Pub Date : 2025-10-01DOI: 10.1016/j.chinastron.2025.11.010
Wei Wei , Xu Teng , Hou Yong-hui , Sun Yue
Measuring the interference fringes of scientific and tracking targets simultaneously within an equal optical path angle in the atmosphere can result in the accuracy of astrometry at the microarcsecond level through precise optical path difference measurement between the two interference fringes. A phase measurement method based on spatial modulation is proposed for high-precision astrometry using the long baseline stellar interferometer. Synchronous phase shifting is achieved through polarization modulation, providing phase level optical path difference measurement. And the accuracy of optical path difference detection is further improved through multiple measurements and statistical averaging. This article demonstrates the feasibility of the phase detection method through numerical simulation and experiments, with detection accuracy better than 1/18 wavelength and optical path difference statistical measurement accuracy better than 5 nm. Furthermore, the source of error is analyzed through environmental disturbance measurement, laying a technical foundation for achieving the established scientific goal of China's under construction hundred meter long baseline interferometer.
{"title":"Research on the Phase Detection Method in Long Baseline Stellar Interferometer Based on Spatial Modulation","authors":"Wei Wei , Xu Teng , Hou Yong-hui , Sun Yue","doi":"10.1016/j.chinastron.2025.11.010","DOIUrl":"10.1016/j.chinastron.2025.11.010","url":null,"abstract":"<div><div>Measuring the interference fringes of scientific and tracking targets simultaneously within an equal optical path angle in the atmosphere can result in the accuracy of astrometry at the microarcsecond level through precise optical path difference measurement between the two interference fringes. A phase measurement method based on spatial modulation is proposed for high-precision astrometry using the long baseline stellar interferometer. Synchronous phase shifting is achieved through polarization modulation, providing phase level optical path difference measurement. And the accuracy of optical path difference detection is further improved through multiple measurements and statistical averaging. This article demonstrates the feasibility of the phase detection method through numerical simulation and experiments, with detection accuracy better than 1/18 wavelength and optical path difference statistical measurement accuracy better than 5 nm. Furthermore, the source of error is analyzed through environmental disturbance measurement, laying a technical foundation for achieving the established scientific goal of China's under construction hundred meter long baseline interferometer.</div></div>","PeriodicalId":35730,"journal":{"name":"Chinese Astronomy and Astrophysics","volume":"49 4","pages":"Pages 798-808"},"PeriodicalIF":0.0,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145692982","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-10-01DOI: 10.1016/j.chinastron.2025.11.008
Bu Qing-cui
Low magnetic field neutron stars X-ray binaries are the systems where the magnetic field strength of the primary star (neutron star) is less than 10 Gauss. In these systems, the neutron star undergoes Roche lobe overflow, whereby matter is accreted from its companion star through an accretion disk. During the accretion process, a substantial quantity of gravitational energy is released and transformed into X-ray radiation in the vicinity of the neutron star. The X-ray emissions from these systems typically exhibit rapid temporal variability with short time scales, along with changes in spectral characteristics. These celestial objects are of great significance in fundamental physics, particularly in testing general relativity and strong gravitational field effects, as well as studying the equation of state of ultra-dense matter. This review presents a summary of observational research on weakly magnetic field neutron stars in low-mass X-ray binaries, with a focus on recent advancements in the study of kilohertz quasi-periodic oscillations, hard X-ray tails, and the evolution of the accretion disk-corona geometry along the accretion state, since the launch of the Insight-HXMT (Insight Hard Xray Modulation Telescope) satellite.
