Wenda Zhang, M. Dovvciak, M. Bursa, Jivr'i Svoboda, V. Karas
One of the most promising methods to measure the spin of an accreting black hole is fitting the broad iron Kα line in the X-ray spectrum. The line profile also depends on the geometry of the hard X-ray emitting corona. To put constraints on the black hole spin and corona geometry, it is essential to understand how do they affect the iron Kα line emissivity profile. In this work, we present calculations of the illumination and the iron Kα emissivity profiles performed with the Monte-Carlo GR radiative transfer code Monk. We focus on distinction between the illumination and emissivity profiles, which is in most previous studies neglected. We show that especially for the case of black hole X-ray binaries (BHXRBs), the difference is very large. For active galactic nuclei (AGNs), the emissivity profile has a more similar shape as the illumination profile, but it is notably steeper in the innermost region within a few gravitational radii. We find out that the different behavior between AGN and black hole X-ray binary discs is due to the different energy spectra of the illuminating radiation. This suggests that the emissivity profile of the iron Kα line cannot be determined by black hole spin and corona geometry alone and the energy spectrum of the illuminating radiation has to be taken into account. We also examined the effect of including the self-irradiation, and find it to be more important than the corona emission in BHXRBs.
测量吸积黑洞自旋的最有前途的方法之一是拟合 X 射线光谱中的宽铁 Kα 线。这条线的轮廓还取决于发射硬X射线的日冕的几何形状。要对黑洞自旋和日冕几何形状施加约束，就必须了解它们如何影响铁Kα线的发射率曲线。在这项工作中，我们介绍了利用蒙特卡洛 GR 辐射传递代码 Monk 进行的照明和铁 Kα 辐射率曲线计算。我们重点讨论了照度和发射率剖面之间的区别，这在之前的大多数研究中都被忽略了。我们的研究表明，特别是在黑洞 X 射线双星（BHXRBs）的情况下，两者的差别非常大。对于活动星系核（AGNs），发射率曲线的形状与照度曲线更为相似，但在几个引力半径内的最内侧区域，发射率曲线明显更为陡峭。我们发现，AGN 和黑洞 X 射线双星盘之间的不同行为是由于照明辐射的能谱不同造成的。这表明，铁 Kα 线的发射率曲线不能仅由黑洞自旋和日冕几何决定，还必须考虑照射辐射的能谱。我们还研究了自辐射的影响，发现它比 BHXRBs 中的日冕辐射更重要。
{"title":"Inferring the iron K emissivity profiles of accretion discs irradiated by extended coronae","authors":"Wenda Zhang, M. Dovvciak, M. Bursa, Jivr'i Svoboda, V. Karas","doi":"10.1093/mnras/stae1714","DOIUrl":"https://doi.org/10.1093/mnras/stae1714","url":null,"abstract":"\u0000 One of the most promising methods to measure the spin of an accreting black hole is fitting the broad iron Kα line in the X-ray spectrum. The line profile also depends on the geometry of the hard X-ray emitting corona. To put constraints on the black hole spin and corona geometry, it is essential to understand how do they affect the iron Kα line emissivity profile. In this work, we present calculations of the illumination and the iron Kα emissivity profiles performed with the Monte-Carlo GR radiative transfer code Monk. We focus on distinction between the illumination and emissivity profiles, which is in most previous studies neglected. We show that especially for the case of black hole X-ray binaries (BHXRBs), the difference is very large. For active galactic nuclei (AGNs), the emissivity profile has a more similar shape as the illumination profile, but it is notably steeper in the innermost region within a few gravitational radii. We find out that the different behavior between AGN and black hole X-ray binary discs is due to the different energy spectra of the illuminating radiation. This suggests that the emissivity profile of the iron Kα line cannot be determined by black hole spin and corona geometry alone and the energy spectrum of the illuminating radiation has to be taken into account. We also examined the effect of including the self-irradiation, and find it to be more important than the corona emission in BHXRBs.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"135 16","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141656260","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}
R. Riffel, N. Mallmann, G. S. Ilha, T. Storchi-Bergmann, R. Riffel, S. Rembold, D. Bizyaev, Janaina C do Nascimento, J. Schimoia, L. D. da Costa, N. Boardman, M. Boquien, G. Couto
