在中子星低质量X射线双星1 RXS J180408中软X射线状态期间的盘反射和可能的盘风。9 -342058

Geometry of the X-ray source 1H 0707-495

We investigate constraints for the size and location of the X-ray source in 1H 0707-495 determined from the shape of the relativistically smeared reflection from the accretion disc. We develop a new code to model an extended X-ray source and we apply it to all archival XMM observations of 1H 0707-495. Contrary to Wilkins et al. we find that the relativistic reflection in this source is not consistent with an extended uniform corona. Instead, we find that the X-ray source must be very compact, with the size of at most a gravitational radius, and located at most at a few gravitational radii from…

GRS 1915+105心跳期间的风-风连接

Disk-Wind Connection During the Heartbeats of GRS 1915+105

在银河系黑洞的软态中可以看到盘和风的特征，而在硬态中可以看到喷流。在这里，我们研究的磁盘风连接在GRS 1915+105的$ρ$类的变化，使用联合NuSTAR钱德拉观测。源显示50秒极限循环振荡。通过包括反射光谱提供的新信息，并使用相位分辨光谱，我们发现，从黑体发射推断的内盘的变化是不匹配的反射测量。后者几乎是恒定的，独立于连续模型。这两个半径只有在星盘温度颜色校正因子改变时才具有可比性，这种影响可能是由于金属丰度的变化引起的星盘不透明度的变化。盘的倾角与从喷流轴推断的倾角相似，并且振荡约10度。同时钱德拉数据显示，存在两个风速在500-5000 km/s之间的风分量，可能还有两个风速达到20，000 km/s（~0.06 c）。色谱柱密度约为5e 22 cm $^{-2}$。测得风响应时间的上限为2秒，这意味着发射半径<6 e10 cm。风速和吸收通量的变化要求风的几何形状在振荡期间发生变化，限制风从距离黑洞290 - 1300 rg的距离发射。这两个数据集都支持基本模型的预测，即凸起起源于内部磁盘，并随着不稳定性的发展而向外移动。

活动星系核硬X射线光子指数$Γ$与反射标度因子$\Re$相关的日冕凝聚

The condensation of the corona for the correlation between the hard X-ray photon index $Γ$ and the reflection scaling factor $\Re$ in active galactic nuclei

观测发现，活动星系核中的硬X射线光子指数$Γ$与康普顿反射标度因子$\Re$之间存在很强的相关性。在本文中，我们提出的$Γ-\Re$相关性可以解释的框架内的凝聚的热日冕到冷吸积盘周围的超大质量黑洞。在该模型中，它被假定为，最初，垂直延伸的热气（日冕）被提供给中央的超大质量黑洞通过捕获的星际介质和恒星风。在这种情况下，当初始质量吸积速率为$\dot M/ \dot M_{\rm Edd} \gtrsim 0.01$，在临界半径$r_{\rm d}$时，部分热气开始凝聚到黑洞的赤道盘平面上，形成内部冷吸积盘。然后，物质以盘冠结构的形式被吸积，这种结构向下延伸到黑洞最里面的稳定圆形轨道。内盘的大小由初始质量吸积率决定。随着初始质量吸积率的增大，内盘尺寸增大，导致康普顿反射标度因子$\Re$增大，硬X射线光子指数$Γ$增大.通过与具有良好拟合的X射线谱的Seyfert星系样本的比较，发现我们的模型可以大致解释观测结果。最后，我们讨论了将我们的模型应用于高质量X射线双星的可能性，这被认为是由来自伴星的热风提供燃料。

用NuSTAR观测快速旋转恒星质量黑洞4U 1630-472中的盘风

The Disk Wind in the Rapidly Spinning Stellar-Mass Black Hole 4U 1630-472 Observed with NuSTAR

我们提出了一个短的NuSTAR观测恒星质量的黑洞和低质量的X射线二进制4U 1630 $-$ 472的分析。由于NuSTAR的灵敏度，在该源中首次清楚地检测到来自内部吸积盘的反射。通过对反射光谱的拟合，我们发现了一个快速旋转的黑洞$a_{*}=0.985^{+0.005}_{-0.014}$（$1σ$统计误差）的证据。然而，档案数据显示，该源的射电光度相对较低。最近声称喷流功率和黑洞自旋之间的关系将预测一个较低的自旋或一个较高的峰值射电光度。我们还报告了在$7.03\pm0.03$千电子伏的吸收功能的明确检测，可能发出信号的磁盘风。如果这条谱线出现在稠密的中等电离气体（$\logξ=3.6^{+0.2}_{-0.3}$）中，并由类氦Fe XXV占主导地位，则风速为$v/c=0.043^{+0.002}_{-0.007}$（12900 $^{+600}_{-2100}$ km s $^{-1}$）。如果这条谱线与更高度电离的气体（$\logξ=6.1^{+0.7}_{-0.6}$）有关，并且主要是Fe XXVI，那么在考虑系统误差后，蓝移的证据只是边缘性的。我们的分析表明，电离风可能在200 $-$ 1100 Rg内发射，并且可能是磁驱动的。

