Suzaku Observations of SS Cygni in Quiescence and Outburst

Publications of the Astronomical Society of Japan

Okada, Shunsaku¹  Mukai, Koji⁶  Nakamura, Ryoko⁴  Hayashi, Takayuki²  Terada, Yukikatsu³  Hamaguchi, Kenji⁷  Ishida, Manabu⁵ 

[1] Institute of Space and Astronautical Science/JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510 Space System Division, NEC Corporation, 1-10 Nisshin-cho, Fuchu, Tokyo 183-8501;Institute of Space and Astronautical Science/JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510 Department of Physics, Tokyo Metropolitan University, 1-1 Minami-Osawa, Hachioji, Tokyo 192-0397;Department of Physics, Saitama University, 255 Shimo-okubo, Sakura-ku, Saitama 338-8570;Institute of Space and Astronautical Science/JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510 Department of Physics, Tokyo Institute of Technology, 2-12-1 Ookayama, Megro-ku, Tokyo 152-8551;Institute of Space and Astronautical Science/JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510;CRESST and X-ray Astrophysics Laboratory, NASA/GSFC, Greenbelt, MD 20771, USA;CRESST and X-ray Astrophysics Laboratory, NASA/GSFC, Greenbelt, MD 20771, USADepartment of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA

关键词: "accretion;    accretion disks";    plasmas;    "stars: dwarf novae";    "X-rays: individual (SS Cygni)";   

DOI  :  10.1093/pasj/61.sp1.S77

学科分类：天文学(综合)

来源: Oxford University Press

【 摘 要 】

WepresentresultsfromtheSuzakuobservationsofthedwarfnovaSSCyginquiescenceandoutburstin2005November.ThehighsensitivityoftheHXDPINandthehighspectralresolutionoftheXISenabledustodeterminetheplasmaparameterswithunprecedentedprecision.Themaximumtemperatureoftheplasmainquiescence,20.4$$^{+4.0}_{-2.6}$$(stat)$$pm$$3.0(sys)keV,issignificantlyhigherthanthatinoutburst,6.0$$^{+0.2}_{-1.3}$$keV.Theelementalabundancesareclosetothesolaronesformedium-$$Z$$elements(Si,S,Ar),whereastheydeclinebothinlighterandheavierelements,exceptforthatofcarbon,whichis2solar,atleast.Thesolidangleofthereflectorsubtendingoveranopticallythinthermalplasmais$$Omega^{mQ}/(2pi)$$$$=$$1.7$$pm$$0.2(stat)$$pm$$0.1(sys)inquiescence.A6.4keVironK$$alpha$$lineisresolvedintonarrowandbroadcomponents.Thesefactsindicatethatboththewhitedwarfandtheaccretiondiskcontributetothereflection.Weconsiderthestandardopticallythinboundarylayerasbeingthemostplausiblepicturefortheplasmaconfigurationinquiescence.Thesolidangleofthereflectorinoutburst,$$Omega^{mO}!!/(2pi)$$$$=$$0.9$$^{+0.5}_{-0.4}$$,andabroad6.4keVironlineindicatethatthereflectioninoutburstoriginatesfromtheaccretiondiskandanequatorialaccretionbelt.Thebroad6.4keVlinesuggeststhattheopticallythinthermalplasmaisdistributedontheaccretiondisklikesolarcorona.

【 授权许可】

Unknown