Modeling of coronal X-ray emission from active cool stars

  • R. A. Stern
  • S.K. Antiochos
  • F.R. HarndenJr.
Session III: Small Scale Atmospheric Structures: Data
Part of the Lecture Notes in Physics book series (LNP, volume 254)


X-ray pulse-height spectra of the most active cool stars in the Hyades cluster obtained with the Einstein IPC cannot be modeled using isothermal thin plasma emission. Addition of a second isothermal component provides acceptable fits. However, a more physically meaningful set of coronal parameters is provided by models which consist of an ensemble of loops with a single maximum temperature, but with the temperature distribution within the loop determined by loop physics. Such models have been successfully fit to the IPC pulse-height spectra. Constraints on loop parameters are discussed for four F-G dwarfs in the Hyades.


Loop Model Loop Footpoints Isothermal Component Conductive Heat Transport Coronal Parameter 


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Copyright information

© Springer-Verlag 1986

Authors and Affiliations

  • R. A. Stern
    • 1
  • S.K. Antiochos
    • 2
  • F.R. HarndenJr.
    • 3
  1. 1.Lockheed Palo Alto Research LaboratoryUSA
  2. 2.Naval Research LaboratoryUSA
  3. 3.Harvard-Smithsonian Center for AstrophysicsUSA

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