Modelling nanoflares in active regions and implications for coronal heating mechanisms

P.J. Cargill, H.P. Warren, S.J. Bradshaw

Research output: Contribution to journalArticlepeer-review

35 Citations (Scopus)

Abstract

Recent observations from the Hinode and Solar Dynamics Observatory spacecraft have provided major advances in understanding the heating of solar active regions (ARs). For ARs comprising many magnetic strands or sub-loops heated by small, impulsive events (nanoflares), it is suggested that (i) the time between individual nanoflares in a magnetic strand is 500-2000 s, (ii) a weak 'hot' component (more than 106.6 K) is present, and (iii) nanoflare energies may be as low as a few 1023 ergs. These imply small heating events in a stressed coronal magnetic field, where the time between individual nanoflares on a strand is of order the cooling time. Modelling suggests that the observed properties are incompatible with nanoflare models that require long energy build-up (over 10 s of thousands of seconds) and with steady heating.
Original languageEnglish
JournalPhilosophical Transactions of the Royal Society. A, Mathematical, Physical and Engineering Sciences
Volume373
Issue number2042
Early online date20 Apr 2015
DOIs
Publication statusPublished - 28 May 2015

Keywords

  • Solar corona
  • Magnetic reconnection
  • Emission measure

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