Measured mass-loss rates of solar-like stars as a function of age and activity

Collisions between the winds of solar-like stars and the local interstellar medium result in a population of hot hydrogen gas surrounding these stars. Absorption from this hot H I can be detected in high-resolution Lyalpha spectra of these stars from the Hubble Space Telescope. The amount of absorption can be used as a diagnostic for the stellar mass-loss rate. We present new mass-loss rate measurements derived in this fashion for four stars (epsilon Eri, 61 Cyg A, 36 Oph AB, and 40 Eri A). Combining these measurements with others, we study how mass loss varies with stellar activity. We find that for the solar-like GK dwarfs, the mass loss per unit surface area is correlated with X-ray surface flux. Fitting a power law to this relation yields (M) over dot proportional to F(X)(1.15+/-0.20). The active M dwarf Proxima Cen and the very active RS CVn system And appear to be inconsistent with this relation. Since activity is known to decrease with age, the above power-law relation for solar-like stars suggests that mass loss decreases with time. We infer a power-law relation of (M) over dot proportional to t(-2.00+/-0.52). This suggests that the solar wind may have been as much as 1000 times more massive in the distant past, which may have had important rami cations for the history of planetary atmospheres in our solar system, that of Mars in particular.