Yuchuan Wu's scientific contributions

... Şenavcı et al. (2018) investigate the RS CVn eclipsing binary SV Cam (F9V+K4V) and identify excess absorption which the authors interpret as cool plasma (filaments/prominences) obscuring the primary component. For reviews on stellar CMEs see Moschou et al. (2019), Leitzinger & Odert (2022), Osten (2023), Tian et al. (2023). For the detection of stellar CMEs the approaches are manifold as can already be seen from the methodologies mentioned above. ...

... Previous studies of solar CMEs have proved that CMEs may cause dimmings and Doppler shift signals in the disk-integrated spectra (e.g., Mason et al. 2014Mason et al. , 2016Xu et al. 2022;Lu et al. 2023). Multiple efforts have been carried out to extract similar signals from the stellar spectra (e.g., Argiroffi et al. 2019;Veronig et al. 2021;Chen et al. 2022;Loyd et al. 2022;Lu et al. 2022;Namekata et al. 2021) but there is still no completely unambiguous detection of stellar CMEs so far. This could occur because the spectral resolution and signal-to-noise ratio of the current instruments are not sufficient for detection, or because other manifestations of stellar activity (such as plasma heating/cooling and local flows during flares) could produce similar signals that are difficult to be completely ruled out. ...

... After we acquire the denoised spectrum, a three-component fitting, which has often been applied in stellar flare observations (Wu et al. 2022), is employed to identify the line broadening and red asymmetry of the spectrum. The three components consist of a Voigt function, a Gauss function, and a constant. ...