The Flaring Corona of UX Arietis
Abstract
Description
Here we present observational results on the RS CVn star UX Arietis from four very-long-baseline interferometry observations distributed in time to cover the rotational period of 6.44 days. The data are better fit by two Gaussian components than by the usual core-plus-halo model. In the first three days the sizes of the two components did not change much from hour to hour but their relative position and orientation changed from day to day. The origin of this evolution can be explained by geometrical factors (i.e., star rotation). The fourth day a large flare occurred and dramatic changes in the sizes of the Gaussian components were seen.
Procs. of "Coronae of Stars and Accretion Disks", to be published at the Memorie della Societa Astronomica Italiana; 3 pages, 3 figures, 1 table, needs mem.cls
Procs. of "Coronae of Stars and Accretion Disks", to be published at the Memorie della Societa Astronomica Italiana; 3 pages, 3 figures, 1 table, needs mem.cls