Evolution of the starspots in V478 Lyrae from 1980 to 1988

Spot modelling of the flare M4.5 dwarf YZ CMi

“…Basically, three major developments in the analysis of spotted stars' light curves have appeared in the last two decades: the analysis of spotted systems with the Wilson-Devinney code (Wilson & Devinney 1971), the systematic approach to fitting circular spots in outline (e.g. Budding 1977, Dorren 1987) and the technique of fitting combinations of an idealized light curve of a single spot to many observed light curves (Hall et al 1989). …”

Zonal Model of Starspots. Application to RS CVn Systems

“…Its photometric variability was discovered by Henry [18] and the complete set of published photometric data has been reviewed by Hall et al [19] For calculating the spotting activity we have used the coefficients dB/dV, dR/dV, and dI/ dV obtained from our unpublished observations of 1994 and the parameters of the star given in Ref. 19.…”

“…The temperature of the spots is T spot = 3640 K ( 185 = ∆ T K). The star experiences very rapid (over a few weeks) changes in the configuration of the spots[19], so our calculations yield a large scatter in the average latitude ϕ of the spots. Since the spotted area and their average latitude are not clearly correlated, we cannot say…”

Learning about Stellar Dynamos from Long–term Photometry of Starspots

“…When a spotted variable is observed continuously for many years, several different spotted regions are seen to appear, exist, and disappear, and typically they have rotation periods which are significantly different from each other. Recent examples of this behavior are V478 Lyr (Hall et al, 1990c), V1817 Cyg = HR 7428 (Hall et al, 1990a), and V1149 Ori = HD 37824 (Hall et al, 1990b). An older example is BY Dra (Oskanyan et al, 1977).…”