Two-Phase Heating in Flaring Loops
arXiv:1802.00871 · doi:10.3847/1538-4357/aaad10
Abstract
We analyze and model a C5.7 two-ribbon solar flare observed by SDO, Hinode and GOES on 2011 December 26. The flare is made of many loops formed and heated successively over one and half hours, and their footpoints are brightened in the UV 1600 A before enhanced soft X-ray and EUV missions are observed in flare loops. Assuming that anchored at each brightened UV pixel is a half flaring loop, we identify more than 6,700 half flaring loops, and infer the heating rate of each loop from the UV light curve at the foot-point. In each half loop, the heating rate consists of two phases, an intense impulsive heating followed by a low-rate heating persistent for more than 20 minutes. Using these heating rates, we simulate the evolution of their coronal temperatures and densities with the model of "enthalpy-based thermal evolution of loops" (EBTEL). In the model, suppression of thermal conduction is also considered. This model successfully reproduces total soft X-ray and EUV light curves observed in fifteen pass-bands by four instruments GOES, AIA, XRT, and EVE. In this flare, a total energy of 4.9x10^30 ergs is required to heat the corona, around 40% of this energy is in the slow heating phase. About two fifth of the total energy used to heat the corona is radiated by the coronal plasmas, and the other three fifth transported to the lower atmosphere by thermal conduction.
arXiv comment18 pages, 10 figures, accepted by ApJ
References in corpus (21)
- Highly Efficient Modeling of Dynamic Coronal Loops
- Thermal Diagnostics with the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory: A Validated Method for Differential Emission Measure Inversions
- Microflares and the Statistics of X-ray Flares
- Temporal evolution of multiple evaporating ribbon sources in a solar flare
- A Database of Flare Ribbon Properties From Solar Dynamics Observatory I: Reconnection Flux
- The influence of numerical resolution on coronal density in hydrodynamic models of impulsive heating
- Observations of conduction driven evaporation in the early rise phase of solar flares
- Quantitative Examination of a Large Sample of Supra-Arcade Downflows in Eruptive Solar Flares
- Evidence of thermal conduction suppression in a solar flaring loop by coronal seismology of slow-mode waves
- Evolution of the Loop-Top Source of Solar Flares--Heating and Cooling Processes
- Modeling the Line-of-Sight Integrated Emission in the Corona: Implications for Coronal Heating
- Inference of Heating Properties from "Hot" Non-flaring Plasmas in Active Region Cores I. Single Nanoflares
- 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
- Heating of Flare Loops With Observationally Constrained Heating Functions
- Long Duration Flare Emission: Impulsive or Gradual Heating?
- Evolution of a Current Sheet in a Solar Flare
- Determining Heating Rates in Reconnection Formed Flare Loops of the M8.0 Flare on 2005 May 13
- Hard X-ray and UV Observations of the 2005 January 15 Two-ribbon Flare
- A Flare Observed in Coronal, Transition Region and Helium I 10830 Å Emissions
- Heating and cooling of coronal loops with turbulent suppression of parallel heat conduction
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- Connecting Chromospheric Condensation Signatures to Reconnection Driven Heating Rates in an Observed Flare
- Geometric Assumptions in Hydrodynamic Modeling of Coronal and Flaring Loops
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- Probing the Production of Extreme-ultraviolet Late-Phase Solar Flares by Using the Model Enthalpy-Based Thermal Evolution of Loops
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