论文标题
使用XMM-Newton观测
X-ray properties of dwarf nova EY Cyg and the companion star using an XMM-Newton observation
论文作者
论文摘要
我们使用45 ks \ textit {xmm-newton}的X射线分析x-ray nova ey cyg进行了静止的天文台档案数据。我们在X射线中发现轨道调制。我们使用模型使用模型来拟合EPIC PN，MOS1和MOS2数据，用于星际培养基吸收（\ textIt {tbabs}）和一个多振体等离子体发射模型，该模型具有幂律的温度分布（CEVMKL），如预期的，低含量的静脉曲张率高的静脉曲张。 The \textit{XMM-Newton} EPIC spectra of the source yields a maximum temperature $kT_{\rm max}$ $\sim$ 14.9$^{+3.3}_{-2.2}$ keV with an unabsorbed X-ray flux and luminosity of (1.8--2.0) $\times$ 10$^{-12}$ ergs $^{ - 1} $ cm $^{ - 1} $和（8.7-9.7）$ \ times $ 10 $^{31} $ ergs $^{ - 1} $，在能量范围0.1至50 kev中。在0.5 keV以下的能量下，有3--4个Sigma多余，我们使用\ textit {mekal}，powerlaw和Bbody模型对多余的建模，并偏爱模型\ textit {mekal}，这是物理的。根据先前的研究，该系统中的次要被认为是K型恒星，可能在软X射线区域辐射。具有添加剂\ textIt {mekal}型号的拟合，给出$ kt $ $ \ sim $ 0.1 kev的温度，没有吸附的X射线通量和光度为（2.7--8.8）$ \ times $ 10 $^{ - 14} $ 10 $^{ - 14} $ ERGS $ 10 $^{30} $ ergs $^{ - 1} $，适合伴侣星。根据定时和光谱分析的结果，我们强烈建议EY CYG的次要是K型恒星。
We present the X-ray analysis of dwarf nova EY Cyg using the 45 ks \textit{XMM-Newton} observatory archival data obtained in quiescence. We find orbital modulations in X-rays. We simultaneously fitted EPIC pn, MOS1 and MOS2 data using a model for interstellar medium absorption (\textit{tbabs}) and a multi-temperature plasma emission model with a power-law distribution of temperatures (CEVMKL) as expected from low accretion rate quiescent dwarf novae. The \textit{XMM-Newton} EPIC spectra of the source yields a maximum temperature $kT_{\rm max}$ $\sim$ 14.9$^{+3.3}_{-2.2}$ keV with an unabsorbed X-ray flux and luminosity of (1.8--2.0) $\times$ 10$^{-12}$ ergs$^{-1}$ cm$^{-1}$ and (8.7--9.7) $\times$ 10$^{31}$ ergs$^{-1}$, respectively, in the energy range 0.1 to 50 keV. There is 3--4 sigma excess at energies below 0.5 keV, we model the excess using \textit{MEKAL}, POWERLAW and BBODY models and favor the model \textit{MEKAL} which is physical. According to previous studies, the secondary in this system is thought to be a K-type star which may radiate in the soft X-ray region. The fit with an additive \textit{MEKAL} model gives a temperature of $kT$ $\sim$ 0.1 keV with an unabsorbed X-ray flux and luminosity of (2.7--8.8) $\times$ 10$^{-14}$ ergs$^{-1}$ cm$^{-1}$ and (1.3--4.2) $\times$ 10$^{30}$ ergs$^{-1}$, respectively, for the companion star. Based on the results from the timing and spectral analysis, we highly suggest that the secondary of EY Cyg is a K-type star.