从X射线偏振反射特征看致密天体附近赤道物质的形状与电离

Shape and ionization of equatorial matter near compact objects from X-ray polarization reflection signatures

受IXPE任务启发，本文构建了具有任意电离剖面的光学厚轴对称反射介质模型，探讨0.1-100 keV线偏振对致密天体赤道3D物质结构的推断能力，发现电离变化与反射器形状对观测偏振有显著影响。

方舟120的软、硬X射线过剩的反射源

A reflection origin for the soft and hard X-ray excess of Ark 120

在过去的几年里，人们提出了几种模型来解释在第1型活动星系核（AGN）的X射线谱中观测到的广泛存在的软过剩。特别是，从光致电离吸积盘反射相对论效应模糊已被证明是成功的复制的光谱形状和变异模式的许多来源。作为对这种情况的进一步测试，我们分析了最近对Arakelian 120的~100 ks长的朱雀观测，Arakelian 120是一个典型的“裸”塞弗特1星系，预计没有复杂的吸收系统来模仿软过剩或掩盖这个关键组成部分的固有特性。我们表明，反射模型，允许温暖/模糊和冷/遥远的再处理提供了一个自洽的和令人信服的解释的宽带X射线发射的方舟120，还具有结构化的铁功能和高能量驼峰。虽然温暖的吸收体，风/流出和多康普顿化区域可能发挥重要作用，在源具有更高的光谱复杂性，这种情况下，研究增加了证据的存在模糊盘反射的X射线光谱的1型活动星系核的基本组成部分。

Wideband Study of the Brightest Black Hole X-ray Binary 4U 1543-47 in the 2021 Outburst: Signature of Disk-Wind Regulated Accretion

A comprehensive wideband spectral analysis of the brightest black hole X-ray binary 4U $1543-47$ during its 2021 outburst is carried out for the first time using NICER, NuSTAR, and AstroSat observations by phenomenological and reflection modelling. The source attains a super-Eddington peak luminosity and remains in the soft state, with a small fraction ($< 3\%$) of the inverse-Comptonized photons. The spectral modelling reveals a steep photon index ($Γ\sim 2-2.6$) and relatively high inner disk temperature ($T_{in}\sim 0.9-1.27$ keV). The line-of-sight column density varies between ($0.45-0.54…

A variable ionized disk wind in the black-hole candidate EXO 1846-031

After 34 years, the black-hole candidate EXO 1846-031 went into outburst again in 2019. We investigate its spectral properties in the hard intermediate and the soft states with NuSTAR and Insight-HXMT. A reflection component has been detected in the two spectral states but possibly originating from different illumination spectra: in the intermediate state, the illuminating source is attributed to a hard coronal component, which has been commonly observed in other X-ray binaries, whereas in the soft state the reflection is probably produced by the disk self-irradiation. Both cases support EXO 1…

Evidence for an emerging disc wind and collimated outflow during an X-ray flare in the narrow-line Seyfert 1 galaxy Mrk 335

A triggered 140 ks XMM-Newton observation of the narrow-line Seyfert 1 (NLS1) Mrk 335 in December 2015 caught the active galaxy at its lowest X-ray flux since 2007. The NLS1 is relatively quiescent for the first ~120 ks of the observation before it flares in brightness by a factor of about five in the last 20 ks. Although only part of the flare is captured before the observation is terminated, the data reveal significant differences between the flare and quiescent phases. During the low-flux state, Mrk 335 demonstrates a reflection-dominated spectrum that results from a compact corona around a…

极窄线Seyfert 1星系1H 0707-495的质量和自旋及其对触发相对论喷流的意义

The Mass and Spin of The Extreme Narrow Line Seyfert 1 Galaxy 1H 0707-495 and Its Implications for The Trigger for Relativistic Jets

