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We present the results of a new study on the relationship between coronal X-ray emission and stellar rotation in late-type main-sequence stars. We have selected a sample of 259 dwarfs in the B− V range 0.5-2.0, including 110 field stars and 149 members of the Pleiades, Hyades,α Persei, IC 2602 and IC 2391 open clusters. All the stars have been observed with ROSAT, and most of them have photometrically-measured rotation periods available. Our results confirm that two emission regimes exist, one in which the rotation period is a good predictor of the total X-ray luminosity, and the other in which a constant saturated X-ray to bolometric luminosity ratio is attained; we present a quantitative estimate of the critical rotation periods below which starsof different masses (or spectral types) enter the saturated regime. In thiswork wehave also empirically derived a characteristic time scale,τe, which we have used to investigate the relationship between the X-ray emission level and an X-ray-based Rossby number Re = Prot/τe: we show that our empirical time scaleτe resembles the theoretical convective turnover time for 0.4 . M/M⊙. 1.2, but it also has the same functional dependence on B− V as L −1/2 bol in the color range 0.5 . B− V. 1.5. Our results imply that - for non-saturated coronae - the Lx - Prot relation is equivalent to the Lx/Lbol vs. Re relation.

astronomy and astrophysics

The stellar activity-rotation relationship revisited: Dependence of saturated and non-saturated X-ray emission regimes on stellar mass for late-type dwarfs