Stargazing Adventures

AutoPhOT 安装指南（Mac Apple Silicon）

Sat, 07 Feb 2026 13:38:37 +0000

这份说明记录了在 Apple Silicon 设备上成功安装 AutoPhOT 的完整步骤，适用于需要全功能（Astrometry.net + HOTPANTS + PyZOGY）的场景。

盘-冕几何辐射成分示意图

Fri, 23 Jan 2026 01:57:15 +0000

Schematic illustration of (a) a black hole-disk-corona model including thermal, Compton, and reflection components, and (b) a black hole disk model with reflection component from self-irradiation of the disk (thermal returning) and iterative reflection (reflection returning). The color gradient in the disk indicates that the temperature increases towards the black hole. As shown in Fig. 1(a), the observed spectrum of black hole XRBs typically consists of three primary components: (i) a thermal component originating from a geometrically thin, optically thick accretion disk (Shakura & Sunyaev 1973; Page & Thorne 1974) ; (ii) a Comptonized component produced by a hot corona that inverse-Compton scatters soft disk photons (Thorne & Price 1975; Shapiro et al. 1976) ; and (iii) a reflection component resulting from the illumination of the disk by the corona (George & Fabian 1991). The disk is thought to be cold as it can efficiently emit radiation and its thermal spectrum peaks in the soft X-rays (∼ 1 keV). The coronal spectrum takes a power-law like form that can extend to above 100 keV. A particularly important effect in this context is returning radiation (or self-irradiation) (purple and brown arrows in Fig. 1(b)), i.e., disk emission that is bent back onto the accretion disk by the strong gravitational field of the black hole. The first calculations of this effect were performed by Cunningham (1976) in the context of thermal disk spectra, while Li et al.(2005) later showed that it can mimic the effect of a higher accretion rate. credit: [Modeling X-ray reflection spectra from returning radiation:application to 4U 1630–47](https://arxiv.org/pdf/2601.14860)。

macOS下载安装KerrC

Wed, 21 Jan 2026 06:37:52 +0000

## 一、准备 ### 1. 下载KerrC ```shell git clone https://gitlab.com/krawcz/kerrc-x-ray-fitting-code.git ``` ### 2. 安装hdf5 ```shell brew install hdf5 ``` ### 3. 下载安装sherpa ```shell conda create -n sherpa -c https://cxc.cfa.harvard.edu/conda/sherpa -c conda-forge sherpa conda activate sherpa conda install -c conda-forge matplotlib astropy ``` ### 4. 下载和安装boost 下载 ```shell wget https://archives.boost.io/release/1.90.0/source/boost_1_89_0.tar.bz2 ``` 安装 ```shell cd boost_1_89_0 ./bootstrap.sh --with-libraries=python ./b2 -j4 # 屏幕打印 # The Boost C++ Libraries were successfully built! # The following directory should be added to compiler include paths: # /Users/btwang/workshop/code/polarized_radiation_transfer_code/kerrc-x-ray-fitting-code/boost_1_89_0 # The following directory should be added to linker library paths: # /Users/btwang/workshop/code/polarized_radiation_transfer_code/kerrc-x-ray-fitting-code/boost_1_89_0/stage/lib ``` ## 二、编译在进入kerrc-x-ray-fitting-code/raytracing/目录，临时把 Homebrew 放到前面（Apple Silicon 一般是 /opt/homebrew）： ```shell export PATH='/opt/homebrew/bin:$PATH' which h5c++ # 现在应该是 /opt/homebrew/bin/h5c++ ``` ```shell make # 最后打印的内容：5 warnings generated. # h5c++ -lm aliev.o glampedakis.o kerr.o metric.o pani.o wind.o N.o corona.o dataWriter.o xTrack.o -o xTrack ``` ## 三、运行使用以下类型的语句运行代码： ./xTrack -d -D -K -n 2000 -r -10 -c 0000000 -f outdir 这些选项在代码 xTrack.cpp 中进行了解释。

FXTSoft 在 macOS (Apple Silicon) 上安装成功步骤总结

Thu, 01 Jan 2026 13:21:58 +0000

环境背景 • 机器：Apple Silicon（M 系列） • 系统：macOS • 目标：安装 FXTSoft（x86_64） • 已存在：HEASoft（arm64） • 解决思路：Rosetta + Intel Homebrew + 环境切换

下面是一份**“FXTSoft 在 macOS（Apple Silicon）上成功安装”的精简复盘清单**，按时间顺序 + 关键坑位整理，适合你以后快速查阅或给同组同学参考。

