{"title":"Emission processes in x‐ray pulsars","authors":"A. Harding","doi":"10.1063/1.45983","DOIUrl":null,"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":0.0000,"publicationDate":"2008-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"4","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"The evolution of X‐ray binaries","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1063/1.45983","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 4
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.
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