标题： 500秒差距内恒星射电种群的统计学：一项VLASS-Gaia DR3研究 显示英文标题

标题： Demography of stellar radio population within 500 pc: A VLASS-Gaia DR3 study

摘要： 在本工作中，我们对VLASS快速查看目录以及\textit{盖亚DR3}进行了系统分析，以确定500pc范围内的3GHz射电发射器的光学对应物，从而获得一个均匀的恒星射电源统计样本。 我们在\textit{盖亚 DR3}颜色-星等图中识别出了3GHz发射器的不同群体。 我们还列出了可能的源（瞬态、高度可变或背景伪影），这些源可以通过后续观测进行确认。 大多数检测到的源由主序G型、K型和M型恒星组成，包括超冷矮星。 明确这些群体的射电辐射来源可以帮助我们进一步了解恒星和行星磁场的起源。 通过分析源的亮度温度与其光谱类型的变化，我们初步将可能的发射机制与不同物体类型相关联。 我们检查了样本中静默射电和X射线发射之间的相关性，这可以为当前对Gudel-Benz关系的理解提供关键见解，这对于建模稳定射电发射和日冕加热至关重要。 这项VLASS-\textit{\textit{盖亚DR3}}分析作为多波长后续观测的试点研究，有助于更好地理解恒星结构、建模耀斑活动并检测由恒星-行星相互作用引起的射电发射。 显示英文摘要

摘要： In this work, we have carried out a systematic analysis of the VLASS quick look catalogs together with \textit{Gaia DR3} to identify the optical counterparts of 3~GHz radio emitters within 500~pc to obtain a homogeneous statistical sample of stellar radio sources. We have identified distinct populations of 3 GHz emitters across the \textit{Gaia DR3} color-magnitude diagram. We also present candidate sources (transient, highly variable or background artifacts) which can be confirmed by follow-up observations. A majority of the detected sources constitute main sequence G, K and M-type stars including ultra-cool dwarfs. Pinning down the origin of radio emission from these populations can help us gain further insights into the origin of stellar and planetary magnetic fields. By analyzing the variation of brightness temperature of the sources with their spectral type, we have tentatively associated possible emission mechanisms with different object types. We inspected the correlation between quiescent radio and X-ray emission for our sample that can provide crucial insights into the current understanding of the Gudel-Benz relationship, which is essential for modeling steady radio emission and coronal heating. This VLASS-\textit{\textit{Gaia DR3}} analysis acts as a pilot study for follow-up observations at multiple wavelengths to better understand stellar structure, model flaring activities and detect radio emission caused by star-planet interactions.