“复杂的”窄线塞弗特1（NLS 1）1H 0707-495的X射线光谱的相对论反射模型需要一个高自旋、中等倾角、低质量的黑洞。在这些参数固定的情况下，观测到的光学/紫外辐射直接决定了通过外盘的质量吸积速率，从而预测了热光度。这是$140-260~\times$爱丁顿极限。这样一个圆盘应该能产生强风，而风一般都是clusivelous的。改变相对于cluperous风结构的倾角，可以解释“复杂”NLS 1（如1H 0707-495）和“简单”NLS（如PG 1244+026）之间令人费解的差异。拦截风的视线在铁上显示出来自风的热相的深吸收特征，以及当团块隐藏X射线源时的随机下降和复杂吸收（复杂NLS 1），而这两个特征对于更多的正面倾斜都不存在（简单NLS 1）。这种几何形状与相对论反射模型中自旋测量所假设的平盘的清晰视图完全不同，因此即使是1H 0707-495也可能具有低自旋。如果是这样的话，这就重新开启了一个最简单的、因此也是非常有吸引力的可能性，即高黑洞自旋是触发高相对论性（体洛伦兹因子$\sim 10-15$）喷流的充分必要条件。

用朱雀发现天鹅座X-2的红斜K_α铁线

Discovery of Red-Skewed K_alpha iron line in Cyg X-2 with Suzaku

本文报道了在朱雀观测站对中子星低质量X射线双星天鹅座X-2的观测结果。线条轮廓显示出明显的红色翅膀。这一发现增加了观察到红色倾斜铁线的中子星源的数量，并强烈表明这种现象不仅在黑洞中很常见，而且在其他类型的吸积致密物体中也很常见。我们检查的线轮廓的模型，其属性的生产相对论效应，由于从冷吸积盘的X射线辐射的反射，也作为一个结果的线形成在扩展的风/流出配置。这两种模型都能够充分代表所观察到的线轮廓。我们认为线建模的结果在亚秒级的变化。虽然我们无法最终取消的模型之一，我们发现，风的范式有几个相对论磁盘反射模型的优势。

Testing The Lamp-Post and Wind Reverberation Models with XMM-Newton Observations of NGC 5506

The lamp-post geometry is often used to model X-ray data of accreting black holes. Despite its simple assumptions, it has proven to be powerful in inferring fundamental black hole properties such as the spin. Early results of X-ray reverberations showed support for such a simple picture, though wind-reverberation models have also been shown to explain the observed delays. Here, we analyze new and old XMM-Newton observations of the variable Seyfert-1 galaxy NGC 5506 to test these models. The source shows an emission line feature around 6.7 keV that is delayed relative to harder and softer energ…

活动星系核的X射线吸收和反射

X-ray Absorption and Reflection in Active Galactic Nuclei

X射线光谱学提供了一个机会，研究复杂的混合物的发射和吸收成分的环核区域的活动星系核，并了解吸积过程，燃料AGN和反馈的材料，他们的宿主星系。我们描述的光谱特征，可以研究和审查的X射线光谱和光谱变化的活动星系，集中在最近的钱德拉，XMM-牛顿和朱雀数据本地1型活动星系核的进展。我们描述了吸收的证据，涵盖了广泛的柱密度，电离和动力学，并讨论了越来越多的证据，部分覆盖吸收的数据在能量> 10千电子伏。这样的吸收也可以解释所观察到的X射线光谱曲率和可变性的AGN在较低的能量，并可能是一个重要的因素，在塑造这类源的观察到的属性。考虑自洽模型的本地活动星系核表明，X射线光谱可能包括吸收和反射效应的组合，从材料起源于几个光天的黑洞，以及在更大的规模。这是可能的活动星系核X射线光谱可能会受到强烈影响的存在下，预计在系统中具有高吸积率的盘风外流，我们描述的模型，试图预测通过这种风的辐射转移的影响，并讨论了新的数据来测试和解决这些想法的前景。

利用宽吸收线类星体揭示活动星系核盘风的X射线/紫外特性

Unveiling the X-ray/UV properties of disk winds in active galactic nuclei using broad and mini-broad absorption line quasars

