Accretion onto the Companion of η Carinae during the Spectroscopic Event. IV. The Disappearance of Highly Ionized Lines
Accretion onto the Companion of η Carinae during the Spectroscopic Event. IV. The Disappearance of Highly Ionized Lines
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光谱事件 IV 期间在 η Carinae 伴星上的吸积。
DOI：
10.1086/514811
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发表时间：
2007
期刊：
影响因子：
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通讯作者：
N. Soker
中科院分区：
文献类型：
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作者：
N. Soker
结果表明，η船底座大质量双星系统的高电离发射线强度的快速大幅下降可以用吸积模型来解释。这些发射线是由双星周围星云中的物质发出的，这些星云受到来自热的次级恒星的辐射的电离。辐射线每5.54年经历一次长达3个月的深度衰落，假定为双星系统的轨道周期。在吸积模型中，在~70天内，质量较小的次星是从主风中吸积质量，而不是吹起它的疾风。吸积事件有两个效应，大大降低了来自次星的高能电离辐射通量：(1)吸积质量吸收了较大比例的电离通量。(2)吸积的质量在次星周围形成了一层临时的毯子，增加了它的有效半径，从而降低了它的有效温度和高能光子的流量。这一解释与发射线的褪色是一致的，同时X射线正在下降到最小值，而且在极地方向的褪色不那么明显。
We show that the rapid and large decrease in the intensity of high-ionization emission lines from the η Carinae massive binary system can be explained by the accretion model. These emission lines are emitted by material in the nebula around the binary system that is being ionized by radiation from the hot secondary star. The emission lines suffer 3 months long deep fading every 5.54 yr, assumed to be the orbital period of the binary system. In the accretion model, for ~70 days the less massive secondary star is accreting mass from the primary wind instead of blowing its fast wind. The accretion event has two effects that substantially reduce the high-energy ionizing radiation flux from the secondary star: (1) The accreted mass absorbs a larger fraction of the ionizing flux. (2) The accreted mass forms a temporary blanket around the secondary star that increases its effective radius, hence lowering its effective temperature and the flux of high-energy photons. This explanation is compatible with the fading of the emission lines at the same time the X-ray is declining to its minimum and with the fading being less pronounced in the polar directions.
XRISM 对船底座埃塔的观测
DOI：
--
发表时间：
2021
期刊：
影响因子：
--
作者：
前田良知;the XRISM PV;Eta Carinae team
通讯作者：
Eta Carinae team