论文标题
异步极性V1432 AQL的积聚几何形状
The Accretion Geometry of the Asynchronous Polar V1432 Aql
论文作者
论文摘要
V1432 AQL是唯一黯然失色的异步极性（AP），它提供了一个出色的实验室，可以研究增生物质与磁场之间的相互作用。但是，由于其复杂的排放，对其积聚几何形状的物理理解仍然很出色。在这里，我们报告了一项X射线光谱研究，使用\ nustar \ and \ swift的同时观察结果。我们检测到大量的康普顿反思，并确认了早期的X射线温度$ \ sim52 $ kev的早期报告。我们建议多温度发射是由于特定积聚率在吸积区域的分布所致，这导致在加热区域上的温度分布，并解释了软X射线的高温。我们将这些特征解释为AP中无效积聚的结果。因此，吸积流可以深入到磁层中，并在其赤道附近的较窄的吸积区域上喂白矮人（WD）。此外，宽带X射线还提供了积聚的详细信息； $ \ sim 1 \ sim 10^{ - 10} 〜m _ {\ odot} 〜yr^{ - 1} $的低总收集率与v1432 aql是最近的NOVA相矛盾，而高度高的增强率是$ \ sim 5.6〜 g〜cm^cm^cm^complient complencation V1432 AQL矛盾的猜测。 WD。
As the only eclipsing asynchronous polar (AP), V1432 Aql provides an excellent laboratory to study the interaction between the accreted matter and the magnetic field. However, due to its complex emission, a more physical understanding of its accretion geometry is still outstanding. Here, we report an X-ray spectral study using contemporaneous observations from \nustar\ and \swift. We detect significant Compton reflection and confirm earlier reports of a high soft X-ray temperature $\sim52$ keV. We suggest that the multi-temperature emission is due to a distribution of the specific accretion rate over the accretion region, which leads to a continuous temperature distribution over the heated area and explains the high temperature of the soft X-rays. We interpret these characteristics as the results of the inefficient accretion in APs. Thus the accretion stream can punch deeply into the magnetosphere and feed the white dwarf (WD) over a much narrower accretion region near its equator. Additionally, the broad-band X-rays provide details of the accretion; the low total accretion rate of $\sim 1 \times 10^{-10} ~M_{\odot} ~yr^{-1}$ contradicts the speculation that V1432 Aql was a recent nova, while the high specific accretion rate of $\sim 5.6 ~g ~cm^{-2} ~s^{-1}$ explains the significant reflection from the surface of the WD.