{"title":"Correction to: Determining star-formation rates in active galactic nuclei hosts via stellar population synthesis","authors":"R. Riffel, N. Mallmann, G. S. Ilha, T. Storchi-Bergmann, R. Riffel, S. Rembold, D. Bizyaev, Janaina C do Nascimento, J. Schimoia, L. D. da Costa, N. Boardman, M. Boquien, G. Couto","doi":"10.1093/mnras/stae1592","DOIUrl":"https://doi.org/10.1093/mnras/stae1592","url":null,"abstract":"","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":" 21","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141676714","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}
{"title":"Correction to: The binding of cosmological structures by massless topological defects","authors":"","doi":"10.1093/mnras/stae1647","DOIUrl":"https://doi.org/10.1093/mnras/stae1647","url":null,"abstract":"","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":" 12","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141674257","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}
{"title":"Correction to: Detecting strongly lensed type Ia supernovae with LSST","authors":"","doi":"10.1093/mnras/stae1662","DOIUrl":"https://doi.org/10.1093/mnras/stae1662","url":null,"abstract":"","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":" 11","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141674589","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}
S. Bellstedt, A. Robotham, S. Driver, Claudia Lagos, L. J. Davies, R. H. W. Cook
{"title":"Correction to: Resolving cosmic star formation histories of present-day bulges, discs, and spheroids with P ro F use","authors":"S. Bellstedt, A. Robotham, S. Driver, Claudia Lagos, L. J. Davies, R. H. W. Cook","doi":"10.1093/mnras/stae1665","DOIUrl":"https://doi.org/10.1093/mnras/stae1665","url":null,"abstract":"","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":" 3","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141674824","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}
{"title":"Correction to: Gamma-ray observations of MAXI J1820+070 during the 2018 outburst","authors":"","doi":"10.1093/mnras/stae1630","DOIUrl":"https://doi.org/10.1093/mnras/stae1630","url":null,"abstract":"","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":" 9","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141676803","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 supernova remnant (SNR) IC 443 is one of the best-studied Galactic SNRs at many wavelengths. It is interacting with a very complex environment, including the SNR G189.6 + 3.3 and H ii regions. In this paper, we report on observations of IC 443 and G189.6 + 3.3 using 1.5- and 1-m telescopes to better understand the nature of these SNRs in the optical band. We obtain H$alpha$ images showing both filamentary and diffuse structures, and long-slit spectra from many locations, with Balmer and forbidden lines detected for IC 443 and G189.6 + 3.3. The [S ii]/ H$alpha$ ratios confirm the SNR nature of G189.6 + 3.3. The ranges of our estimated electron density and pre-shock cloud density clearly indicate the complex structure surrounding IC 443 and G189.6 + 3.3. We also investigate the archival H i data and newly find some shell-like distributions of H i that are possibly associated with G189.6 $+$ 3.3.
超新星残余（SNR）IC 443 是在多种波长下研究得最好的银河系 SNR 之一。它与一个非常复杂的环境相互作用，包括 SNR G189.6 + 3.3 和 H ii 区域。在本文中，我们报告了利用1.5米和1米望远镜对IC 443和G189.6 + 3.3的观测结果，以更好地了解这些光学波段SNR的性质。我们获得了显示丝状结构和弥漫结构的 H$alpha$ 图像，并从许多地方获得了长狭缝光谱，为 IC 443 和 G189.6 + 3.3 探测到了巴尔默线和禁止线。S ii]/ H$alpha$ 比率证实了 G189.6 + 3.3 的 SNR 性质。我们估计的电子密度和震前云密度的范围清楚地表明了IC 443和G189.6 + 3.3周围的复杂结构。我们还研究了存档的 H i 数据，新发现了一些可能与 G189.6 $+$ 3.3 有关的 H i 壳状分布。
