Accretion Column Structure of Magnetic Cataclysmic Variables from X-Ray Spectroscopy
Accretion Column Structure of Magnetic Cataclysmic Variables from X-Ray Spectroscopy
复制标题
X 射线光谱中磁激变变量的吸积柱结构
DOI：
--
复制
发表时间：
2006
期刊：
影响因子：
--
通讯作者：
C. Mauche
中科院分区：
文献类型：
--
作者：
R. Hoogerwerf;N. Brickhouse;C. Mauche
利用Chandra HETG数据，我们得到了中间极型巨变星EX hydre的Mg XI和Mg XII的光谱线的光曲线。在白矮星自旋周期上折叠的mgxi光曲线显示出在mgxii或宽带光曲线中看不到的两个尖峰。当吸积柱被白矮星体掩星时，在自转轴与吸积柱的夹角为α = 18°、Mg - XI辐射距离白矮星表面的高度为> 0.0004白矮星半径，即> 4 km时，会产生这样的尖峰。mgxii和宽频光曲线中没有尖峰可以解释，如果它的大部分发射形成在更大的高度，超过0.004白矮星半径或超过40公里，在白矮星表面以上，尽管这与标准Aizu吸积柱模型的预测不一致。
Using Chandra HETG data, we present light curves for individual spectral lines of Mg XI and Mg XII for EX Hydrae, an intermediate polar-type cataclysmic variable. The Mg XI light curve, folded on the white dwarf spin period, shows two spikes that are not seen in the Mg XII or broadband light curves. Occultation of the accretion column by the body of the white dwarf would produce such spikes for an angle between the rotation axis and the accretion columns of α = 18° and a height of the Mg XI emission above the white dwarf surface of ≲0.0004 white dwarf radii, or ≲4 km. The absence of spikes in the Mg XII and broadband light curves could then be explained if the bulk of its emission forms at much larger height, more than 0.004 white dwarf radii or over 40 km, above the white dwarf surface, although this is not consistent with the predictions of the standard Aizu model of the accretion column.