Measuring coverage of dark spots on cool stars is important in understanding how stellar magnetic activity scales with the rotation rate and convection zone depth. In this respect, it is crucial to infer surface magnetic patterns on G and K stars, to reveal solar-like stellar dynamos in action. Molecular bands serve as invaluable indicators of cool spots on the surfaces of stars, as they play a crucial role in enabling accurate assessments of the extent of spot coverage across the stellar surface. Therefore, more reliable surface images can be obtained considering the inversion of atomic lines with molecular bands. In this context, we simultaneously carry out Doppler imaging (DI) using atomic lines as well as Titanium Oxide (TiO) band profiles of PW And (K2 V) and also investigate chromospheric activity indicators for the first time in the literature, using the high-resolution spectra. The surface spot distribution obtained from the inversion process represents both atomic line and TiO-band profiles quite accurately. The chromospheric emission is also correlated with photospheric spot coverage, except during a possible flare event during the observations. We detect frequent flare activity, using TESS photometry. We also introduce a new open-source, Python-based DI code SpotDIPy that allows performing surface reconstructions of single stars using the maximum entropy method. We test the code by comparing surface reconstruction simulations with the extensively used DoTS code. We show that the surface brightness distribution maps reconstructed via both codes using the same simulated data are consistent with each other.
The determination of solar wind outflow velocity is fundamental in order to probe the mechanisms of wind acceleration in the corona. We aim to study, via the Doppler dimming technique, the effects that the chromospheric Lyα line profile shape causes on the determination of the outflow speed of coronal HI atoms. The Doppler dimming technique takes into account the decrease of coronal Lyα radiation in regions where HI atoms flow out in the solar wind. Starting from UV observations (UVCS/SOHO) of the coronal Lyα line and simultaneous measurements of pB (LASCO/SOHO and Mk3/MLSO), we studied the ef…
We studied an X1.6 solar flare produced by NOAA AR 12602 on 2014 October 22. The entirety of this event was covered by RHESSI, IRIS, and Hinode/EIS, allowing analysis of the chromospheric response to a nonthermal electron driver. We derived the energy contained in nonthermal electrons via RHESSI spectral fitting, and linked the time-dependent parameters of this call to the response in Doppler velocity, density, and nonthermal width across a broad temperature range. The total energy injected was $4.8\times10^{30}$ erg, and lasted $352$ seconds. This energy drove explosive chromospheric evaporat…
Explosive chromospheric evaporation driven by nonthermal electrons around one footpoint of a solar flare loop
我们探索了2014年10月27日（SOL 2014 -10-27）太阳耀斑脉冲阶段期间微波/HXR发射和多普勒速度之间的时间关系，在耀斑最大值之前，在微波（34 GHz）和硬X射线（HXR，25-50 keV）波段的光变曲线上显示脉冲。成像观测表明，该脉冲主要来自一个太阳耀斑环的一个足点。在这次太阳耀斑期间，界面区成像光谱仪（IRIS）的狭缝就停留在这个足点上。用高斯拟合方法提取了Fe XXI 1354.09 A和Si IV 1402.77 A的多普勒速度。结果表明，Fe XXI 1354.09 A（logT~7.05）在日冕中的热谱线发生了蓝移，而Si IV 1402.77 A（logT~4.8）在过渡区中的冷谱线发生了红移，表明色球发生了爆炸性蒸发。在AIA 131 A图像中还观察到沿火炬环的蒸发上升流。据我们所知，这是第一次报告色球蒸发的证据，从光谱和成像观测在同一耀斑。微波和HXR脉冲都与多普勒速度有很好的相关性，这表明色球蒸发是由太阳耀斑环的这个脚点周围的非热电子驱动的。
Doppler-shifted Signatures in the Chromospheric Line Profiles of II Pegasi
Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences（中国科学院天体结构与演化重点实验室）；International Centre of Supernovae, Yunnan Key Laboratory（超新星国际中心，云南省重点实验室）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）
We present a statistical study of chromospheric evaporation in solar flares using simultaneous observations by the RHESSI X-ray telescope and the IRIS UV spectrograph. The results are compared with radiation hydrodynamic flare models from the F-CHROMA RADYN database. For each event, we study spatially-resolved Doppler shifts of spectral lines formed in the transition region (C\,II\,1334.5\,Å) and hot coronal plasma (Fe\,XXI\,1354.1\,Å) to investigate the dynamics of the solar atmosphere during the flare impulsive phase. We estimate the energy fluxes deposited by high-energy electrons using X-r…
