J/other/RMxAA/56.139   On the evolution of angular momentum      (Bohigas, 2020)
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Beginning of ReadMe : J/other/RMxAA/56.139 On the evolution of angular momentum (Bohigas, 2020) ================================================================================ On the evolution of angular momentum, magnetic activity and mass loss rate of late type main sequence stars. Bohigas J. <Rev. Mex. Astron. Astrofis., 56, 139-171 (2020)> =2020RMxAA..56..139B (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Stars, dwarfs ; Stars, late-type ; Photometry ; Magnetic fields Keywords: stars: evolution - stars: late-type - stars: magnetic fields - stars: mass loss - stars: rotation Abstract: Selecting the best quality data, I find that nearly all 0.5 to 1.2M_sun_ main sequence stars converge to a single rotational mass dependent sequence after 750Myr; when the mass is larger than 0.8M_sun_, most of them converge in  120Myr. If stars rotate as rigid bodies, the angular momentum of the vast majority is within clearly outlined bounds. The lower boundary defines a terminal main sequence rotational isochrone, the upper one coincides with slow rotators from the Pleiades and stars from Praesepe delineate a third one. Mass dependent exponential relationships between angular momentum and age are determined from these isochrones. Age estimates based on the angular momentum, are acceptable in middle aged stars older than 750Myr and more massive than 0.6-0.7M_sun_. The evolution of the Rossby number indicates that the Parker dynamo may cease early on in stars where M/M_sun_>=1.1. An empirical formula for the torque, an idealized model for it and a relation between rotational period and magnetic field, lead to a formula for the evolution of the mass loss rate, predicting that the present solar rate is close to a minimum and that it was around five times more vigorous when life on Earth started. Description: The rotational periods of field and open cluster stars computed in 28 publications, were collected to investigate the evolution of angular momentum during main sequence. The open cluster sample was put together with the intention of covering the largest possible range of ages after the termination of the disk locking phase. To homogenize the data set, I collected the spectral type, visual magnitude and classification of each star as reported by SIMBAD, their G, BP and RP band magnitudes and parallax from Gaia DR2, and their J, H and K magnitudes from the Two Micron All Sky Survey. The Gaia magnitudes were used to obtain their Johnson-Cousins visual magnitude. This information is collected in 20 tables, coded as [name]d.dat. Three of these (corotd.dat, hatnetd.dat and keplerd.dat) are for field stars, the others are for 17 open cluster stars with their named coded in the file identification. This tables were used to exclude from further analysis all stars with rotational period and magnitudes with errors greater than 20%, light curve modulations produced by other sources of variability besides single star rotation and object types that may indicate that the angular momentum evolution of a single star may have been affected by an external agent. Stellar parameters for these stars were inferred matching (within error bars) the observed absolute magnitudes in the Johnson-Cousins V band and the Bessel+Brett J,H and K bands to those deduced from the latest Yale-Postdam stellar isochrones. This information is collected in 20 tables, coded as [name]p.dat.

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