these binary systems. I discuss how neutron stars born in binaries as rotation‐powered pulsars are initially spun down by electromagnetic and plasma torques, until accretion of matter from the companion star begins. I describe how accretion torques spin up and spin down the star during the main x‐ray emission phase of neutron stars accreting from disks, winds, or equatorial rings produced by mass loss from their companions. I outline the final phase of spinup of the neutron stars into recycled rotation‐powered pulsars.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"2 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":"127053995","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}
引用次数: 1
Emission processes in x‐ray pulsars x射线脉冲星的发射过程
The evolution of X‐ray binaries Pub Date : 2008-05-12 DOI: 10.1063/1.45983
A. Harding
{"title":"Emission processes in x‐ray pulsars","authors":"A. Harding","doi":"10.1063/1.45983","DOIUrl":"https://doi.org/10.1063/1.45983","url":null,"abstract":"The processes that are important in x‐ray pulsar emission are dominated by the strong magnetic fields of the accreting neutron star. These processes include the channeling of accretion flow from the companion via either a disk or a wind onto the neutron star polar caps, the deceleration of the accreting particles and the radiation mechanisms that form the spectrum. I will review x‐ray pulsar emission models in both the high‐luminosity sources, where the accreting plasma is stopped by radiation pressure, and the low‐luminosity sources, where the accretion flow is stopped by either a collisionless shock or Coulomb collisions. The formation of cyclotron lines in pulsar spectra will also be discussed.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"34 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":"125072786","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}
引用次数: 4
The USA experiment on the Argos Satellite: A low cost instrument for timing x‐ray binaries 美国在Argos卫星上的实验:一种低成本的x射线双星计时仪器
The evolution of X‐ray binaries Pub Date : 2008-05-12 DOI: 10.1063/1.45941
K. Wood, G. Fritz, P. Hertz, W. Johnson, M. N. Lovelette, M. Wolff, E. Bloom, G. Godfrey, J. Hanson, P. Michelson, R. Taylor, H. Wen
{"title":"The USA experiment on the Argos Satellite: A low cost instrument for timing x‐ray binaries","authors":"K. Wood, G. Fritz, P. Hertz, W. Johnson, M. N. Lovelette, M. Wolff, E. Bloom, G. Godfrey, J. Hanson, P. Michelson, R. Taylor, H. Wen","doi":"10.1063/1.45941","DOIUrl":"https://doi.org/10.1063/1.45941","url":null,"abstract":"The Unconventional Stellar Aspect (USA) experiment to be launched in September 1995 on the Advanced Research and Global Observations Satellite (ARGOS) is a low‐cost, quick—yet scientifically ambitious—x‐ray timing experiment. It is designed for the dual purpose of scientific research in x‐ray timing and time resolved spectroscopy and also for exploration of applications of x‐ray sensor technology. Bright galactic x‐ray binaries are used simultaneously for both scientific and applied objectives.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"37 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":"124349216","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}
引用次数: 4
Dynamical Evidence for Black Holes in Soft X-ray Transients and Other X-ray Binaries 软x射线瞬态和其他x射线双星中黑洞的动力学证据
The evolution of X‐ray binaries Pub Date : 2008-05-12 DOI: 10.1063/1.45987
A. Cowley
{"title":"Dynamical Evidence for Black Holes in Soft X-ray Transients and Other X-ray Binaries","authors":"A. Cowley","doi":"10.1063/1.45987","DOIUrl":"https://doi.org/10.1063/1.45987","url":null,"abstract":"Although various observational properties have been suggested as indicators of a black hole in a binary system (e.g., rapid x‐ray fluctuations, ultra‐soft x‐ray spectra, etc.), the most certain way to determine the mass is to measure it dynamically, using observed radial velocities of the companion star. This paper discusses the x‐ray binaries for which such observational evidence for a stellar black hole is presently available.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"39 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":"126342971","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}
引用次数: 0
Orbital period changes in the eclipsing pulsar binary PSR B1957+20 食脉冲星双星PSR B1957+20轨道周期的变化
The evolution of X‐ray binaries Pub Date : 2008-05-12 DOI: 10.1063/1.45958
Z. Arzoumanian, A. Fruchter, Joseph H. Taylor
{"title":"Orbital period changes in the eclipsing pulsar binary PSR B1957+20","authors":"Z. Arzoumanian, A. Fruchter, Joseph H. Taylor","doi":"10.1063/1.45958","DOIUrl":"https://doi.org/10.1063/1.45958","url":null,"abstract":"PSR B1957+20 is a 1.6 ms pulsar orbited by a ∼0.025 M⊙ companion which eclipses the pulsar’s radio signal during approximately ten percent of the 9.2 hour orbit. The eclipses are thought to be caused by an ionized ‘‘cometary’’ wind trailing the companion in its orbit and constantly infused with new matter. The companion has been optically identified—its luminosity is strongly modulated with the orbital period of the system, consistent with synchronous rotation and heating by irradiation from the pulsar. We thus appear to be watching a pulsar in the process of slowly evaporating its companion, the star which presumably spun it up to millisecond periods during an earlier low‐mass x‐ray binary phase in the system’s evolution.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"88 17","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2008-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"120969636","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}
引用次数: 0
Dim x‐ray sources in globular clusters 球状星团中的暗淡x射线源
The evolution of X‐ray binaries Pub Date : 2008-05-12 DOI: 10.1063/1.45967
J. Grindlay
{"title":"Dim x‐ray sources in globular clusters","authors":"J. Grindlay","doi":"10.1063/1.45967","DOIUrl":"https://doi.org/10.1063/1.45967","url":null,"abstract":"Recent results are reviewed from sensitive x‐ray observations of globular clusters with ROSAT. It is clear that virtually all globulars contain a ‘‘core source’’ with soft x‐ray luminosity of ∼1032.5 erg/s, thus confirming the original Einstein Observatory discovery of such ‘‘dim sources’’ within globular clusters. High Resolution X‐ray images (HRI) with ROSAT show that these sources can be resolved into ≳3–5 sources with correspondingly reduced luminosities. High resolution optical images with HST in Hα vs. R are reviewed and show that emission line objects with uv excesses are found within the ≲6‘ positional uncertainties of the dim x‐ray sources in NGC 6397 and possibly also NGC 6752. The distinction between CVs and quiescent LMXBs is discussed, as well as additional constraints imposed by the dim sources in globulars. The overall results now becoming available from high resolution imaging with ROSAT (HSI) and HST argue that CVs have finally been discovered in globular clusters.","PeriodicalId":101857,"journal":{"name":"The evolution of X‐ray binaries","volume":"128 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":"128295253","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}
引用次数: 0
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