{"title":"Optical and H i observations of IC 443 and G189.6 + 3.3 in a complex environment","authors":"H. Bakış, G. Paylı, E. Aktekin, H. Sano, A. Sezer","doi":"10.1093/mnras/stae1653","DOIUrl":"https://doi.org/10.1093/mnras/stae1653","url":null,"abstract":"\u0000 The supernova remnant (SNR) IC 443 is one of the best-studied Galactic SNRs at many wavelengths. It is interacting with a very complex environment, including the SNR G189.6 + 3.3 and H ii regions. In this paper, we report on observations of IC 443 and G189.6 + 3.3 using 1.5- and 1-m telescopes to better understand the nature of these SNRs in the optical band. We obtain H$alpha$ images showing both filamentary and diffuse structures, and long-slit spectra from many locations, with Balmer and forbidden lines detected for IC 443 and G189.6 + 3.3. The [S ii]/ H$alpha$ ratios confirm the SNR nature of G189.6 + 3.3. The ranges of our estimated electron density and pre-shock cloud density clearly indicate the complex structure surrounding IC 443 and G189.6 + 3.3. We also investigate the archival H i data and newly find some shell-like distributions of H i that are possibly associated with G189.6 $+$ 3.3.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":" 8","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141674787","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}
S. Puertas, L. Drissen, C. Robert, L. Rousseau-Nepton, R. Martin, Philippe Amram, Thomas P. Martin
We present a spatially resolved study of the kinematical properties of known supernova remnants (SNRs) in the nearest galaxies of the SIGNALS survey, namely NGC 6822 (one object) and M33 (163 objects), based on data obtained with the SITELLE Imaging Fourier Transform Spectrometer (iFTS) at the Canada-France-Hawaii Telescope. The purpose of this paper is to provide a better scheme of identification for extragalactic SNRs and, in particular, to distinguish between H ii regions and SNRs. For that we have used diagrams which involve both the [S ii]/Hα ratio and the velocity dispersion (σ). We also introduce a new parameter, $xi = {[rm S, small {II}] over Halpha } times sigma$, which enhances still the contrast between SNRs and the rest of the ionised gas. More than 90% of the SNRs in our entire sample show an integrated [S ii]/Hα ratio larger than the canonical value (0.4). 86% of the SNRs present in our field show a significant velocity dispersion. The spectral resolution of our observations allows us to observe the complex velocity structure of some SNRs.
我们根据加拿大-法国-夏威夷望远镜的 SITELLE 成像傅立叶变换光谱仪（iFTS）获得的数据，对 SIGNALS 勘测最近的星系，即 NGC 6822（1 个天体）和 M33（163 个天体）中的已知超新星残余（SNRs）的运动学性质进行了空间分辨研究。本文的目的是为河外 SNR 提供一个更好的识别方案，尤其是区分 H ii 区域和 SNR。为此，我们使用了涉及[S ii]/Hα 比率和速度色散（σ）的图表。我们还引入了一个新参数，$xi = {[rm S, small {II}] over Halpha }。timessigma$，它可以增强SNR与其他电离气体之间的对比度。在我们的整个样本中，90%以上的SNR的综合[S ii]/Hα 比率大于标准值（0.4）。在我们的观测场中，86%的自闪烁体显示出明显的速度色散。我们观测的光谱分辨率使我们能够观测到一些SNR的复杂速度结构。
{"title":"Properties of supernova remnants in SIGNALS galaxies – I. NGC 6822 and M33","authors":"S. Puertas, L. Drissen, C. Robert, L. Rousseau-Nepton, R. Martin, Philippe Amram, Thomas P. Martin","doi":"10.1093/mnras/stae1641","DOIUrl":"https://doi.org/10.1093/mnras/stae1641","url":null,"abstract":"\u0000 We present a spatially resolved study of the kinematical properties of known supernova remnants (SNRs) in the nearest galaxies of the SIGNALS survey, namely NGC 6822 (one object) and M33 (163 objects), based on data obtained with the SITELLE Imaging Fourier Transform Spectrometer (iFTS) at the Canada-France-Hawaii Telescope. The purpose of this paper is to provide a better scheme of identification for extragalactic SNRs and, in particular, to distinguish between H ii regions and SNRs. For that we have used diagrams which involve both the [S ii]/Hα ratio and the velocity dispersion (σ). We also introduce a new parameter, $xi = {[rm S, small {II}] over Halpha } times sigma$, which enhances still the contrast between SNRs and the rest of the ionised gas. More than 90% of the SNRs in our entire sample show an integrated [S ii]/Hα ratio larger than the canonical value (0.4). 86% of the SNRs present in our field show a significant velocity dispersion. The spectral resolution of our observations allows us to observe the complex velocity structure of some SNRs.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"16 4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141693822","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}
