Is a High Mass Loss Rate for the Sun a Solution to the Faint Young Sun Paradox?

Details Is a High Mass Loss Rate for the Sun a Solution to the Faint Young Sun Paradox? Is a High Mass Loss Rate for the Sun a Solution to the Faint Young Sun Paradox?

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21731904l&link_type=abstract

American Astronomical Society, AAS Meeting #217, #319.04; Bulletin of the American Astronomical Society, Vol. 43, 2011

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Scientific paper

During the Archean eon (3.8 Ga) standard stellar evolution theory predicts a solar luminosity of only 75% of the present value; this luminosity predicts freezing surface temperatures on both early Earth and Mars. Yet geological evidence supports the existence of liquid water on these planets during this time. It has been suggested that the Sun had a higher mass and hence higher luminosity at early epochs, but lost mass through a much denser stellar wind. One test of this hypothesis would be detection of large mass loss rates from young solar analogs. However, such detections are difficult due to weak stellar winds and a multi-wavelength study may be necessary. An indirect method of studying these stellar winds and mass loss, involves the interaction of the wind with the interstellar medium (ISM). This interaction leads to Lyman-α absorption lines (aka hydrogen walls). In addition, radio observations of several young, near-by solar-like stars, using the Very Large Array (VLA), have lead to calculations for upper limits of mass loss from these stars. We will present results from a continuation of this latter approach using the Extended Very Large Array (EVLA) to observe the young, near-by solar analogs, π gt01 UMa and κ01 Cet.

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