The 19th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun
Published August 22, 2016 | Version v1
Conference paper Open

The coronal evolution of pre-main-sequence stars

Creators

  • 1. University of St Andrews
  • 2. University of Michigan
  • 3. University of Exeter

Contributors

Contact person:

  • 1. Uppsala University, University of North Georgia

Description

The bulk of X-ray emission from pre-main-sequence (PMS) stars is coronal in origin. We demonstrate herein that stars on Henyey tracks in the Hertzsprung-Russell diagram have lower log(LX/L*), on average, than stars on Hayashi tracks. This effect is driven by the decay of LX once stars develop radiative cores.  LX decays faster with age for intermediate mass PMS stars, the progenitors of main sequence A-type stars, compared to those of lower mass.  As almost all main sequence A-type stars show no detectable X-ray emission, we may already be observing the loss of their coronae during their PMS evolution.  Although there is no direct link between the size or mass of the radiative core and LX, the longer stars have spent with partially convective interiors, the weaker their X-ray emission becomes.  This conference paper is a synopsis of Gregory, Adams & Davies (2016).

Notes

Contributed talk, plenary session.

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Additional details

Related works

Is identical to
arXiv:1608.05434 (arXiv)

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