基于CHASE太阳作为恒星光谱观测的太阳暗条质量统计
Statistics of Solar Filament Mass based on CHASE Sun-as-a-star Spectroscopic Observations
AI总结：
本研究利用CHASE的太阳作为恒星观测，通过机器学习识别1346个太阳暗条，建立其三维形态标度，验证了太阳作为恒星估算暗条质量的可靠性，为恒星暗条质量估算提供参考。
AI中文摘要：
暗条是悬浮在太阳及其他恒星高温日冕中的冷而致密的等离子体，准确估算其质量对理解后续爆发及诱发的空间天气效应具有重要意义，但该任务受限于其固有的几何不确定性，尤其是在空间未分辨的恒星观测中。为测试和校准恒星暗条质量估算方法，我们利用中国哈勃太阳探测器（CHASE）的全日面Hα光谱观测，对太阳暗条开展太阳作为恒星的统计分析。通过机器学习分割模型，我们识别出2024年1月至2025年10月期间的共1346个暗条；通过空间积分暗条区域构建虚拟太阳作为恒星光谱，再通过云模型拟合得到其光学参数。校正投影效应后，我们建立了具有代表性的三维形态标度：长度、视宽度与视线深度的比例约为L:W_app:D_LOS≈4.5:1:1.7，暗条深度的中位数约为8000公里。值得注意的是，全样本中太阳作为恒星估算的质量与空间分辨的本征质量高度一致，对数空间回归斜率为1.07。作为首个太阳暗条的大样本太阳作为恒星研究，我们的结果为暗条几何与质量提供了经验约束，为基于Hα光谱估算恒星暗条质量提供了关键参考。
英文摘要：
Filaments are cool and dense plasmas suspended in the hot corona of the Sun and other stars. Accurately estimating their masses is of great significance for understanding subsequent eruptions and induced space weather effects, but it remains hindered by their intrinsic geometric uncertainties, particularly in spatially unresolved stellar observations. To test and calibrate the methods for estimating the masses of stellar filaments, we conduct a statistical Sun-as-a-star analysis of solar filaments, utilizing full-disk H$α$ spectroscopic observations from the Chinese H$α$ Solar Explorer (CHASE). A total of 1346 filaments, covering a period from January 2024 to October 2025, are identified via a machine-learning segmentation model. We construct their virtual sun-as-a-star spectra by spatially integrating the filament regions and then obtain their optical parameters by cloud-model fitting. Upon correcting projection effects, we establish a representative three-dimensional morphological scaling of length, apparent width, and line-of-sight depth ($L:W_{\rm app}:D_{\rm LOS} \approx 4.5:1:1.7$), with a median filament depth of about 8000 km. Interestingly, the Sun-as-a-star estimated mass shows high consistency with the resolved intrinsic mass across the full sample, with a log-space regression slope of 1.07. As the first large-sample Sun-as-a-star study of solar filaments, our results provide empirical constraints on filament geometries and masses, offering a critical reference for estimating stellar filament masses based on H$α$ spectroscopy.