低磁场中子星x射线双星是指主星（中子星）的磁场强度小于1010高斯的系统。在这些系统中，中子星经历罗氏叶溢出，即物质通过吸积盘从伴星吸积。在吸积过程中，大量的引力能被释放并在中子星附近转化为x射线辐射。这些系统的x射线辐射通常在短时间尺度上表现出快速的时间变异性，以及光谱特征的变化。这些天体在基础物理学中，特别是在检验广义相对论和强引力场效应，以及研究超密物质的状态方程方面具有重要意义。本文综述了低质量x射线双星中弱磁场中子星的观测研究，重点介绍了自Insight- hxmt （Insight hard x射线调制望远镜）卫星发射以来，在千赫兹准周期振荡、硬x射线尾和吸积盘-日冕几何形状沿吸积状态演变的研究进展。
{"title":"Highlight Sciences on Low Magnetic Field Neutron Stars X-ray Binaries with Insight-HXMT","authors":"Bu Qing-cui","doi":"10.1016/j.chinastron.2025.11.008","DOIUrl":"10.1016/j.chinastron.2025.11.008","url":null,"abstract":"<div><div>Low magnetic field neutron stars X-ray binaries are the systems where the magnetic field strength of the primary star (neutron star) is less than 10<span><math><msup><mrow></mrow><mn>10</mn></msup></math></span> Gauss. In these systems, the neutron star undergoes Roche lobe overflow, whereby matter is accreted from its companion star through an accretion disk. During the accretion process, a substantial quantity of gravitational energy is released and transformed into X-ray radiation in the vicinity of the neutron star. The X-ray emissions from these systems typically exhibit rapid temporal variability with short time scales, along with changes in spectral characteristics. These celestial objects are of great significance in fundamental physics, particularly in testing general relativity and strong gravitational field effects, as well as studying the equation of state of ultra-dense matter. This review presents a summary of observational research on weakly magnetic field neutron stars in low-mass X-ray binaries, with a focus on recent advancements in the study of kilohertz quasi-periodic oscillations, hard X-ray tails, and the evolution of the accretion disk-corona geometry along the accretion state, since the launch of the <em>Insight</em>-HXMT (Insight Hard Xray Modulation Telescope) satellite.</div></div>","PeriodicalId":35730,"journal":{"name":"Chinese Astronomy and Astrophysics","volume":"49 4","pages":"Pages 702-711"},"PeriodicalIF":0.0,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145693050","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-10-01DOI: 10.1016/j.chinastron.2025.11.001
Lin Ying-ru , Lu Wei-jian , Qin Huan-chang , Pan Cai-juan
Outflow is a crucial form of quasar feedback and plays a significant role in understanding the co-evolution process of quasars and their host galaxies. This paper collects relevant literatures on the velocity shifts of outflow absorption lines, organizes the case data therein, conducts a comparative analysis of the identification methods, identification difficulties, and formation mechanisms of absorption line velocity shifts, and discusses the future research directions in this field. Although the current number of observational cases of absorption line velocity shifts is limited and their physical mechanisms remain unclear, with the growth of quasar survey data and the advancement of data processing technologies, breakthroughs in related research are expected. The study of absorption line velocity shifts can not only deepen the understanding of quasar outflow phenomena but also provide a new perspective for research on galaxy evolution.
{"title":"Progress in the Study of Velocity Shifts in Quasar Absorption Lines","authors":"Lin Ying-ru , Lu Wei-jian , Qin Huan-chang , Pan Cai-juan","doi":"10.1016/j.chinastron.2025.11.001","DOIUrl":"10.1016/j.chinastron.2025.11.001","url":null,"abstract":"<div><div>Outflow is a crucial form of quasar feedback and plays a significant role in understanding the co-evolution process of quasars and their host galaxies. This paper collects relevant literatures on the velocity shifts of outflow absorption lines, organizes the case data therein, conducts a comparative analysis of the identification methods, identification difficulties, and formation mechanisms of absorption line velocity shifts, and discusses the future research directions in this field. Although the current number of observational cases of absorption line velocity shifts is limited and their physical mechanisms remain unclear, with the growth of quasar survey data and the advancement of data processing technologies, breakthroughs in related research are expected. The study of absorption line velocity shifts can not only deepen the understanding of quasar outflow phenomena but also provide a new perspective for research on galaxy evolution.</div></div>","PeriodicalId":35730,"journal":{"name":"Chinese Astronomy and Astrophysics","volume":"49 4","pages":"Pages 645-664"},"PeriodicalIF":0.0,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145692983","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-10-01DOI: 10.1016/j.chinastron.2025.11.003
Wu Dong-hong
We define an entropy related to mass ordering in multi-planet systems. Through Monte Carlo simulations and -body simulations, we explore the impact of dynamical evolution on the entropy of planetary mass ordering. Our findings suggest that collisions and positional swaps during the dynamical evolution of planetary systems can modify the entropy of mass ordering within the system. Positional swaps tend to gradually increase the entropy of mass ordering, whereas collisions may lead to a decrease. Despite the potential decrease in the system's entropy, the ratio of the current system's mass ordering entropy to the maximum attainable mass ordering entropy consistently rises, indicating the system's progression toward equilibrium. Observations on Kepler multi-planet systems reveal that about 16.9%±4.7% of them still maintain an ordered mass distribution, implying that these systems may not have experienced significant dynamical evolution.
