Long Duration Flare Emission: Impulsive or Gradual Heating?
arXiv:1604.05342 · doi:10.3847/0004-637X/820/1/14
Abstract
Flare emissions in X-ray and EUV wavelengths have previously been modeled as the plasma response to impulsive heating from magnetic reconnection. Some flares exhibit gradually evolving X-ray and EUV light curves, which are believed to result from superposition of an extended sequence of impulsive heating events occurring in different adjacent loops or even unresolved threads within each loop. In this paper, we apply this approach to a long duration two-ribbon flare SOL2011-09-13T22 observed by the Atmosphere Imaging Assembly (AIA). We find that to reconcile with observed signatures of flare emission in multiple EUV wavelengths, each thread should be heated in two phases, an intense impulsive heating followed by a gradual, low-rate heating tail that is attenuated over 20-30 minutes. Each AIA resolved single loop may be composed of several such threads. The two-phase heating scenario is supported by modeling with both a zero-dimensional and a 1D hydrodynamic code. We discuss viable physical mechanisms for the two-phase heating in a post-reconnection thread.
References in corpus (7)
- The Interface Region Imaging Spectrograph (IRIS)
- Highly Efficient Modeling of Dynamic Coronal Loops
- Evidence of thermal conduction suppression in a solar flaring loop by coronal seismology of slow-mode waves
- Decay Phase Cooling and Inferred Heating of M- and X-class Solar Flares
- A Quantitative Model of Energy Release and Heating by Time-dependent, Localized Reconnection in a Flare with a Thermal Loop-top X-ray Source
- A simple model of chromospheric evaporation and condensation driven conductively in a solar flare
- How gas-dynamic flare models powered by Petschek reconnection differ from those with ad hoc energy sources
Cited by in corpus (21)
- Spectral signatures of chromospheric condensation in a major solar flare
- Elongation of Flare Ribbons
- What determines the X-ray intensity and duration of a solar flare?
- Transition Region and Chromospheric Signatures of Impulsive Heating Events. II. Modeling
- Effect of transport coefficients on excitation of flare-induced standing slow-mode waves in coronal loops
- Solar Flare Arcade Modelling: Bridging the gap from 1D to 3D Simulations of Optically Thin Radiation
- The direct relation between the duration of magnetic reconnection and the evolution of GOES light curves in solar flares
- Two-Phase Heating in Flaring Loops
- Correlated Spatiotemporal Evolution of Extreme-Ultraviolet Ribbons and Hard X-rays in a Solar Flare
- Efficient Calculation of Non-Local Thermodynamic Equilibrium Effects in Multithreaded Hydrodynamic Simulations of Solar Flares
- The Neupert Effect of Flare UltraViolet and Soft X-ray Emissions
- Connecting Chromospheric Condensation Signatures to Reconnection Driven Heating Rates in an Observed Flare
- Geometric Assumptions in Hydrodynamic Modeling of Coronal and Flaring Loops
- Plasma Brightenings in a Failed Solar Filament Eruption
- Response of SDO/HMI observables to heating of the solar atmosphere by precipitating high-energy electrons
- Comparative study of electric currents and energetic particle fluxes in a solar flare and Earth magnetospheric substorm
- A Model for Gradual Phase Heating Driven by MHD Turbulence in Solar Flares
- Solar Flare Irradiance: Observations and Physical Modeling
- Temperature and differential emission measure evolution of a limb flare on 13 January 2015
- A Solar Magnetic-fan Flaring Arch Heated by Non-thermal Particles and Hot Plasma from an X-ray Jet Eruption
- Tracing Field Lines That Are Reconnecting or Expanding or Both