Unveiling the spectacular over 24-hour flare of star CD-36 3202

We studied the light curve of the star CD-36 3202, observed by TESS for the presence of stellar spots and to analyze the rotationally modulated flare. We mainly wanted to model the light curve of this flare and estimate its location regarding stellar spots. The flare lasted approximately 27$\,$h. Using our tool new \texttt{findinc\_mc} we managed to estimate the inclination angle of the star to $70^\circ\pm8^\circ$. With \texttt{BASSMAN} we modeled the light curve of the CD-36 3202 and we estimated that three spots are present on the surface of this star. The mean temperature of the spots was about $4000\pm 765\,$K, and the total spottedness was on average $11.61\%\pm0.13\,$\%. We created a new tool named \texttt{MFUEA} to model rotationally modulated flares. Using this software we estimated the latitude of the flare long-duration event equal to $69^{+2}_{-1}\,$deg in latitude. Our estimation of the flare's location was the first recreation of the exact position of a flare compared with the spots. The flare is placed 12$^\circ$ from the center of the coolest spot. This makes the flare related to the magnetic processes above the active region represented by the spot. Removing the effects of rotational modulation from the flare light curve allowed us to correct the estimation of bolometric energy released during the event from $(1.15\pm 0.35)\times 10^{35}\,$erg to $(3.99\pm 1.22)\times 10^{35}\,$erg.Comment: Eight pages, six figures; accepted by A&A on 24/11/202

Analysis of Solar-like X-Class Flare on Wolf 359 Observed Simultaneously with TESS and XMM-Newton

We present an analysis of a flare on the Wolf 359 star based on simultaneous observations of TESS and XMM-Newton. A stellar flare with energy comparable to an X-class solar flare is analyzed on this star for the first time. The main goal of the study was to determine whether the same physical processes drive and occur in stellar flares as in the solar flares. We tried to estimate the flare class by various direct and indirect methods. Light curves and spectra in different energy ranges were used to determine the parameters and profiles of the flare. From the XMM-Newton EPIC-pn X-ray data, we estimated the temperature and emission measure during the flare. The thermodynamical timescale and the loop semi-length were also determined with two different methods. The RGS spectra enabled us to calculate the differential emission measure (DEM) distributions. The obtained DEM distributions have three components at temperature values of 3 MK, 7 MK, and 16-17 MK. The analysis of the line ratio in helium-like triplets allowed us to determine the plasma electron density. Our results for the flare loop on Wolf 359 were compared to typical parameters for solar flares observed with GOES and RHESSI. This supports our conclusion that the processes taking place in stellar flares are like those in solar flares. The determined geometrical parameters of the phenomenon do not differ from the values of analogs occurring on the Sun.Comment: 13 pages, 8 figures, accepted to Ap