{"title":"Exploring the Evolution of the Entropy Related to Mass Ordering in Multi-planet Systems","authors":"Wu Dong-hong","doi":"10.1016/j.chinastron.2025.11.003","DOIUrl":"10.1016/j.chinastron.2025.11.003","url":null,"abstract":"<div><div>We define an entropy related to mass ordering in multi-planet systems. Through Monte Carlo simulations and <span><math><mi>N</mi></math></span>-body simulations, we explore the impact of dynamical evolution on the entropy of planetary mass ordering. Our findings suggest that collisions and positional swaps during the dynamical evolution of planetary systems can modify the entropy of mass ordering within the system. Positional swaps tend to gradually increase the entropy of mass ordering, whereas collisions may lead to a decrease. Despite the potential decrease in the system's entropy, the ratio of the current system's mass ordering entropy to the maximum attainable mass ordering entropy consistently rises, indicating the system's progression toward equilibrium. Observations on Kepler multi-planet systems reveal that about 16.9%±4.7% of them still maintain an ordered mass distribution, implying that these systems may not have experienced significant dynamical evolution.</div></div>","PeriodicalId":35730,"journal":{"name":"Chinese Astronomy and Astrophysics","volume":"49 4","pages":"Pages 773-784"},"PeriodicalIF":0.0,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145692976","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The detection of dark matter remains a paramount scientific objective in modern astronomy and physics. Axions from Quantum Chromodynamics (QCD) have emerged as natural candidates for dark matter due to their theoretical properties. Currently, efforts are focused on detecting axions with micro-electronvolt mass using electromagnetic responses in GHz-band microwave cavities, but these experiments have yielded null results. Therefore, it is imperative to explore detection strategies for lower-mass axions. This paper addresses the need for detecting lighter axions with subelectronvolt mass by discussing the design and optimization of tunable microwave cavities in the hundreds of MHz band. The study explores the optimal resonant modes, shape factors, and frequency scanning rates for these cavities. Numerical simulations indicate that the proposed eight-rod cavity structure increases the scanning rate nearly a hundredfold compared to standard cavities in the same frequency band, with a reduction in axion detection sensitivity by only about threefold. Although the results presented are based on numerical simulations and require experimental validation, this research offers a forward-looking reference for constructing future experimental setups for QCD axion electromagnetic response detection in the sub-GHz frequency band.
{"title":"Numerical Designs and Parameter Optimizations of Microwave Cavities for the Lighter Dark Matter Axion Detection","authors":"Zhong Zhi-jiang , Zheng Hao , Gao Li , Jiang Qing-quan , Wei Lian-fu","doi":"10.1016/j.chinastron.2025.11.002","DOIUrl":"10.1016/j.chinastron.2025.11.002","url":null,"abstract":"<div><div>The detection of dark matter remains a paramount scientific objective in modern astronomy and physics. Axions from Quantum Chromodynamics (QCD) have emerged as natural candidates for dark matter due to their theoretical properties. Currently, efforts are focused on detecting axions with micro-electronvolt mass using electromagnetic responses in GHz-band microwave cavities, but these experiments have yielded null results. Therefore, it is imperative to explore detection strategies for lower-mass axions. This paper addresses the need for detecting lighter axions with subelectronvolt mass by discussing the design and optimization of tunable microwave cavities in the hundreds of MHz band. The study explores the optimal resonant modes, shape factors, and frequency scanning rates for these cavities. Numerical simulations indicate that the proposed eight-rod cavity structure increases the scanning rate nearly a hundredfold compared to standard cavities in the same frequency band, with a reduction in axion detection sensitivity by only about threefold. Although the results presented are based on numerical simulations and require experimental validation, this research offers a forward-looking reference for constructing future experimental setups for QCD axion electromagnetic response detection in the sub-GHz frequency band.</div></div>","PeriodicalId":35730,"journal":{"name":"Chinese Astronomy and Astrophysics","volume":"49 4","pages":"Pages 739-755"},"PeriodicalIF":0.0,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145692973","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-10-01DOI: 10.1016/j.chinastron.2025.11.005
