近日，XRISM国际协作组揭示了来自超级爱丁顿x射线双星的分层风比预期的要慢。2025年9月17日出版的《自然》杂志发表了这项成果。

在强引力下的吸积盘无处不在地产生风，在恒星质量x射线双星（黑洞和中子星）和超大质量黑洞的x射线波段中可以看到蓝移吸收线。一些最强大的风（称为爱丁顿风）预计会产生于辐射压力足以将物质从内盘（LLEdd）中分离出来的系统。这些风应该速度极快，并携带大量的动能，如果与超大质量黑洞联系在一起，就会使它们成为反馈机制的主要竞争者，这种反馈机制将黑洞的成长与它们的宿主星系联系起来。

研究组展示了银河系中子星x射线双星GX 13+1的XRISM Resolve光谱，它揭示了吸收线中最密集的风之一。这种康普顿厚的风大大削弱了通量，使它看起来很微弱，尽管它本质上比普通的（LLEdd）更发光。然而，这种风极其缓慢，更符合外盘x射线辐射引发的热辐射风的预测，而不是由内盘辐射压力驱动的爱丁顿风的预测。这对双星中明亮吸积流的风的起源提出了新的限制，但也强调了在最近对一个具有类似高爱丁顿比的超大质量黑洞的观测中看到的超快（v~0.3c）风所需要的非常不同的起源。

附：英文原文

Title: Stratified wind from a super-Eddington X-ray binary is slower than expected

Author: Chris Done, Misaki Mizumoto, Joey Neilsen or Ryota Tomaru.

Issue&Volume: 2025-09-17

Abstract: Accretion disks in strong gravity ubiquitously produce winds, seen as blueshifted absorption lines in the X-ray band of both stellar mass X-ray binaries (black holes and neutron stars)1,2,3,4 and supermassive black holes5. Some of the most powerful winds (termed Eddington winds) are expected to arise from systems in which radiation pressure is sufficient to unbind material from the inner disk (LLEdd). These winds should be extremely fast and carry a large amount of kinetic power, which, when associated with supermassive black holes, would make them a prime contender for the feedback mechanism linking the growth of those black holes with their host galaxies6. Here we show the XRISM Resolve spectrum of the galactic neutron star X-ray binary, GX 13+1, which reveals one of the densest winds ever seen in absorption lines. This Compton-thick wind significantly attenuates the flux, making it appear faint, although it is intrinsically more luminous than usual (LLEdd). However, the wind is extremely slow, more consistent with the predictions of thermal-radiative winds launched by X-ray irradiation of the outer disk than with the expected Eddington wind driven by radiation pressure from the inner disk. This puts new constraints on the origin of winds from bright accretion flows in binaries, but also highlights the very different origin required for the ultrafast (v~0.3c) winds seen in recent Resolve observations of a supermassive black hole at a similarly high Eddington ratio7.

DOI: 10.1038/s41586-025-09495-w

Source: https://www.nature.com/articles/s41586-025-09495-w