XMM-Newton observation of the eclipsing binary Algol

发布时间：2018-03-01 14:14

  本文关键词： stars abundance — star binaries eclipsing — stars flare — stars individual Algol　出处：《Research in Astronomy and Astrophysics》2011年04期 　论文类型：期刊论文

【摘要】：We present an XMM-Newton observation of the eclipsing binary Algol which contains an X-ray dark B8V primary and an X-ray bright K2IV secondary.The observation covered the optical secondary eclipse and captured an X-ray flare that was eclipsed by the B star.The XMM-Newton European Photon Imaging Camera and Reflection Grating Spectrometer spectra of Algol in its quiescent state are described by a two-temperature plasma model.The cool component has a temperature around 6.4×106 K while that of the hot component ranges from 2 to 4.0×107 K.Coronal abundances of C,N,O,Ne,Mg,Si and Fe were obtained for each component for both the quiescent and the flare phases,generally with upper limits for S and Ar,and upper limits for C,N,and O from the hot component.F-tests show that the abundances do not need to be differentbetween the cool and the hot componentand between the quiescent and the flare phase with the exception of Fe.Although the Fe abundance of the cool component remains constant at ～0.14,the hot component shows an Fe abundance of ～0.28,which increases to ～0.44 during the flare.This increase is expected from the chromospheric evaporation model.The absorbing column density NH of the quiescent emission is 2.5×1020 cm-2,while that of the flare-only emission is significantly lower and consistent with the column density of the interstellar medium.This observation substantiates earlier suggestions of the presence of X-ray absorbing material in the Algol system.
[Abstract]:We present an XMM-Newton observation of the eclipsing binary Algol which contains an X-ray dark B8V primary and an X-ray bright K2IV secondary.The observation covered covered the optical eclipse and captured an X-ray flare was eclipsed by the B star.The European Imaging Camera Camera Camera spectra spectra of its its its state state are by are are state 4# cool component has a temperature around around. 6.4 脳 106K while that of the hot component ranges from 2 to 4.0 脳 107K.Coronal abundances of NNOONNNNNONEONAE MANONEONAE component.F-tests hot do not were obtained for each component component both the quiescent and the flare flare #enasesally with upper upper upper for S and Arbor and upper limits limits limits for hot component.F-tests component.F-tests component.F-tests abundances do not need to be differentbetween the cool and and and cool and and cool and and and cool cool. Phase with the exception of the the cool component remains constant at 0.14 the hot component shows an Fe abundance of 0.28which increases to 0.44 during increase flare.This flare.This increase is from from chromospheric evaporation model.The absorbing column density model.The model.The absorbing column density NH of the emission emission is 2.5 脳 1020 cm-2while emission of emission that is significantly emission is significantly lower and consistent with with the the the of the the. Earlier suggestions of the presence of X-ray absorbing material in the Algol system.
【基金】：supported by the National Natural Science Foundation of China (Grant Nos. 10903007, 10778716and 10878012)
【分类号】：P144.9
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本文编号：1552274