Boy is it ever eccentric with eccentricity ~0.8. Maybe the
The chromospherically active bit is because the spin periods of the stars show up as period variations in the brightness on top of the much longer orbital eclipse periods, starspots.
https://arxiv.org/abs/2109.07586
As part of an All-Sky Automated Survey for SuperNovae (ASAS-SN) search for sources with large flux decrements, we discovered a transient where the quiescent, stellar source, ASASSN-V J192114.84+624950.8, rapidly decreased in flux by ∼55% (∼0.9 mag) in the g-band. The \textit{TESS} light curve revealed that the source is a highly eccentric, eclipsing binary. Fits to the light curve using \textsc{phoebe} find the binary orbit to have e=0.79, Porb=18.462 days, and i=88.6∘ and the ratios of the stellar radii and temperatures to be R2/R1=0.71 and Te,2/Te,1=0.82. Both stars are chromospherically active, allowing us to determine their rotational periods of P1=1.52 days and P2=1.79 days, respectively. A LBT/MODS spectrum shows that the primary is a late-G or early-K type dwarf. Fits to the SED show that the luminosities and temperatures of the two stars are $L_1 = 0.48~L_{\sun}$, T1=5050 K, $L_2 = 0.12~L_{\sun}$, and T2=4190 K. We conclude that ASASSN-V J192114.84+624950.8 consists of two chromospherically active, rotational variable stars in a highly elliptical eclipsing orbit.