XRB不同谱态下吸积流的构型

Wed, 24 Dec 2025 08:35:51 +0000

上图为能谱态下吸积流的构型，点代表ADAF盘，水平条代表薄吸积盘。

Disk-corona模型

Mon, 17 Nov 2025 07:58:41 +0000

Disk-corona模型。

macos免密 SSH 登录服务器

Tue, 28 Oct 2025 11:21:59 +0000

在 macOS 上，免密 SSH 登录服务器的标准方法是通过 SSH 公钥认证（public key authentication）.一次配置好之后，你就可以直接输入： ```bash ssh username@server.address ``` #### 1. 在本地生成密钥在 macOS 终端输入： ```bash ssh-keygen -t rsa -b 4096 -C 'btwang@server' ``` 一路回车即可输出类似： ```bash Generating public/private rsa key pair. Enter file in which to save the key (/Users/yourname/.ssh/id_rsa): ``` 生成的文件： • 私钥：\~/.ssh/id_rsa（保密！） • 公钥：\~/.ssh/id_rsa.pub #### 2. 上传公钥到服务器 ```bash ssh-copy-id username@server.address ``` #### 3. 免密登录 ```bash ssh username@server.address ``` #### 提交slurm作业 ```bash sbatch run_vegas.slurm squeue -u $USER ```。

HMXB 4U 1700-377

Mon, 22 Sep 2025 02:07:26 +0000

Fig. 4. Summary of the fit results. From top to bottom, the modulation curves in phase D and F, the X-ray count rate, PD (2–8 keV), PD (2–4 keV), PD (4–8 keV), column density, photon index, and normalization of the powerlaw. The hatch marks in the PD (2–8 keV) panel represent the MDP for each time interval. The three colors indicating variability are the same as in Figure 3. Alt Text: Summary plot of spectral fit results over time 原文链接：[First Detection of X-ray Polarization and Its Short-term Increase Pre- and Post-Eclipse in HMXB 4U 1700-377](https://arxiv.org/pdf/2509.14494v1)。

M74 X-1

Wed, 17 Sep 2025 03:38:54 +0000

(a) 耀发态观测（观测号：2057、2058、0154350101）同时拟合所得到的光谱与残差，采用的模型为 tbabs*(po)、tbabs*(diskbb+po)、tbabs*(diskbb+gauss+po)，并联动 NH、Tin、Γ 和高斯参数。

ELISA使用教程

Tue, 16 Sep 2025 12:46:37 +0000

### 打印能量 ```python ECLAIRs_pluse1 = Data( name=f'{event_name}_pluse1', erange=[4.0, 20.0], specfile=f'./{folder_name}/GRB250419A_PEO_1er_episode.grp', respfile=f'./{folder_name}/GRB250419A_PEO_rmf_1er_episode.fits', ancrfile=f'./{folder_name}/ECL-RSP-ARF_20220515T01.fits', group='opt' ) print(ECLAIRs_pluse1.channel_emean) ``` ### 计算能量流量 ``` import numpy as np Emax = round(max(ECLAIRs_pluse1.channel_emean)) print(f'Emax={Emax}') Flux = posterior.flux(emin=4,emax=Emax,cl=1.,energy=True,hdi=False,comps=False) median_flux = Flux.median['GRB 250419A_pluse1'].value lower_flux, upper_flux = Flux.intervals['GRB 250419A_pluse1'][0].value, Flux.intervals['GRB 250419A_pluse1'][1].value exponent = np.floor(np.log10(abs(median_flux))) print(f'{median_flux/10**(exponent):.2f} \ (+{(upper_flux - median_flux)/10**(exponent):.2f}, \ {(lower_flux-median_flux)/10**(exponent):.2f}) e{exponent:.0f} erg/cm^2/s') ```。

eROSITA 探测到的新星的分布

Mon, 15 Sep 2025 03:24:10 +0000

图 2：银河系内所有历史新星（灰色）与 eROSITA 探测到的新星（红色）的分布。

The canonical behavior of the early X-ray light curve for GRBs

Fri, 12 Sep 2025 01:29:49 +0000

原文链接：[Evidence for a Canonical GRB Afterglow Light Curve in the Swift XRT Data](https://arxiv.org/pdf/astro-ph/0508332)。

EP250911a的光变曲线和能谱拟合

Fri, 12 Sep 2025 01:16:37 +0000