Doppler imaging combined with high-cadence photometry. I. Revisiting the surface of a pre-main-sequence flare star
Kyoto University（京都大学）；Ankara University（安卡拉大学）；Max-Planck-Institut für Sonnensystemforschung（马克斯·普朗克太阳系研究所）；Hitotsubashi University（一桥大学）；The Hakubi Center for Advanced Research, Kyoto University（京都大学哈库比高级研究中心）；NASA Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；The Catholic University of America（美利坚天主教大学）；National Astronomical Observatory of Japan（日本国立天文台）；Nishi-Harima Astronomical Observatory, University of Hyogo（兵库县立西播磨天文台）
To study motions and oscillations in the solar chromosphere and at the transition region (TR) level we analyze some extreme Doppler shifts observed off-limb with the Interface Region Imaging Spectrograph (IRIS). Raster scans and slit-jaw imaging observations performed in the near-ultraviolet (NUV) channels were used. Large transverse oscillations are revealed by the far wings profiles after accurately removing the bulk average line profiles of each sequence. Different regions around the Sun are considered. Accordingly, the cool material of spicules is observed in Mg II lines rather dispersed u…
The relation between stellar magnetic field geometry and chromospheric activity cycles I: The highly variable field of Epsilon Eridani at activity minimum
Spectropolarimetric data allow for simultaneous monitoring of stellar chromospheric $\log{R^{\prime}_{\rm{HK}}}$ activity and the surface-averaged longitudinal magnetic field, $B_l$, giving the opportunity to probe the relationship between large-scale stellar magnetic fields and chromospheric manifestations of magnetism. We present $\log{R^{\prime}_{\rm{HK}}}$ and/or $B_l$ measurements for 954 mid-F to mid-M stars derived from spectropolarimetric observations contained within the PolarBase database. Our magnetically active sample complements previous stellar activity surveys that focus on inac…
Studying cool star magnetic activity gives an important insight into the stellar dynamo and its relationship with stellar properties, as well as allowing us to place the Sun's magnetism in the context of other stars. Only 61 Cyg A (K5V) and $τ$ Boo (F8V) are currently known to have magnetic cycles like the Sun's, where the large-scale magnetic field polarity reverses in phase with the star's chromospheric activity cycles. $τ$ Boo has a rapid $\sim$240 d magnetic cycle, and it is not yet clear whether this is related to the star's thin convection zone or if the dynamo is accelerated by interact…
Young, fast rotating single stars can show dramatically different magnetic signatures and levels of magnetic activity as compared with the Sun. While losing angular momentum due to magnetic breaking and mass loss through stellar winds, the stars gradually spin down resulting in decreasing levels of activity. Studying magnetic activity on such solar analogues plays a key role in understanding the evolution of solar-like stars and allows a glimpse into the past of the Sun as well. In order to widen our knowledge of the magnetic evolution of the Sun and solar-like stars, magnetic activity of the …
A detailed investigation of the magnetic properties of young Sun-like stars can provide valuable information on our Sun's magnetic past and its impact on the early Earth. We determine the properties of the moderately rotating young Sun-like star kappa Ceti's magnetic and activity cycles using 50 years of chromospheric activity data and six epochs of spectropolarimetric observations. The chromospheric activity was determined by measuring the flux in the Ca II H and K lines. A generalised Lomb-Scargle periodogram and a wavelet decomposition were used on the chromospheric activity data to establi…