He Zi-qi , Fu Yu-ming , Wu Xue-bing , He Ling-xue
The Fe Low-ionization Broad Absorption Line Quasar (FeLoBALQ) is one of the rarest types of all quasars. Quasars blow out the surrounding violently, forming extreme outflows from which low ionized elements e.g. Fe provide the absorbing feature in FeLoBALQ spectra. Carrying high kinetic energy, the outflows of FeLoBALQ may possibly be enough for powering the relationship between the supermassive black hole mass and the host-galaxy bulge velocity dispersion . On the other hand, evidence has been found for the co-existence of FeLoBALQ with hosts' starburst or recent major merger. However, the FeLoBALQ sample collected so far is not large enough to stand for these theories statistically. This research focuses on digging out hidden FeLoBALQs from large quasar surveys, forming a FeLoBALQ catalog large enough for statistical and physical analyze. Adopting Convolutional Neural Network (CNN) method, 160 FeLoBALQs are newly identified from totally 50931 quasars in the SDSS (Sloan Digital Sky Survey) DR7Q (Data Release 7 Quasar catalog) in the redshift range of 0.8 2.125, with previous identified FeLoBALQ spectra as training sample. The FeLoBALQs' color is found redder than normal quasars, and previously identified FeLoBALQs are lightly redder than newly identified ones; these differences are more obvious on bluer end than on redder end, and nearly disappear in mid-infrared band. The proportion of FeLoBALQs out of all quasars given is 0.43%, higher than previous prediction, but may still be underestimated. Further researches may expand this method to larger samples e.g. SDSS DR16Q (Data Release 16 Quasar catalog) for larger FeLoBALQ sample, which may help to answer the questions of the relationship between FeLoBALQ and host galaxy star formation, FeLoBALQ and galaxy major merger, and the coevolution of galaxies and central supermassive black holes.
{"title":"Identifying FeLoBAL Quasars in SDSS DR7Q with the Convolutional Neural Network","authors":"He Zi-qi , Fu Yu-ming , Wu Xue-bing , He Ling-xue","doi":"10.1016/j.chinastron.2025.11.005","DOIUrl":"10.1016/j.chinastron.2025.11.005","url":null,"abstract":"<div><div>The Fe Low-ionization Broad Absorption Line Quasar (FeLoBALQ) is one of the rarest types of all quasars. Quasars blow out the surrounding violently, forming extreme outflows from which low ionized elements e.g. Fe provide the absorbing feature in FeLoBALQ spectra. Carrying high kinetic energy, the outflows of FeLoBALQ may possibly be enough for powering the <span><math><mrow><mi>M</mi><mo>−</mo><msub><mi>σ</mi><mo>*</mo></msub></mrow></math></span> relationship between the supermassive black hole mass <span><math><mi>M</mi></math></span> and the host-galaxy bulge velocity dispersion <span><math><msub><mi>σ</mi><mo>*</mo></msub></math></span>. On the other hand, evidence has been found for the co-existence of FeLoBALQ with hosts' starburst or recent major merger. However, the FeLoBALQ sample collected so far is not large enough to stand for these theories statistically. This research focuses on digging out hidden FeLoBALQs from large quasar surveys, forming a FeLoBALQ catalog large enough for statistical and physical analyze. Adopting Convolutional Neural Network (CNN) method, 160 FeLoBALQs are newly identified from totally 50931 quasars in the SDSS (Sloan Digital Sky Survey) DR7Q (Data Release 7 Quasar catalog) in the redshift range of 0.8 <span><math><mrow><mo><</mo><mi>z</mi><mo><</mo></mrow></math></span> 2.125, with previous identified FeLoBALQ spectra as training sample. The FeLoBALQs' color is found redder than normal quasars, and previously identified FeLoBALQs are lightly redder than newly identified ones; these differences are more obvious on bluer end than on redder end, and nearly disappear in mid-infrared band. The proportion of FeLoBALQs out of all quasars given is 0.43%, higher than previous prediction, but may still be underestimated. Further researches may expand this method to larger samples e.g. SDSS DR16Q (Data Release 16 Quasar catalog) for larger FeLoBALQ sample, which may help to answer the questions of the relationship between FeLoBALQ and host galaxy star formation, FeLoBALQ and galaxy major merger, and the coevolution of galaxies and central supermassive black holes.</div></div>","PeriodicalId":35730,"journal":{"name":"Chinese Astronomy and Astrophysics","volume":"49 4","pages":"Pages 756-772"},"PeriodicalIF":0.0,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145692975","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-10-01DOI: 10.1016/j.chinastron.2025.11.004
