Consequences of evolution through the giant domain for stars of 2 - 5 M

Ronald L. Gilliland

Research output: Contribution to journalArticle

Abstract

Stars of 2 - 5 M reside on the main sequence with only extremely weak and narrow surface convection zones suggesting that significant dynamo activity may not be possible. As the stars evolve off the main sequence into the giant domain the convection zone rapidly deepens allowing for the initiation of a dynamo. Evolution into the giant domain also increases the generation of acoustic flux from sub-atmospheric turbulence, the dissipation of which may contribute to chromospheric heating. We discuss the computation of convective turnover time scales for the giant configurations that are structurally quite different from main sequence envelopes. We compare the theoretical expectations for dynamo activity with observations of stellar rotation rates across the HR diagram.

Original languageEnglish (US)
Pages (from-to)183-186
Number of pages4
JournalAdvances in Space Research
Volume6
Issue number8
DOIs
StatePublished - 1986

Fingerprint

Stars
convection
stellar rotation
Hertzsprung-Russell diagram
stars
Atmospheric turbulence
atmospheric turbulence
dissipation
turnover
envelopes
acoustics
turbulence
Acoustics
diagram
Fluxes
heating
timescale
Heating
configurations
Convection

All Science Journal Classification (ASJC) codes

  • Aerospace Engineering
  • Astronomy and Astrophysics
  • Geophysics
  • Atmospheric Science
  • Space and Planetary Science
  • Earth and Planetary Sciences(all)

Cite this

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Consequences of evolution through the giant domain for stars of 2 - 5 M. / Gilliland, Ronald L.

In: Advances in Space Research, Vol. 6, No. 8, 1986, p. 183-186.

Research output: Contribution to journalArticle

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