Auroral emission lines result from the interaction between magnetic field and stellar wind, offering valuable insights into physical properties and processes occurring within magnetospheres of celestial bodies. While extensively studied in planetary and exoplanetary atmospheres, in ultra-cool dwarfs, and as radio emission from early-type stars, the presence of specific auroral emission lines in hot star spectra remains unexplored. In this study, we utilized TLUSTY code to simulate the auroral lines, while modelling the effect of the interaction between stellar wind and magnetosphere through X-ray irradiation. Utilizing high-resolution synthetic spectra generated from model atmospheres, we identified potential candidate lines indicative of auroral emission, which were absent in non-irradiated spectra. Emission lines in synthetic spectra were present primarily in the infrared domain. The most prominent line generated by irradiation was He ii 69458 Å, which appeared in all our model atmospheres with effective temperatures ranging from 15 kK to 30 kK. We also calculated the minimum irradiation required to detect emission in this most prominent line. The presence of emission lines was interpreted by considering changes in the population of different excited states of given atoms. Besides the appearance of infrared emission lines, high-energy irradiation causes infrared excess. To complement our simulations, we also searched for auroral lines in Far Ultraviolet Spectroscopic Explorer (FUSE) observations, which are deposited in the Multimission Archive at Space Telescope (MAST) catalogue. The comparison of observed spectra with synthetic spectra did not identify any possible candidate emission lines in FUSE spectra.
极光发射线是磁场和恒星风相互作用的结果，为了解天体磁层的物理特性和过程提供了宝贵的信息。虽然对行星和系外行星大气、超冷矮星以及早期型恒星的射电辐射进行了广泛研究，但对热星光谱中存在的特定极光发射线仍未进行探索。在这项研究中，我们利用 TLUSTY 代码模拟了极光线，同时通过 X 射线辐照模拟了恒星风和磁层之间相互作用的影响。利用从模型大气中生成的高分辨率合成光谱，我们确定了指示极光发射的潜在候选线，这些线在非辐照光谱中是不存在的。合成光谱中的发射线主要出现在红外域。辐照产生的最突出的线是 He ii 69458 Å，它出现在我们所有模型大气中，有效温度从 15 kK 到 30 kK 不等。我们还计算了在这条最突出的线中探测到辐射所需的最小辐照度。我们通过考虑特定原子不同激发态的数量变化来解释发射线的存在。除了红外发射线的出现，高能辐照也会导致红外过量。为了补充模拟结果，我们还在远紫外分光探测器（FUSE）的观测数据中寻找极光线，这些数据已存入空间望远镜多任务档案（MAST）目录。将观测到的光谱与合成光谱进行比较后，并未在 FUSE 光谱中发现任何可能的候选发射线。
{"title":"Unveiling stellar aurorae: Simulating auroral emission lines in hot stars induced by high-energy irradiation","authors":"Michal Kajan, J. Krtička, J. Kubát","doi":"10.1093/mnras/stae1273","DOIUrl":"https://doi.org/10.1093/mnras/stae1273","url":null,"abstract":"\u0000 Auroral emission lines result from the interaction between magnetic field and stellar wind, offering valuable insights into physical properties and processes occurring within magnetospheres of celestial bodies. While extensively studied in planetary and exoplanetary atmospheres, in ultra-cool dwarfs, and as radio emission from early-type stars, the presence of specific auroral emission lines in hot star spectra remains unexplored. In this study, we utilized TLUSTY code to simulate the auroral lines, while modelling the effect of the interaction between stellar wind and magnetosphere through X-ray irradiation. Utilizing high-resolution synthetic spectra generated from model atmospheres, we identified potential candidate lines indicative of auroral emission, which were absent in non-irradiated spectra. Emission lines in synthetic spectra were present primarily in the infrared domain. The most prominent line generated by irradiation was He ii 69458 Å, which appeared in all our model atmospheres with effective temperatures ranging from 15 kK to 30 kK. We also calculated the minimum irradiation required to detect emission in this most prominent line. The presence of emission lines was interpreted by considering changes in the population of different excited states of given atoms. Besides the appearance of infrared emission lines, high-energy irradiation causes infrared excess. To complement our simulations, we also searched for auroral lines in Far Ultraviolet Spectroscopic Explorer (FUSE) observations, which are deposited in the Multimission Archive at Space Telescope (MAST) catalogue. The comparison of observed spectra with synthetic spectra did not identify any possible candidate emission lines in FUSE spectra.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"30 19","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140968352","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}
