Two coherent radio emission mechanisms operate in stellar coronae: plasma emission and cyclotron emission. They directly probe the electron density and magnetic field strength respectively. Most stellar radio detections have been made at cm-wavelengths where it is often not possible to uniquely identify the emission mechanism, hindering the utility of radio observations in probing coronal conditions. In anticipation of stellar observations from a suite of sensitive low-frequency ($ν\sim 10^2\,{\rm MHz}$) radio telescopes, here I apply the general theory of coherent emission in non-relativistic plasma to the low-frequency case. I consider the recently reported low-frequency emission from dMe flare stars AD Leo and UV Ceti and the quiescent star GJ 1151 as test cases. My main conclusion is that unlike the cm-wave regime, for reasonable turbulence saturation regimes, the emission mechanism in metre-wave observations ($ν\sim 10^2\,{\rm MHz}$) can often be identified based on the observed brightness temperature, emission duration and polarisation fraction. I arrive at the following heuristic: M-dwarf emission that is $\gtrsim \,$hour-long with $\gtrsim 50\%$ circular polarised fraction at brightness temperatures of $\gtrsim 10^{12}\,$K at $\sim 100\,{\rm MHz}$ in canonical M-dwarfs strongly favours a cyclotron maser interpretation.
Rotationally modulated highly circularly polarised radio pulses from the rapidly rotating M dwarf ASKAP J181335-604720
Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University（北京师范大学天文与前沿科学研究院）；School of Physics and Astronomy, Beijing Normal University（北京师范大学物理与天文学院）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Physics, The University of Sydney（悉尼大学物理学院）
Unraveling the complex magnetosphere of the B star HD 133880 via wideband observation of coherent radio emission
HD 133880是六颗已知通过电子回旋脉泽发射（ECME）过程产生相干脉冲射电辐射的热磁星之一。在本文中，我们提出了一个广泛的频率范围内，覆盖近300 - 4000兆赫的巨型米波射电望远镜（GMRT）和卡尔G。Jansky甚大阵列（VLA）这项研究是同类研究中的第一项，发现了该现象和宿主恒星的几个有趣特征。我们发现，ECME脉冲的可观察到的属性，例如右和左圆偏振脉冲之间的时间延迟，脉冲的幅度，和它们的上限截止频率似乎是依赖于恒星的方向相对于视线。我们认为，所有这些现象，这是超出了理想的图片，可以归因于一个高度的方位角不对称的物质分布在磁层的磁场轴，这是一个结果的两个高旋转轴（旋转轴和磁场轴之间的角度）的恒星和恒星磁场偏离偶极拓扑结构。
Searching for radio emission from stellar wind-magnetosphere interaction or co-rotation breakdown in brown dwarfs
Institute of Space Sciences (ICE-CSIC)（空间科学研究所）；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究学院）；Institute of Applied Computing & Community Code (IAC3)（应用计算与社区代码研究所）
Coherent radio bursts, polarity reversal, and quiescent emission from the M4V dwarf WW PsA
The University of Sydney（悉尼大学）；ARC Centre of Excellence for Gravitational Wave Discovery (OzGrav)（引力波发现卓越研究中心）；CSIRO Space and Astronomy（澳大利亚联邦科学与工业研究组织空间与天文部）；National Centre for Radio Astrophysics, Tata Institute of Fundamental Research（塔塔基础研究院国家射电天文学中心）；International Centre for Radio Astronomy Research (ICRAR), University of Western Australia（西澳大利亚大学国际射电天文研究中心）；Australia Telescope National Facility, CSIRO Space & Astronomy（澳大利亚望远镜国家设施，澳大利亚联邦科学与工业研究组织空间与天文部）；Swinburne University of Technology（斯威本科技大学）
Jets and Outflows in Young Stellar Objects with the SKAO
Leiden University（莱顿大学）；Univ. Grenoble Alpes（格勒诺布尔阿尔卑斯大学）；Sapienza University of Rome（罗马智慧大学）；Consiglio Nazionale delle Ricerche（意大利国家研究委员会）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）；SOKENDAI (The Graduate University for Advanced Studies)（日本综合研究大学院大学）；University of Leeds（利兹大学）；Academia Sinica（中央研究院）；National Institute of Science Education and Research（国家科学教育与研究机构）；Homi Bhabha National Institute（霍米·巴巴国立研究所）；California Institute of Technology（加州理工学院）
GMRT Survey of Radio Emission from Magnetic Massive Stars -- I: Emission from Single Stars at sub-GHz Frequencies
National Centre for Radio Astrophysics, Tata Institute of Fundamental Research（塔塔基础研究院国家射电天体物理中心）；Department of Physics, Engineering Physics & Astronomy, Queen’s University（女王大学物理、工程物理与天文系）；Department of Physics & Space Science, Royal Military College of Canada（加拿大皇家军事学院物理与空间科学系）；Department of Physics and Astronomy, Bartol Research Institute, University of Delaware（特拉华大学巴托尔研究所物理与天文系）
利用 GMRT 对 28 颗磁热星进行亚千兆赫频率巡天，探测到 11 颗，发现低频射电光度与磁场强度和自转周期相关，并检验了离心突破模型，其中 HD 37742 是首颗在亚千兆赫频率探测到的磁 O 型星。
