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The solar wind in time

Published online by Cambridge University Press:  05 July 2012

Jeffrey L. Linsky ,
Brian E. Wood  and
Seth Redfield
Jeffrey L. Linsky
Affiliation:
JILA, University of Colorado and NIST, Boulder, Colorado 80309-0440, USA email: jlinsky@jilau1.colorado.edu
Brian E. Wood
Affiliation:
Naval Research Laboratory, Space Science Division, Washington, DC 20375, USA email: brian.wood@nrl.navy.mil
Seth Redfield
Affiliation:
Astronomy Department, Wesleyan University, Middletown, CT 06459, USA email: sredfield@wesleyan.edu
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Abstract

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We describe our method for measuring mass loss rates of F–M main sequence stars with high-resolution Lyman-α line profiles. Our diagnostic is the extra absorption on the blue side the interstellar hydrogen absorption produced by neutral hydrogen gas in the hydrogen walls of stars. For stars with low X-ray fluxes, the correlation of observed mass loss rate with X-ray surface flux and age predicts the solar wind mass flux between 700 Myr and the present.

Keywords

ISM:lines and bandsISM:magnetic fieldssolar windstars:windsSun: UV radiationultraviolet:ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S286: Comparative Magnetic Minima: Characterizing quiet times in the Sun and Stars , October 2011 , pp. 286 - 290
Copyright
Copyright © International Astronomical Union 2012

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