发表机构
The University of Sydney; ARC Centre of Excellence for Gravitational Wave Discovery (OzGrav); CSIRO Space and Astronomy; National Centre for Radio Astrophysics, Tata Institute of Fundamental Research; International Centre for Radio Astronomy Research (ICRAR), University of Western Australia; Australia Telescope National Facility, CSIRO Space & Astronomy; Swinburne University of Technology（悉尼大学; 引力波发现卓越研究中心; 澳大利亚联邦科学与工业研究组织空间与天文部; 塔塔基础研究院国家射电天文学中心; 西澳大利亚大学国际射电天文研究中心; 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; 斯威本科技大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
该研究在DINGO调查数据中发现M4V矮星WW PsA的相干射电暴，包括三个长时标圆偏振暴及一个极性反转暴，支持电子回旋脉泽机制，并推断出高倾角物理参数。
AI 中文摘要
磁活动M矮星的相干射电发射主要观察到两种类型：随机类太阳暴和定向的、旋转调制的发射（包括极光脉冲）。对这些恒星的详细监测对于探测驱动发射的等离子体和磁场至关重要。我们对85 pc以内的恒星进行了偏振射电发射搜索，覆盖了来自ASKAP深中性气体起源调查（DINGO）的$2.2\times10^4$小时恒星动态频谱。我们报告发现了来自M4V矮星WW PsA的相干射电暴。除了宁静发射外，我们在283.3小时的数据中探测到三个长持续时间（$\gtrsim$30分钟）的暴，每个暴约100%圆偏振。我们还报告了在我们的搜索未覆盖的一个时期探测到的第四个暴，该暴使用VASTER流水线检测到。其中一个暴在中间出现极性反转，基于此我们倾向于电子回旋脉泽（ECM）机制而非等离子体发射。我们初步提出这些暴是由于旋转调制的ECM脉冲强度变化所致。我们推断了WW PsA所需的物理性质，包括在倾斜转子模型下的高倾角$\beta = 74^{+6}_{-22}$度。
英文摘要
Coherent radio emission from magnetically active M dwarfs is largely observed in two varieties: stochastic solar-like bursts and beamed, rotationally modulated emission including auroral pulses. Detailed monitoring of these stars is critical for probing the plasmas and magnetic fields driving the emission. We conducted a search for polarised radio emission from stars within 85 pc, covering $2.2\times10^4$ h of stellar dynamic spectra from the ASKAP Deep Investigation of Neutral Gas Origins (DINGO) survey. We report the discovery of coherent radio bursts from the M4V dwarf WW PsA. In addition to quiescent emission, we detect three long-duration ($\gtrsim$30 min) bursts, each ~100% circularly polarised, in 283.3 h of data. We also report a fourth burst in an epoch not covered by our search, detected using the VASTER pipeline. One of the bursts features a polarity reversal midway through, based on which we favour the electron cyclotron maser (ECM) mechanism over plasma emission. We tentatively propose the bursts are due to rotationally modulated ECM pulses of variable intensity. We infer the required physical properties of WW PsA, including a high obliquity $β= 74^{+6}_{-22}$ deg under an oblique rotator model.
Comments14 pages, 7 figures, 1 table, accepted for publication in PASA
