Hydrodynamic flare modeling - Comparison of numerical calculations with SMM observations of the 1980 November 12 17:00 UT flare

Abstract

view Abstract Citations (76) References (21) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Hydrodynamic Flare Modeling: Comparison of Numerical Calculations with SMM Observations of the 1980 November 12 17:00 UT Flare Peres, G. ; Reale, F. ; Serio, S. ; Pallavicini, R. Abstract The results of calculations of the evolution of flaring plasma in a simple coronal loop are compared with SMM observations of a well-studied compact flare. Calculations assuming different models of impulsive heating are performed, all starting from the same initial static loop configuration. A mechanism of local heat deposition and a mechanism of flare heating by energetic electron beams are tested with a variety of parameters. It is found that the evolution of the soft X-ray compact flare is mainly dominated by the thermodynamic and hydrodynamic properties of the confined plasma. In order to obtain a close match between calculated and observed X-ray polychromator light curves, a sizable fraction of impulsive energy must be deposited directly in the corona. Local Fe XXV brightenings in the flaring loop do not provide a good diagnostic of the site of energy deposition in solar flares. The total amount of impulsive energy necessary to match the calculated light curves with the observations depends strongly on the effective deposition depth. Publication: The Astrophysical Journal Pub Date: January 1987 DOI: 10.1086/164936 Bibcode: 1987ApJ...312..895P Keywords: Computational Astrophysics; Magnetohydrodynamic Flow; Solar Flares; Stellar Models; Stellar Spectrophotometry; Emission Spectra; Light Curve; Plasma Control; Solar Maximum Mission; X Ray Spectra; Solar Physics; HYDROMAGNETICS; SUN: FLARES full text sources ADS |