Wang Dong-ya, Huang Jian, Liang Wei
Track-Catalogue correlation is the precondition and foundation of large scale space object cataloging maintenance. The accuracy of correlation not only affects normal cataloging processing, but also affects the utilization of observation data and the effectiveness of space object surveillance system. In this paper, a method is put forward to improve the correlation accuracy of large-batch orbital track data. Firstly, based on the characteristics of orbit error propagation, a model is constructed to estimate the orbital prediction time error and to correct observation residual, aiming to transfer the large scale spatial error to a small scale time-domain error. Secondly, a correlation judgement model involving a four-parameter-joint feature vector is proposed, with threshold setting guidelines and a data correlation processing flow followed. Finally, some examples with regard to large-batch simulated and actual measured tracks are checked to illustrate the effectiveness of the method.
{"title":"A Track-Catalogue Correlation Method for Space Debris Utilizing Time Error Correction and Multi-Features Joint Judgements","authors":"Wang Dong-ya, Huang Jian, Liang Wei","doi":"10.1016/j.chinastron.2025.11.004","DOIUrl":"10.1016/j.chinastron.2025.11.004","url":null,"abstract":"<div><div>Track-Catalogue correlation is the precondition and foundation of large scale space object cataloging maintenance. The accuracy of correlation not only affects normal cataloging processing, but also affects the utilization of observation data and the effectiveness of space object surveillance system. In this paper, a method is put forward to improve the correlation accuracy of large-batch orbital track data. Firstly, based on the characteristics of orbit error propagation, a model is constructed to estimate the orbital prediction time error and to correct observation residual, aiming to transfer the large scale spatial error to a small scale time-domain error. Secondly, a correlation judgement model involving a four-parameter-joint feature vector is proposed, with threshold setting guidelines and a data correlation processing flow followed. Finally, some examples with regard to large-batch simulated and actual measured tracks are checked to illustrate the effectiveness of the method.</div></div>","PeriodicalId":35730,"journal":{"name":"Chinese Astronomy and Astrophysics","volume":"49 4","pages":"Pages 785-797"},"PeriodicalIF":0.0,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145692981","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-10-01DOI: 10.1016/j.chinastron.2025.11.006
Wang Wei, Zhu Hai-fan
This paper systematically reviews the primary methods for measuring the fundamental parameters of black holes — mass and spin, and briefly introduces techniques for determining the distances to black hole binary systems. Through case studies, it highlights the importance of precise distance measurements in refining the fundamental parameters of black holes. This paper explores three common approaches to black hole mass measurement: dynamical methods, spectral fitting, and quasiperiodic oscillations, while discussing their practical applications and inherent limitations based on observational results. In the aspect of spin measurement, the focus is on the research achievements of the Insight-HXMT (Insight Hard X-ray Modulation Telescope) satellite. The paper provides an in-depth analysis of two methods: thermal continuum fitting and reflection component fitting, emphasizing the crucial role of the Insight-HXMT satellite in spin research. It meticulously dissects the theoretical foundations and model assumptions of these two methods and presents their measurement processes through examples. Furthermore, we showcase the role and advantages of the Insight-HXMT satellite in spin measurement using these methods.
