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Investigating the characteristics of coronal loop heating by 1D hydrodynamic simulations. R. Susino 1 , A. F. Lanza 2 , A. C. Lanzafame 1 , D. Spadaro 2. 1 Dipartimento di Fisica e Astronomia – Università di Catania 2 INAF – Osservatorio Astrofisico di Catania. Introduction.
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Investigating the characteristics of coronal loop heating by 1D hydrodynamic simulations R. Susino1, A. F. Lanza2, A. C. Lanzafame1, D. Spadaro2 1 Dipartimento di Fisica e Astronomia – Università di Catania 2 INAF – Osservatorio Astrofisico di Catania
Introduction • Open question: is the coronal heating an impulsive or steady process? Uniform or localized in space? • Steady uniform heating is consistent with a number of observed EUV and X-ray loops (e.g. Porter and Klimchuck 1995; Schijver et al. 2004, Warren & Winebarger 2006) • Steady heating cannot explain over/under density of warm/hot loops observed with TRACE, SOHO and Yohkoh(e.g. Aschwanden et al. 1999, 2001; Winebarger et al. 2003; Patsourakos et al. 2004, Klimchuk 2006) • Impulsive (in case localized) heating: nanoflare theory • Problems: multi-thermal structure of loops along the LOS, cospatiality of X-ray and EUV loops… • Importance of forward modeling to provide observational signatures of heating mechanisms 2ndSolaire Network Meeting
Numerical model and simulations • Simulations of an AR coronal loop… • ARGOS 1-D hydrodynamic code with PARAMESH package: • Adaptive grid essential to resolve the thin chromospheric-coronal transition region sections of the loop • Different kinds of energy deposition: • Impulsive vs. steady • Localized at loop footpoints vs. uniform 2nd Solaire Network Meeting
Loop model: geometry Loop length: 80 Mm Loop height: 14 Mm CORONA s1 CHROMOSPHERE Loop radius ≈ 200 km Sub-resolution magnetic strand T ≈ 30000K s→ 60 Mm chromospheric section 2ndSolaire Network Meeting
Loop model: initial conditions Tmax= 0.75 MK (TR loop) Nmin= 1.4 x 108 cm-3 v ≈ 0.1 ÷ 0.2 km s-1 τcool ≈ 1000 s Spatially uniform, steady background heating: 2.0 x 10-5 erg s-1 cm-3 2ndSolaire Network Meeting
Heating rate functions Localized heating - Uniform: F(s)=1 Impulsive heating - Steady: G(t)=const. f = asimmetry parameter (0.75) λ = heating scale-length (10 Mm) EI = total heating per unit volume τ = heating time-scale (25 s) 2ndSolaire Network Meeting
Loop dynamic evolutionLocalized vs. uniform heating Localized heating Uniform heating Energy per pulse: 1024 erg Cadence time: 250 s 2nd Solaire Network Meeting
Loop dynamic evolution Impulsive localized heating: cadence variation Cadence time: 250 s 1000 s (≈ τcool) Energy per pulse: 1024 erg 2nd Solaire Network Meeting
Loop dynamic evolution Impulsive localized heating: energy variation Energy per pulse: 1024 erg 0.5 × 1024 erg Cadence time: 250 s 2nd Solaire Network Meeting
Loop dynamic evolution Impulsive localized heating: energy variation Energy per pulse: 1024 erg 2.0 × 1024 erg Cadence time: 250 s 2ndSolaire Network Meeting
Loop dynamic evolution Impulsive vs. steady heating Localized heating Impulsive heating Energy per pulse: 1024 erg Cadence time: 250 s Steady heating Equivalent energy: 1024 erg 2ndSolaire Network Meeting
Loop dynamic evolution Impulsive vs. steady heating Uniform heating Impulsive heating Energy per pulse: 1024 erg Cadence time: 250 s Steady heating Equivalent energy: 1024 erg 2ndSolaire Network Meeting
Differential Emission Measure • Mean DEM computed averaging the DEMs at 300 different times, randomly selected all over the simulation: • Representation of 300 independent strands observed at the same time • Equivalent to a simulated snapshot observation in a single multistranded loop 2ndSolaire Network Meeting
DEM resultsLocalized vs. uniform heating Localized heating Impulsive Steady Uniform heating Impulsive Steady Energy per pulse: 1024 erg Cadence time: 250 s Initial state SERTS89 AR data 2nd Solaire Network Meeting
DEM results Impulsive localized heating: cadence variation Cadence time: 250 s 500 s 1000 s (≈ τcool) Energy per pulse: 1024 erg Initial state SERTS89 AR data 2ndSolaire Network Meeting
DEM results Impulsive localized heating: energy variation Energy per pulse: 0.5 × 1024 erg 1024 erg 2.0 × 1024 erg 4.0 × 1024 erg Cadence time: 250 s Initial state SERTS89 AR data 2ndSolaire Network Meeting
Summary • The localization of the heating near the loop footpoints is essential to reproduce the observed DEM: • Condensation formation → Contribution to the TR temperature part of the DEMs • Uniform heating is inconsistent at low temperatures • Critical dependence on energy deposition details: • Pulse energy, inter-pulse cadence… • Heating temporal variation (steady vs. impulsive heating ) appears to be non influential… 2ndSolaire Network Meeting