AG Draconis observed with XMM-Newton
AG Draconis observed with XMM-Newton
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AG Draconis 用 XMM-Newton 观察
DOI：
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发表时间：
2008
期刊：
影响因子：
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通讯作者：
A. Skopal
中科院分区：
文献类型：
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作者：
R. González;R. Viotti;T. Iijima;C. Rossi;F. Montagni;S. Bernabei;A. Frasca;A. Skopal
语境。 AG Draconis是X射线中最亮的共生星，也是超软X射线源类的原型之一。目标。研究这种奇特双星系统的 X 射线光谱（涵盖静止期和活动期）对于研究高温光谱成分的物理性质并揭示爆发的起源是必要的。方法。 2003-2005 年期间使用 XMM-Newton 进行的 X 射线和紫外线观测以及协调的光学分光光度监测以及档案数据被用来推导 AG Dra 系统高能源在不同轨道和活动阶段的行为。结果。在静止期间，X 射线发射非常柔和，强度接近之前的 ROSAT 观测结果，具有
Context. AG Draconis is the brightest symbiotic star in X-rays and one of the prototypes of the supersoft X-ray source class. Aims. Study of the X-ray spectrum of this peculiar binary system, covering both quiescence and activity periods, is necessary to investigate the physics of the high temperature spectral component, and to unveil the origin of the outbursts. Methods. X-ray and UV observations with XMM-Newton during 2003–2005 and coordinated optical spectrophotometric monitoring, together with archive data, are employed to derive the behaviour of the high energy source of the AG Dra system during different orbital and activity phases. Results. During quiescence the X-ray emission is very soft and is close in strength to the previous ROSAT observations, with an