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High resolution X-ray spectroscopy of Supergiant HMXB 4U1700−37 during the compact object eclipse.
Monthly Notices of the Royal Astronomical Society ( IF 4.7 ) Pub Date : 2020-12-26 , DOI: 10.1093/mnras/staa3956
M Martínez-Chicharro 1 , V Grinberg 2 , J M Torrejón 1 , N Schulz 3 , L Oskinova 4 , M Nowak 5 , F Fürst 6 , N Hell 7 , R Hainich 4
Affiliation  

We present an analysis of the first observation of the iconic High Mass X-ray Binary 4U 1700−37 with the Chandra High Energy Transmission Gratings during an X-ray eclipse. The goal of the observation was to study the structure/physical conditions in the clumpy stellar wind through high resolution spectroscopy. We find that: a) emission line brightness from K shell transitions, corresponding to near neutral species, directly correlates with continuum illumination. However, these lines do not greatly diminish during eclipse. This is readily explained if fluorescence Kα emission comes from the bulk of the wind. b) The highly ionised Fexxv and Fexxvi Lyα diminish during eclipse. Thus, they must be produced in the vicinity of the compact object where log ξ > 3. c) to describe the emission line spectrum, the sum of two self consistent photo ionisation models with low ionisation (log ξ ∼ −1) and high ionisation (log ξ ∼ 2.4) is required. From their emission measures, the clump-to-interclump density ratio can be estimated to be nc/ni ∼ 300. To fit the complex He-like Sixiii profile, the plasma requires a broadening with vbulk ∼ 840 km s−1. Reproducing the observed r ≈ f line fluxes requires the addition of a third collisionally ionised plasma. d) Emission lines widths appear unresolved at the hetg gratings resolution with exception of Silicon. There is no clear radial segregation between (quasi)neutral and ionised species, consistent with cold wind clumps interspersed in a hot rarefied interclump medium.

中文翻译:

超巨星 HMXB 4U1700−37 在致密天体日食期间的高分辨率 X 射线光谱。

我们对 X 射线日食期间使用 Chandra 高能透射光栅对标志性的高质量 X 射线双星 4U 1700−37 的首次观察进行了分析。观测的目的是通过高分辨率光谱研究团块恒星风的结构/物理条件。我们发现:a)来自 K 壳跃迁的发射线亮度,对应于近中性物种,与连续光照直接相关。然而,这些线在日食期间不会大大减少。如果荧光 Kα 发射来自大部分风,这很容易解释。b) 高度电离的 Fexxv 和 Fexxvi Lyα 在日食期间减少。因此,它们必须在 log ξ > 3 的致密物体附近产生。 c) 来描述发射线谱,需要具有低电离 (log ξ ∼ -1) 和高电离 (log ξ ∼ 2.4) 的两个自洽光电离模型的总和。根据他们的排放量度,团块间密度比可以估计为 nc/ni ∼ 300。为了拟合复杂的类 He 型 Sixiii 剖面,等离子体需要以 vbulk 约 840 km s−1 加宽。再现观察到的 r ≈ f 线通量需要添加第三个碰撞电离等离子体。d) 除硅外,发射线宽度在 hetg 光栅分辨率下似乎未解决。(准)中性和电离物种之间没有明显的径向分离,这与散布在热稀薄的团间介质中的冷风团一致。簇间密度比可以估计为 nc/ni ∼ 300。为了拟合复杂的类 He 型 Sixiii 剖面,等离子体需要加宽 vbulk ∼ 840 km s-1。再现观察到的 r ≈ f 线通量需要添加第三个碰撞电离等离子体。d) 除硅外,发射线宽度在 hetg 光栅分辨率下似乎未解决。(准)中性和电离物种之间没有明显的径向分离,这与散布在热稀薄的团间介质中的冷风团一致。簇间密度比可以估计为 nc/ni ∼ 300。为了拟合复杂的类 He 型 Sixiii 剖面,等离子体需要加宽 vbulk ∼ 840 km s-1。再现观察到的 r ≈ f 线通量需要添加第三个碰撞电离等离子体。d) 除硅外,发射线宽度在 hetg 光栅分辨率下似乎未解决。(准)中性和电离物种之间没有明显的径向分离,这与散布在热稀薄的团间介质中的冷风团一致。d) 除硅外,发射线宽度在 hetg 光栅分辨率下似乎未解决。(准)中性和电离物种之间没有明显的径向分离,这与散布在热稀薄的团间介质中的冷风团一致。d) 除硅外,发射线宽度在 hetg 光栅分辨率下似乎未解决。(准)中性和电离物种之间没有明显的径向分离,这与散布在热稀薄的团间介质中的冷风团一致。
更新日期:2020-12-26
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