Suzaku Observation of the Intermediate Polar V1223 Sagittarii
Suzaku Observation of the Intermediate Polar V1223 Sagittarii
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DOI：
10.1093/pasj/63.sp3.s739
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发表时间：
2010-02
影响因子：
2.3
通讯作者：
T. Hayashi;M. Ishida;Y. Terada;A. Bamba;Takeshi Shionome
中科院分区：
文献类型：
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作者：
T. Hayashi;M. Ishida;Y. Terada;A. Bamba;Takeshi Shionome
本文报道了朱雀星对中间极区人马座V1223的观测结果。采用多温度等离子体发射模型，并考虑冷物质的反射，得到了冲击温度为37.9 + 5：1 - 4：6 keV。这将白色矮星（WD）的质量和半径分别限制在0.82 + 0：05 - 0：06 M和（6.9 stec0.4）-10 8 cm的范围内。从激波后等离子体观察反射器的立体角测量为Ω=2 ° = 0.91 tec0.26。首次在磁CV中探测到了铁K+荧光发射线，发现其中心能量随WD转动而调制。详细的光谱分析表明，该线包括一个稳定的6.4 keV的组件和红移的组件，后者只出现在旋转强度最小相位。前稳定分量的等效宽度（EW）为-80 eV，结合测量的Ω，表明主要反射面是WD面，激波高度不超过WD半径的7%。将这一限制与会津模型预测的高度进行比较（会津，1973年，Prog. Theor.物理、50，344），我们估计吸积发生的分数面积小于WD半径的7 - 10 - 3，这是非食IPs中最严格的限制。另一方面，红移的铁谱线分量可以解释为从激波前的吸积流中发出
We report on the Suzaku observation of the intermediate polar V1223 Sagittarii. Using a multi-temperature plasma emission model with its reflection from a cold matter, we obtained the shock temperature to be 37.9 +5:1 � 4:6 keV. This constrains the mass and the radius of the white dwarf (WD) in the ranges 0.82 +0:05 � 0:06 Mand (6.9˙0.4) � 10 8 cm, respectively, with the aid of a WD mass-radius relation. The solid angle of the reflector viewed from the post-shock plasma was measured to be Ω=2� = 0.91 ˙ 0.26. A fluorescent iron K˛ emission line was detected, whose central energy was discovered to be modulated with the WD rotation for the first time in magnetic-CVs. Detailed spectral analysis indicates that the line comprises a stable 6.4 keV component and a red-shifted component, the latter of which appears only around the rotational intensity-minimum phase. The equivalent width (EW )o f the former stable component, � 80 eV, together with the measured Ω indicates that the major reflector is the WD surface, and the shock height is not more than 7% of the WD radius. Comparing this limitation to the height predicted by the Aizu model (Aizu, 1973, Prog. Theor. Phys., 50, 344), we estimated the fractional area onto which the accretion occurs to be < 7 � 10 � 3 of the WD radius, which is the most severe constraint in non-eclipsing IPs. The red- shifted iron line component, on the other hand, can be interpreted as emanating from the pre-shock accretion flow