新的硬X射线激变变星的表征
Characterization of new hard X-ray Cataclysmic Variables
摘要：
我们的目标是表征9个新的硬X射线选定的激变变星（CV）的样本，明确地将它们识别为中间极性（IP）类型的磁性系统。我们使用X射线进行了定时和光谱分析，同时使用XMM-牛顿收集的紫外和光学数据，并辅以INTEGRAL和Swift提供的硬X射线数据。脉冲到达时间被用来估计轨道周期。X射线光谱用不同吸收柱和发射组分组成的复合模型拟合。在白矮星（WD）自旋周期检测到强X射线脉冲，并发现随着能量的减少。在X射线中，大多数源是自旋主导的系统，尽管有四个源在光波长处是拍频主导的。我们估计了所有系统（除了IGR J16500-3307）的轨道周期，为IGR J 08390 -4833，IGR J18308-1232和IGR J18173-2509提供了第一个估计。所有的X射线谱都是多温谱。V2069 Cyg和RX J 0636 +3535是kT 80 eV的软X射线光学厚组件。在所有源中都检测到6.4keV的强K_α Fe线。在IGR J 08390 -4833中检测到OVII在0.76 keV处的吸收边。WD的质量和下限的吸积率估计。我们发现所有来源都是IP。IGR J 08390 -4833、V2069 Cyg和IGR J16500-3307是纯粹的盘状吸积体，而IGR J18308-1232、IGR J1509-6649、IGR J17195-4100和RX J 0636 +3535则显示出盘状溢出吸积模式。所有的辐射源都显示出激波后区域的温度梯度和激波前气流中物质的高吸收辐射，这也是造成X射线脉动的原因。WD表面的反射可能是荧光铁线的起源。越来越多的证据表明，在IP中存在热吸收剂。将2个系统添加到软X射线IP亚组中证实了\sim的发生率30%。
英文摘要：
We aim at characterizing a sample of 9 new hard X-ray selected Cataclysmic Variable (CVs), to unambiguously identify them as magnetic systems of the Intermediate Polar (IP) type. We performed timing and spectral analysis by using X-ray, and simultaneous UV and optical data collected by XMM-Newton, complemented with hard X-ray data provided by INTEGRAL and Swift. The pulse arrival time were used to estimate the orbital periods. The X-ray spectra were fitted using composite models consisting of different absorbing columns and emission components. Strong X-ray pulses at the White Dwarf (WD) spin period are detected and found to decrease with energy. Most sources are spin-dominated systems in the X-rays, though four are beat dominated at optical wavelengths. We estimated the orbital period in all system (except for IGR J16500-3307), providing the first estimate for IGR J08390-4833, IGR J18308-1232, and IGR J18173-2509. All X-ray spectra are multi-temperature. V2069 Cyg and RX J0636+3535 posses a soft X-ray optically thick component at kT 80 eV. An intense K_alpha Fe line at 6.4 keV is detected in all sources. An absorption edge at 0.76 keV from OVII is detected in IGR J08390-4833. The WD masses and lower limits to the accretion rates are estimated. We found all sources to be IPs. IGR J08390-4833, V2069 Cyg, and IGR J16500-3307 are pure disc accretors, while IGR J18308-1232, IGR J1509-6649, IGR J17195-4100, and RX J0636+3535 display a disc-overflow accretion mode. All sources show a temperature gradient in the post-shock regions and a highly absorbed emission from material located in the pre-shock flow which is also responsible for the X-ray pulsations. Reflection at the WD surface is likely the origin of the fluorescent iron line. There is an increasing evidence for the presence of a warm absorber in IPs. The addition of 2 systems to the subgroup of soft X-ray IPs confirms a \sim 30% incidence.
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