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Cited by 341Stellar, planetary, and galactic studiesSolar and Space Plasma DynamicsAstronomy and Astrophysical Research

TESTING A PREDICTIVE THEORETICAL MODEL FOR THE MASS LOSS RATES OF COOL STARS

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Cranmer, Steven R., Saar, Steven H.·2011·The Astrophysical Journal
DOI 10.1088/0004-637x/741/1/54
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Abstract

The basic mechanisms responsible for producing winds from cool, late-type stars are still largely unknown. We take inspiration from recent progress in understanding solar wind acceleration to develop a physically motivated model of the time-steady mass loss rates of cool main-sequence stars and evolved giants. This model follows the energy flux of magnetohydrodynamic turbulence from a subsurface convection zone to its eventual dissipation and escape through open magnetic flux tubes. We show how Alfvén waves and turbulence can produce winds in either a hot corona or a cool extended chromosphere, and we specify the conditions that determine whether or not coronal heating occurs. These models do not utilize arbitrary normalization factors, but instead predict the mass loss rate directly from a star's fundamental properties. We take account of stellar magnetic activity by extending standard age-activity-rotation indicators to include the evolution of the filling factor of strong photospheric magnetic fields. We compared the predicted mass loss rates with observed values for 47 stars and found significantly better agreement than was obtained from the popular scaling laws of Reimers, Schröder, and Cuntz. The algorithm used to compute cool-star mass loss rates is provided as a self-contained and efficient computer code. We anticipate that the results from this kind of model can be incorporated straightforwardly into stellar evolution calculations and population synthesis techniques.

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  • Stellar winds scale to magnetic fields and activity.

    “Since stellar winds scale to magnetic fields and activity (e.g., Schrijver et al. 2003; Preusse et al. 2005; Cranmer & Saar 2011)”

    From ABOUT EXOBIOLOGY: THE CASE FOR DWARF K STARS (2016) · cites this paper as Cranmer & Saar 2011

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Authors
Cranmer, S. R., & Saar, S. H.
Affiliations
Center for Astrophysics Harvard & Smithsonian (US)
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2011-10-14
Volume
741
Issue
1
Pages
54
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.1088/0004-637x/741/1/54
OpenAlex
W2139806773
Cited by
341
References
1
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FWCI
7.98
Type
journal article
Language
en
Open access
Locations
  • The Astrophysical Journal (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Solar and Space Plasma Dynamics
  • Physical Sciences › Physics and Astronomy › Instrumentation › Astronomy and Astrophysical Research
Keywords
stellar mass loss, cool stars, stellar winds, magnetohydrodynamic turbulence, Alfvén waves, stellar magnetic activity, stellar rotation, coronal heating, main-sequence stars, stellar evolution, population synthesis

About these checks

Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.

Statistics and arithmetic are recomputed, not judged.

Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.

What counts as a claim ›How we measure confidence ›How we check this ›

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