SIMULATIONS of the MG II K and CA II 8542 LINES from AN ALFVÉN WAVE-HEATED FLARE CHROMOSPHERE

Graham S. Kerr, Lyndsay Fletcher, Alexander J.B. Russell, Joel C. Allred

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76 Citations (Scopus)

Abstract

We use radiation hydrodynamic simulations to examine two models of solar flare chromospheric heating: Alfvén wave dissipation and electron beam collisional losses. Both mechanisms are capable of strong chromospheric heating, and we show that the distinctive atmospheric evolution in the mid-to-upper chromosphere results in Mg ii k-line emission that should be observably different between wave-heated and beam-heated simulations. We also present Ca ii 8542 Å profiles that are formed slightly deeper in the chromosphere. The Mg ii k-line profiles from our wave-heated simulation are quite different from those from a beam-heated model and are more consistent with Interface Region Imaging Spectrograph observations. The predicted differences between the Ca ii 8542 Å in the two models are small. We conclude that careful observational and theoretical study of lines formed in the mid-to-upper chromosphere holds genuine promise for distinguishing between competing models for chromospheric heating in flares.

Original languageEnglish
Article number101
JournalAstrophysical Journal
Volume827
Issue number2
DOIs
Publication statusPublished - 20 Aug 2016

Keywords

  • methods: numerical
  • Sun: atmosphere
  • Sun: chromosphere
  • Sun: flares
  • Sun: UV radiation
  • waves

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