The behaviour of the large-scale dipolar field, during a star's magnetic cycle, can provide valuable insight into the stellar dynamo and associated magnetic field manifestations such as stellar winds. We investigate the temporal evolution of the dipolar field of the K dwarf 61 Cyg A using spectropolarimetric observations covering nearly one magnetic cycle equivalent to two chromospheric activity cycles. The large-scale magnetic field geometry is reconstructed using Zeeman Doppler imaging, a tomographic inversion technique. Additionally, the chromospheric activity is also monitored. The observa…
First High-resolution Spectroscopic Observations of an Erupting Prominence Within a Coronal Mass Ejection by the Interface Region Imaging Spectrograph (IRIS)
光谱观测日珥喷发与日冕物质抛射（CME），虽然相对罕见，可以提供有价值的等离子体和三维几何诊断。我们报告了2014年5月9日界面区域成像光谱仪（IRIS）任务的首次观测结果，该任务与2014年5月9日相当的X1.6耀斑相关的壮观快速CME/日珥爆发。喷发的最大天平面速度和多普勒速度分别为1200和460 km/s。在多普勒速度上有两个喷发分量，相隔约200公里/秒：一个主要的明亮分量和一个次要的微弱分量，表明物质的分布是中空的，而不是实心的锥形。喷发涉及一个左旋螺旋结构，它正经历逆时针（自上而下）的解旋运动。有一个时间的演变，从向上喷发到向下回落小于自由落体速度和减少非热谱线宽度。我们发现了一个广泛的Mg II K/H线强度比（小于约2预期的光学薄的热发射）：最低的有史以来报道的中位数值为1.17发现的回落材料和一个非常高的值为1.63附近的日冕雨和中间值为1.53和1.41的两个喷发组件。回退材料在k/h比与多普勒速度以及线强度之间表现出强（$> 5 σ$）线性相关性。我们证明，多普勒调光散射色球发射的喷发物质可以潜在地解释这样的特点。
Stellar flares sometimes show red/blue asymmetries of H$α$ line, which can indicate chromospheric dynamics and prominence activations. However, the origin of asymmetries is not completely understood. For a deeper understanding of stellar data, we performed a Sun-as-a-star analysis of H$α$ line profiles of an M4.2-class solar flare showing dominant emissions from flare ribbons by using the data of the Solar Dynamics Doppler Imager onboard the Solar Magnetic Activity Research Telescope at Hida Observatory. The Sun-as-a-star H$α$ spectra of the flare show red asymmetry of up to $\sim$95 km s$^{-1…
Signatures of photospheric convection throughout the solar atmosphere: the EVE Sun-as-a-star mHz continuum
SUPA School of Physics & Astronomy, University of Glasgow（格拉斯哥大学物理与天文学学院）；Space Science Laboratory, University of California, Berkeley（加州大学伯克利分校空间科学实验室）；University of Warwick（华威大学）；Rosseland Centre for Solar Physics, University of Oslo（奥斯陆大学罗瑟兰太阳物理中心）
We discuss observations of the weak first overtone CO absorption band near 2300 nm with the U.S. National Solar Observatory Array Camera (NAC), a modern mid-infrared detector. This molecular band provides a thermal diagnostic that forms lower in the atmosphere than the stronger fundamental band near 4600 nm. The observed center-to-limb increase in CO line width qualitatively agrees with the proposed higher temperature shocks or faster plasma motions higher in the COmosphere. The spatial extent of chromospheric shock waves is currently at or below the diffraction limit of the available C0 lines…
Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. III. Comparison between Starspot Mapping, Zeeman Doppler Imaging, and Multiwavelength Variability
Hitotsubashi University（一桥大学）；The University of Tokyo（东京大学）；The Hakubi Center for Advanced Research, Kyoto University（京都大学博雅研究高级中心）；Department of Physics, Kyoto University（京都大学物理学系）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Department of Physics, The Catholic University of America（美利坚天主教大学物理学系）；Division of Science, National Astronomical Observatory of Japan, NINS（日本国立天文台科学部）；Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, CNES（图卢兹大学、法国国家科学研究中心、法国国家空间研究中心天体物理与行星学研究所在）；Department of Physics, American University（美国大学物理学系）
The Sun as a planet-host star: Proxies from SDO images for HARPS radial-velocity variations
太阳是唯一一颗表面可以直接以高分辨率分辨的恒星，因此构成了探索恒星径向速度（RV）变化的物理起源的绝佳测试案例。我们提出了HARPS观测的阳光散射的明亮的小行星4/灶神星，从中我们推导出太阳的活动驱动的RV变化。与此同时，太阳动力学天文台上的HMI仪器为我们提供了同时的高空间分辨率磁图，多普勒图和连续图像的太阳在Fe I 6173A线。我们确定RV调制所产生的抑制颗粒蓝移磁化区域和暗斑和亮光斑引起的磁通量不平衡。这些贡献的均方根速度幅度分别为2.40 m/s和0.41 m/s，这证实了对流的抑制是活动引起的RV变化的主要来源，根据以前的研究。我们发现斑点和斑区的多普勒不平衡只有弱相关。因此，光变曲线只能给出对流蓝移抑制的不完全预测。相反，我们必须寻找直接跟踪可见恒星半球上的谱斑覆盖的代理。由HARPS谱导出的色球通量指数R'_HK在这方面表现不佳，可能是由于色球和光球临边增亮/变暗的差异。我们还发现，活动驱动的RV变化的太阳是强烈相关的全磁盘磁通量密度，这可能成为一个有用的代理活动相关的RV噪音。