Cheng Liu, Xiaofeng Wang, Xiaobin Zhang, Mikhail Kovalev, Jie Lin, G. Xi, Jun Mo, Gaici Li, Haowei Peng, Xin Li, Qiqi Xia, A. Iskandar, Xiangyun Zeng, Letian Wang, Liying Zhu, Xuan Song, Jincheng Guo, Xiaojun Jiang, Shengyu Yan, Jicheng Zhang
We present a comprehensive photometric and spectroscopic analysis of the short-period (∼5.32 hours) and low-mass eclipsing binary TMTSJ0803 discovered by Tsinghua-Ma Huateng Telescope for Survey (TMTS). By fitting the light curves and radial velocity data with the Wilson–Devinney code, we find that the binary is composed of two late spotted active M dwarfs below the fully convective boundary. This is supported by the discovery of a significant Balmer emission lines in the LAMOST spectrum and prominent coronal X-ray emission. In comparison with the typical luminosity of rapidly rotating fully convective stars, the much brighter X-ray luminosity (LX/Lbol = 0.0159 ± 0.0059) suggests the stellar magnetic activity of fully convective stars could be enhanced in such a close binary system. Given the metallicity of [M/H] = − 0.35 dex as inferred from the LAMOST spectrum, we measure the masses and radii of both stars to be M1 = 0.169 ± 0.010 M⊙, M2 = 0.162 ± 0.016 M⊙, R1 = 0.170 ± 0.006 R⊙, and R2 = 0.156 ± 0.006 R⊙, respectively. Based on the luminosity ratio from the light curve modeling, the effective temperatures of two components are also estimated. In comparison with the stellar evolution models, the radii and effective temperatures of two components are all below the isochrones. The radius deflation might be mainly biased by a small radial velocity (RV) data or (and) a simple correction on RVs, while the discrepancy in effective temperature might be due to the enhanced magnetic activity in this binary.
{"title":"The first low-mass eclipsing binary within the fully convective zone from TMTS","authors":"Cheng Liu, Xiaofeng Wang, Xiaobin Zhang, Mikhail Kovalev, Jie Lin, G. Xi, Jun Mo, Gaici Li, Haowei Peng, Xin Li, Qiqi Xia, A. Iskandar, Xiangyun Zeng, Letian Wang, Liying Zhu, Xuan Song, Jincheng Guo, Xiaojun Jiang, Shengyu Yan, Jicheng Zhang","doi":"10.1093/mnras/stae1266","DOIUrl":"https://doi.org/10.1093/mnras/stae1266","url":null,"abstract":"\u0000 We present a comprehensive photometric and spectroscopic analysis of the short-period (∼5.32 hours) and low-mass eclipsing binary TMTSJ0803 discovered by Tsinghua-Ma Huateng Telescope for Survey (TMTS). By fitting the light curves and radial velocity data with the Wilson–Devinney code, we find that the binary is composed of two late spotted active M dwarfs below the fully convective boundary. This is supported by the discovery of a significant Balmer emission lines in the LAMOST spectrum and prominent coronal X-ray emission. In comparison with the typical luminosity of rapidly rotating fully convective stars, the much brighter X-ray luminosity (LX/Lbol = 0.0159 ± 0.0059) suggests the stellar magnetic activity of fully convective stars could be enhanced in such a close binary system. Given the metallicity of [M/H] = − 0.35 dex as inferred from the LAMOST spectrum, we measure the masses and radii of both stars to be M1 = 0.169 ± 0.010 M⊙, M2 = 0.162 ± 0.016 M⊙, R1 = 0.170 ± 0.006 R⊙, and R2 = 0.156 ± 0.006 R⊙, respectively. Based on the luminosity ratio from the light curve modeling, the effective temperatures of two components are also estimated. In comparison with the stellar evolution models, the radii and effective temperatures of two components are all below the isochrones. The radius deflation might be mainly biased by a small radial velocity (RV) data or (and) a simple correction on RVs, while the discrepancy in effective temperature might be due to the enhanced magnetic activity in this binary.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"35 17","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140971567","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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