本文系统地回顾了测量黑洞基本参数质量和自旋的主要方法，并简要介绍了确定黑洞双星距离的技术。通过案例研究，强调了精确的距离测量在提炼黑洞基本参数中的重要性。本文探讨了三种常用的黑洞质量测量方法：动力学方法、光谱拟合方法和准周期振荡方法，并根据观测结果讨论了它们的实际应用和固有局限性。在自旋测量方面，重点介绍了Insight- hxmt （Insight Hard x射线调制望远镜）卫星的研究成果。深入分析了热连续体拟合和反射分量拟合两种方法，强调了Insight-HXMT卫星在自旋研究中的关键作用。详细剖析了这两种方法的理论基础和模型假设，并通过实例介绍了它们的测量过程。此外，我们还展示了Insight-HXMT卫星在使用这些方法进行自旋测量中的作用和优势。
{"title":"An Overview of the Insight-HXMT Scientific Satellite Measuring Fundamental Parameters of Black Holes","authors":"Wang Wei, Zhu Hai-fan","doi":"10.1016/j.chinastron.2025.11.006","DOIUrl":"10.1016/j.chinastron.2025.11.006","url":null,"abstract":"<div><div>This paper systematically reviews the primary methods for measuring the fundamental parameters of black holes — mass and spin, and briefly introduces techniques for determining the distances to black hole binary systems. Through case studies, it highlights the importance of precise distance measurements in refining the fundamental parameters of black holes. This paper explores three common approaches to black hole mass measurement: dynamical methods, spectral fitting, and quasiperiodic oscillations, while discussing their practical applications and inherent limitations based on observational results. In the aspect of spin measurement, the focus is on the research achievements of the <em>Insight</em>-HXMT (Insight Hard X-ray Modulation Telescope) satellite. The paper provides an in-depth analysis of two methods: thermal continuum fitting and reflection component fitting, emphasizing the crucial role of the <em>Insight</em>-HXMT satellite in spin research. It meticulously dissects the theoretical foundations and model assumptions of these two methods and presents their measurement processes through examples. Furthermore, we showcase the role and advantages of the <em>Insight</em>-HXMT satellite in spin measurement using these methods.</div></div>","PeriodicalId":35730,"journal":{"name":"Chinese Astronomy and Astrophysics","volume":"49 4","pages":"Pages 678-701"},"PeriodicalIF":0.0,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145692974","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-10-01DOI: 10.1016/j.chinastron.2025.11.007
Yang Shuai-kang, You Bei
Black hole X-ray binary (BHXRB) is a binary system consisting of a central compact black hole and its companion star. Its outburst phase is always accompanied by multi-wavelength emission. With the development of the multi-messenger astronomy, a general picture of the physical processes and spectral energy distribution (SED) behind the multi-wavelength radiation has been formed. The accretion disk and corona around the black hole dominate the X-ray emission; BHXRBs are always accompanied by jets, and the jets are the main source of radio emission; the physical process that dominates the optical/near-infrared emission is more complicated. It is generally believed that there are three physical processes involved, X-ray reprocessing, viscous thermal radiation from the outer accretion disc, and jet emission. Many researches indicate that there is often a clear power-law correlation between the flux of the multi-wavelength emissions. This implies a correlation between the physical processes behind the multi-wavelength emissions. However, the specific physical processes underlying the association between the jet and the accretion disc remain unclear. It has been suggested that the weak external magnetic field in the BHXRB can be radially dragged inwards by the accretion disc to form a strong magnetic field near the black hole. This process results in a significant amplification of the magnetic field in the accretion flow. And it is a prerequisite for theoretical studies of the BZ (Blandford-Znajek) model and the BP (Blandford-Payne) model for jet launching and acceleration. Also, the strong magnetic fields can change the structure of the internal accretion flow, possibly forming the magnetically arrested accretion disks (MADs) in regions close to the black hole. Using the broad band X-ray observations from Insight-HXMT (Insight Hard X-ray Modulation Telescope), we are able to glimpse the high-energy radiation processes occurring in such densely compact regions. we will review the researches on BHXRB accretion magnetic field advection and jets over the decades, and introduce the recent research on black hole accretion and magnetic field advection.
