HADES RV计划与HARPS-N在TNG。VII。根据色球指示器的时间序列高分辨率光谱学的M-矮星的旋转和活动
HADES RV Programme with HARPS-N at TNG. VII. Rotation and activity of M-Dwarfs from time-series high-resolution spectroscopy of chromospheric indicators
摘要：
我们的目标是调查存在的签名的磁周期和旋转的样本71早期M-矮星从HADES RV计划使用高分辨率的时间序列光谱的Ca II H & K和H α色球活动指标，径向速度系列，交叉关联函数和V-波段测光的参数。我们主要使用HARPS-N光谱，获得了四年，并添加HARPS光谱从公共ESO数据库和ASAS测光光变曲线作为支持数据，延长了一些恒星的观测基线长达12年。我们提供了log（R 'hk）测量的所有恒星的样本中，周期长度测量的13颗恒星，旋转周期的33颗恒星，我们能够测量的径向速度信号的半振幅旋转在16颗恒星。我们补充我们的工作与以前的结果，并确认和完善以前报道的色球发射的平均水平之间的关系，测量的日志（R 'hk），与旋转周期，并与测得的半振幅的活动引起的径向速度信号的早期M-矮星。我们寻找了测量的旋转周期和磁周期长度之间的可能关系，发现这两个量之间的弱相关性。利用先前的vsin i测量结果，我们估计了样本中所有恒星的两极与视线的倾角，并估计了行星GJ 3998 b和c的质量范围（2.5 - 4.9 Mearth和6.3 - 12.5 Mearth），GJ 625 b（2.82 Mearth），GJ 3942 b（7.1 - 10.0 Mearth）和GJ 15 A b（3.1 - 3.3 Mearth），假设它们的轨道与恒星旋转共面。
英文摘要：
We aim to investigate the presence of signatures of magnetic cycles and rotation on a sample of 71 early M-dwarfs from the HADES RV programme using high-resolution time-series spectroscopy of the Ca II H & K and Halpha chromospheric activity indicators, the radial velocity series, the parameters of the cross correlation function and the V-band photometry. We used mainly HARPS-N spectra, acquired over four years, and add HARPS spectra from the public ESO database and ASAS photometry light-curves as support data, extending the baseline of the observations of some stars up to 12 years. We provide log(R'hk) measurements for all the stars in the sample, cycle length measurements for 13 stars, rotation periods for 33 stars and we are able to measure the semi-amplitude of the radial velocity signal induced by rotation in 16 stars. We complement our work with previous results and confirm and refine the previously reported relationships between the mean level of chromospheric emission, measured by the log(R'hk), with the rotation period, and with the measured semi-amplitude of the activity induced radial velocity signal for early M-dwarfs. We searched for a possible relation between the measured rotation periods and the lengths of the magnetic cycle, finding a weak correlation between both quantities. Using previous v sin i measurements we estimated the inclinations of the star's poles to the line of sight for all the stars in the sample, and estimate the range of masses of the planets GJ 3998 b and c (2.5 - 4.9 Mearth and 6.3 - 12.5 Mearth), GJ 625 b (2.82 Mearth), GJ 3942 b (7.1 - 10.0 Mearth) and GJ 15A b (3.1 - 3.3 Mearth), assuming their orbits are coplanar with the stellar rotation.
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