The evolution of X-ray emission in young stars

Thomas Preibisch, Eric D. Feigelson

Research output: Contribution to journalArticle

184 Citations (Scopus)

Abstract

The evolution of magnetic activity in late-type stars is part of the intertwined rotation-age-activity relation, which provides an empirical foundation to the theory of magnetic dynamos. We study the age-activity relation in the premain-sequence (PMS) regime, for the first time using mass-stratified subsamples. The effort is based on the Chandra Orion Ultradeep Project (COUP), which provides very sensitive and homogenous X-ray data on a uniquely large sample of 481 optically well-characterized low-extinction low-mass members of the Orion Nebula Cluster, for which individual stellar masses and ages could be determined. More than 98% of the stars in this sample are detected as X-ray sources. Within the PMS phase for stellar ages in the range ∼0.1-10 Myr, we establish a mild decay in activity with stellar age τ roughly as L X ∝ τ -1/3. On longer timescales, when the Orion stars are compared to main-sequence stars, the X-ray luminosity decay law for stars in the 0.5 M < M < 1.2 M mass range is more rapid with L X ∝ τ -0.75 over the wide range of ages 5 yr < log τ < 9.5 yr. When the fractional X-ray luminosity L X/L bol and the X-ray surface flux are considered as activity indicators, the decay law index is similarly slow for the first 1-100 Myr but accelerates for older stars. The magnetic activity history for M stars with masses 0.1 M < M < 0.4 M is distinctly different. Only a mild decrease in X-ray luminosity, and even a mild increase in L X/L bol and F X, is seen over the 1-100 Myr range, though the X-ray emission does decay over long timescales on the main sequence. Together with COUP results on the absence of a rotation-activity relation in Orion stars, we find that the activity-age decay is strong across the entire history of solar-type stars but is not attributable to rotational deceleration during the early epochs. A combination of tachocline and distributed convective dynamos may be operative in young solar-type stars. The results for the lowest mass stars are most easily understood by the dominance of convective dynamos during both the PMS and main-sequence phases.

Original languageEnglish (US)
Pages (from-to)390-400
Number of pages11
JournalAstrophysical Journal, Supplement Series
Volume160
Issue number2
DOIs
StatePublished - Oct 1 2005

Fingerprint

stars
rotating generators
x rays
decay
luminosity
timescale
histories
surface flux
Orion nebula
history
young
M stars
main sequence stars
deceleration
stellar mass
extinction
time measurement
project

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

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title = "The evolution of X-ray emission in young stars",
abstract = "The evolution of magnetic activity in late-type stars is part of the intertwined rotation-age-activity relation, which provides an empirical foundation to the theory of magnetic dynamos. We study the age-activity relation in the premain-sequence (PMS) regime, for the first time using mass-stratified subsamples. The effort is based on the Chandra Orion Ultradeep Project (COUP), which provides very sensitive and homogenous X-ray data on a uniquely large sample of 481 optically well-characterized low-extinction low-mass members of the Orion Nebula Cluster, for which individual stellar masses and ages could be determined. More than 98{\%} of the stars in this sample are detected as X-ray sources. Within the PMS phase for stellar ages in the range ∼0.1-10 Myr, we establish a mild decay in activity with stellar age τ roughly as L X ∝ τ -1/3. On longer timescales, when the Orion stars are compared to main-sequence stars, the X-ray luminosity decay law for stars in the 0.5 M ⊙ < M < 1.2 M ⊙ mass range is more rapid with L X ∝ τ -0.75 over the wide range of ages 5 yr < log τ < 9.5 yr. When the fractional X-ray luminosity L X/L bol and the X-ray surface flux are considered as activity indicators, the decay law index is similarly slow for the first 1-100 Myr but accelerates for older stars. The magnetic activity history for M stars with masses 0.1 M ⊙ < M < 0.4 M ⊙ is distinctly different. Only a mild decrease in X-ray luminosity, and even a mild increase in L X/L bol and F X, is seen over the 1-100 Myr range, though the X-ray emission does decay over long timescales on the main sequence. Together with COUP results on the absence of a rotation-activity relation in Orion stars, we find that the activity-age decay is strong across the entire history of solar-type stars but is not attributable to rotational deceleration during the early epochs. A combination of tachocline and distributed convective dynamos may be operative in young solar-type stars. The results for the lowest mass stars are most easily understood by the dominance of convective dynamos during both the PMS and main-sequence phases.",
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The evolution of X-ray emission in young stars. / Preibisch, Thomas; Feigelson, Eric D.

In: Astrophysical Journal, Supplement Series, Vol. 160, No. 2, 01.10.2005, p. 390-400.

Research output: Contribution to journalArticle

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