{"title":"Transfer of Magnetic Field and Jets in Black Hole X-Ray Binaries","authors":"Yang Shuai-kang, You Bei","doi":"10.1016/j.chinastron.2025.11.007","DOIUrl":"10.1016/j.chinastron.2025.11.007","url":null,"abstract":"<div><div>Black hole X-ray binary (BHXRB) is a binary system consisting of a central compact black hole and its companion star. Its outburst phase is always accompanied by multi-wavelength emission. With the development of the multi-messenger astronomy, a general picture of the physical processes and spectral energy distribution (SED) behind the multi-wavelength radiation has been formed. The accretion disk and corona around the black hole dominate the X-ray emission; BHXRBs are always accompanied by jets, and the jets are the main source of radio emission; the physical process that dominates the optical/near-infrared emission is more complicated. It is generally believed that there are three physical processes involved, X-ray reprocessing, viscous thermal radiation from the outer accretion disc, and jet emission. Many researches indicate that there is often a clear power-law correlation between the flux of the multi-wavelength emissions. This implies a correlation between the physical processes behind the multi-wavelength emissions. However, the specific physical processes underlying the association between the jet and the accretion disc remain unclear. It has been suggested that the weak external magnetic field in the BHXRB can be radially dragged inwards by the accretion disc to form a strong magnetic field near the black hole. This process results in a significant amplification of the magnetic field in the accretion flow. And it is a prerequisite for theoretical studies of the BZ (Blandford-Znajek) model and the BP (Blandford-Payne) model for jet launching and acceleration. Also, the strong magnetic fields can change the structure of the internal accretion flow, possibly forming the magnetically arrested accretion disks (MADs) in regions close to the black hole. Using the broad band X-ray observations from <em>Insight</em>-HXMT (Insight Hard X-ray Modulation Telescope), we are able to glimpse the high-energy radiation processes occurring in such densely compact regions. we will review the researches on BHXRB accretion magnetic field advection and jets over the decades, and introduce the recent research on black hole accretion and magnetic field advection.</div></div>","PeriodicalId":35730,"journal":{"name":"Chinese Astronomy and Astrophysics","volume":"49 4","pages":"Pages 712-738"},"PeriodicalIF":0.0,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145693051","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-10-01DOI: 10.1016/j.chinastron.2025.11.009
Ma Rui-can
The Insight Hard X-ray Modulation Telescope (Insight-HXMT) satellite has achieved a series of significant scientific breakthroughs during its on-orbit operation, thanks to its unique broadband coverage (1–250 keV) and large effective area. By monitoring the outburst evolution of numerous black hole X-ray binaries (BHXBs), Insight-HXMT has provided crucial observational data for investigating accretion processes during these events. These outbursts include not only typical complete outbursts, which progress through hard, intermediate, and soft states, but also “failed transition outbursts”, where the system remains in the hard or intermediate states without fully transitioning. The broadband capabilities of Insight-HXMT offer a valuable opportunity to gain deeper insights into the properties of the accretion disc, corona, and jet in BHXBs. Furthermore, these observations play a crucial role in advancing our understanding of BHXBs outburst mechanisms and accretion radiation physics. This article focuses on the evolution and characteristics of BHXBs outbursts as revealed by Insight-HXMT data.
{"title":"Study of Outburst Evolution in Black Hole X-ray Binaries with Insight-HXMT","authors":"Ma Rui-can","doi":"10.1016/j.chinastron.2025.11.009","DOIUrl":"10.1016/j.chinastron.2025.11.009","url":null,"abstract":"<div><div>The Insight Hard X-ray Modulation Telescope (<em>Insight</em>-HXMT) satellite has achieved a series of significant scientific breakthroughs during its on-orbit operation, thanks to its unique broadband coverage (1–250 keV) and large effective area. By monitoring the outburst evolution of numerous black hole X-ray binaries (BHXBs), <em>Insight</em>-HXMT has provided crucial observational data for investigating accretion processes during these events. These outbursts include not only typical complete outbursts, which progress through hard, intermediate, and soft states, but also “failed transition outbursts”, where the system remains in the hard or intermediate states without fully transitioning. The broadband capabilities of <em>Insight</em>-HXMT offer a valuable opportunity to gain deeper insights into the properties of the accretion disc, corona, and jet in BHXBs. Furthermore, these observations play a crucial role in advancing our understanding of BHXBs outburst mechanisms and accretion radiation physics. This article focuses on the evolution and characteristics of BHXBs outbursts as revealed by <em>Insight</em>-HXMT data.</div></div>","PeriodicalId":35730,"journal":{"name":"Chinese Astronomy and Astrophysics","volume":"49 4","pages":"Pages 665-677"},"PeriodicalIF":0.0,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145692984","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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