本文对Palomar-Green类星体目录中的6个BAL类星体和7个mini-BAL类星体的46个XMM-Newton观测数据进行了统一分析。使用EPIC-pn进行中等质量的X射线光谱，并允许将一般源光谱形状描述为复杂的，显著偏离幂律发射。在不同能带中的简单幂律分析强烈地表明吸收在形成光谱方面比反射更重要。如果允许吸收气体部分覆盖连续谱发射源或被电离，则推断出$10^{22-24}$ cm $^{-2}$量级的大柱密度。当统计数据足够高时，几乎每一个源都被发现在不同的时间尺度上（从几年到几小时）有不同的光谱形状。总而言之，这些观测结果与辐射驱动的吸积盘风形成这些有趣的宇宙源的光谱是一致的。

Reflections On the Anomalous ANITA Events: The Antarctic Subsurface as a Possible Explanation

The ANITA balloon experiment was designed to detect radio signals initiated by neutrinos and cosmic ray air showers. These signals are typically discriminated by the polarization and phase inversions of the radio signal. The reflected signal from cosmic rays suffer phase inversion compared to a direct tau neutrino event. In this paper we study sub-surface reflection, which can occur without phase inversion, in the context of the two anomalous up-going events reported by ANITA. We find that subsurface layers and firn density inversions may plausibly account for the events, while ice fabric laye…

NICER对4U 1630$-$47的光谱与时序分析及其心跳态

NICER Spectral and Timing Analysis of 4U 1630$-$47 and its Heartbeat State

本研究对黑洞X射线双星4U 1630-47的NICER数据进行了光谱和时序分析，发现反射与盘风特征，并通过相位分辨拟合揭示心跳态由内盘辐射压力不稳定性驱动，伴随粘性传播的硬延迟。

Studying the Reflection Spectra of the New Black Hole X-ray Binary Candidate MAXI J1631-479 Observed by NuSTAR: A Variable Broad Iron Line Profile

We present results from the Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the new black hole X-ray binary candidate MAXI J1631-479 at two epochs during its 2018-2019 outburst, which caught the source in a disk dominant state and a power-law dominant state. Strong relativistic disk reflection features are clearly detected, displaying significant variations in the shape and strength of the broad iron emission line between the two states. Spectral modeling of the reflection spectra reveals that the inner radius of the optically-thick accretion disk evolves from $<1.9$ $r_{\rm g}$…

X射线偏振测量作为区分反射和吸收的新工具--对MCG-6-30-15的预测

X-ray polarimetry as a new tool to discriminate reflection from absorption scenarios -- Predictions for MCG-6-30-15

我们提出了模拟的X射线偏振光谱出现的两个竞争的情况下，提出了解释广泛的Fe Kα线在塞弗特1星系MCG-6-30-15。复吸收的偏振签名研究了部分覆盖的情况下，使用cloudspeedwind和比较的反射模型的基础上的灯柱几何形状。的偏振百分比和角度的形状作为光子能量的函数被发现是明显不同的反射和吸收的情况下。相对论反射在1-10 keV能带中产生比吸收明显更强的极化。偏振角的光谱增加了额外的约束：在吸收情况下，它显示出恒定的形状，而相对论反射情况通常导致偏振角随光子能量的平滑旋转。基于这项工作，我们得出结论，一个软X射线偏振仪上的一个小X射线卫星可能已经区分吸收和反射的情况。X射线成像偏振探测器（XIPE）任务可能会带来一个有希望的机会，该任务已向欧空局提出，以响应定于2017年发射的小型（S级）任务。

Generally Applicable Formalism for Modeling the Observable Signatures of Inflows, Outflows, and Moving Coronal Plasma Close to Kerr Black Holes

We present a generally applicable formalism for modeling the emission, absorption, reflection, and reprocessing of radiation by moving plasma streams close to a Kerr Black hole. The formalism can be used to investigate the observational signatures of a wide range of phenomena, including: (i) the reflection of coronal X-ray radiation off plasma plunging from the inner edge of a black hole accretion disk towards the black hole; (ii) the reflection of coronal X-ray emission off the upper layers of a geometrically thick accretion flow; (iii) the illumination of the accretion disk by a corona movin…

The variable, fast soft X-ray wind in PG 1211+143

The analysis of a series of seven observations of the nearby ($z=0.0809$) QSO, PG 1211+143, taken with the Reflection Grating Spectrometer (RGS) on-board XMM-Newton in 2014, are presented. The high resolution soft X-ray spectrum, with a total exposure exceeding 600 ks, shows a series of blue-shifted absorption lines, from the He and H-like transitions of N, O and Ne, as well as from L-shell Fe. The strongest absorption lines are all systematically blue-shifted by $-0.06c$, originating in two absorption zones, from low and high ionization gas. Both zones are variable on timescales of days, with…