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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Suzaku observation of the intermediate polar V1223 Sagittarii
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Suzaku observation of the intermediate polar V1223 Sagittarii

机译：朱雀的中间极地人马座V1223观测

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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 _(-4.6)~(+5.1) keV. This constrains the mass and the radius of the white dwarf (WD) in the ranges 0.82 _(-0.06)~(+0.05)M and (6.9±0.4) × 10 ~8cm, 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=2π = 0.91±0.26. A fluorescent iron Kα 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) of 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 redshifted iron line component, on the other hand, can be interpreted as emanating from the pre-shock accretion flow via fluorescence. Its EW (28 _(-13)~(+44) eV) and the central energy (6.30 _(-0.05)~(+0.07) keV) at the intensity-minimum phase are consistent with this interpretation.
机译：我们报告了中间极地V1223射手座的朱雀观测。使用多温度等离子体发射模型，该模型具有从冷物质反射的信号，得出的激波温度为37.9 _（-4.6）〜（+5.1）keV。借助于WD质量，这将白矮星（WD）的质量和半径分别限制在0.82 _（-0.06）〜（+0.05）M和（6.9±0.4）×10〜8cm的范围内。半径关系。从震后等离子体观察的反射器的立体角经测量为Ω＝2π＝ 0.91±0.26。检测到一条荧光铁Kα发射线，发现它的中心能量首次在电磁CV中随WD旋转而被调制。详细的光谱分析表明，该谱线包含一个稳定的6.4 keV分量和一个红移分量，后者仅在旋转强度-最小相位附近出现。前一个稳定分量的等效宽度（EW）〜80 eV，加上测得的Ω表示主要反射器是WD表面，并且冲击高度不超过WD半径的7％。将此限制条件与Aizu模型预测的高度进行比较（Aizu，1973，Prog。Theor。Phys。，50，344），我们估计吸积发生的分数面积为<7×10〜（-3）。 WD半径，这是非超越IP中最严格的约束。另一方面，红移的铁谱线分量可以解释为是由震荡前的吸积流通过荧光发出的。其在强度-最小相位下的EW（28 _（-13）〜（+44）eV）和中心能量（6.30 _（-0.05）〜（+0.07）keV）与该解释一致。

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