Spatiotemporal Energy Partitioning in a Nonthermally Dominated Two-loop Solar Flare

Motorina, G. G.; Fleishman, G. D.; Kontar, Eduard P.

doi:10.3847/1538-4357/ab67d1

Cited by 18 publications

(27 citation statements)

References 76 publications

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“…For the M1.2 flare in our study, there is no distinct demarcation point between the main phase and late phase. Motorina et al (2020) studied a flare as a result of loop-loop interaction on 2013 November 5. One loop is tenuous and hot, while the other is dense and cool.…”

Section: Discussionmentioning

confidence: 99%

“…According to their association with CMEs, flares can be classified into eruptive events and confined events (Moore et al 2001). Confined flares are produced by loop-loop interaction (Motorina et al 2020) or triggered by failed filament eruptions (Ji et al 2003;Song et al 2014;Yan et al 2020). The strong strapping field overlying the active region (AR) core plays a dominant role in constraining the eruptions (Wang & Zhang 2007;Myers et al 2015;Sun et al 2015;Amari et al 2018;Baumgartner et al 2018).…”

Section: Introductionmentioning

confidence: 99%

“…Energy partition in flares is an important issue, which has been extensively explored (e.g., Saint-Hilaire & Benz 2002; Emslie et al 2004Emslie et al , 2005Emslie et al , 2012Chamberlin et al 2012;Feng et al 2013;Hannah & Kontar 2013;Milligan et al 2014;Warmuth & Mann 2016a,b, 2020Motorina et al 2020). Stoiser et al (2007) studied 18 microflares observed by the Ramaty Hight Energy Solar Spectroscopic Imager (RHESSI; Lin et al 2002).…”

Section: Introductionmentioning

confidence: 99%

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Energy partition in a confined flare with an extreme-ultraviolet late phase

Zhang,

Cheng,

Dai

et al. 2021

Preprint

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Aims. In this paper, we reanalyze the M1.2 confined flare with a large extreme-ultraviolet (EUV) late phase on 2011 September 9, focusing on its energy partition. Methods. The flare was observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). The three-dimensional (3D) magnetic fields of active region 11283 before flare were obtained using the nonlinear force free field modeling and the vector magnetograms observed by the Helioseismic and Magnetic Imager (HMI) on board SDO. Properties of the nonthermal electrons injected into the chromosphere were obtained from the hard X-ray observations of the Ramaty Hight Energy Solar Spectroscopic Imager (RHESSI). Soft X-ray fluxes of the flare were recorded by the GOES spacecraft. Irradiance in 1−70 Å and 70−370 Å were measured by the EUV Variability Experiment (EVE) on board SDO. Various energy components of the flare are calculated.Results. The radiation (∼5.4×10 30 erg) in 1−70 Å is nearly eleven times larger than the radiation in 70−370 Å, and is nearly 180 times larger than the radiation in 1−8 Å. The peak thermal energy of the post-flare loops is estimated to be (1.7−1.8)×10 30 erg based on a simplified schematic cartoon. Based on previous results of Enthalpy-Based Thermal Evolution of Loops (EBTEL) simulation, the energy inputs in the main flaring loops and late-phase loops are (1.5−3.8)×10 29 erg and 7.7×10 29 erg, respectively. The nonthermal energy ((1.7−2.2)×10 30 erg) of the flare-accelerated electrons is comparable to the peak thermal energy and is sufficient to provide the energy input of the main flaring loops and late-phase loops. The magnetic free energy (9.1×10 31 erg) before flare is large enough to provide the heating requirement and radiation, indicating that the magnetic free energy is adequate to power the flare.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Energy partition in a confined flare with an extreme-ultraviolet late phase

Zhang,

Cheng,

Dai

et al. 2021

Preprint

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“…To provide the scattering rate (i.e., the qǫ 2 parameter) comparable with that of the observations, magnetic tubes would need to have the density contrast of δn/n ≫ 1 (e.g., Robinson 1983 considered a 25-fold increase of the plasma density over dense fibres). Existence of such structures in the solar corona is not supported by EUV observations (e.g., Motorina et al 2020).…”

Section: Monte Carlo Simulation Set-upmentioning

confidence: 92%

Radio Echo in the Turbulent Corona and Simulations of Solar Drift-Pair Radio Bursts

Kuznetsov,

Chrysaphi,

Kontar

et al. 2020

Preprint

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Drift-pair bursts are an unusual type of solar low-frequency radio emission, which appear in the dynamic spectra as two parallel drifting bright stripes separated in time. Recent imaging spectroscopy observations allowed for the quantitative characterization of the drifting pairs in terms of source size, position, and evolution. Here, the drift-pair parameters are qualitatively analyzed and compared with the newly-developed Monte Carlo ray-tracing technique simulating radio-wave propagation in the inhomogeneous anisotropic turbulent solar corona. The results suggest that the drift-pair bursts can be formed due to a combination of the refraction and scattering processes, with the trailing component being the result of turbulent reflection (turbulent radio echo). The formation of drift-pair bursts requires an anisotropic scattering with the level of plasma density fluctuations comparable to that in type III bursts, but with a stronger anisotropy at the inner turbulence scale. The anisotropic radio-wave scattering model can quantitatively reproduce the key properties of drift-pair bursts: the apparent source size and its increase with time at a given frequency, the parallel motion of the source centroid positions, and the delay between the burst components. The trailing component is found to be virtually co-spatial and following the main component. The simulations suggest that the drift-pair bursts are likely to be observed closer to the disk center and below 100 MHz due to the effects of free-free absorption and scattering. The exciter of drift-pairs is consistent with propagating packets of whistlers, allowing for a fascinating way to diagnose the plasma turbulence and the radio emission mechanism.

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“…The development of the Fast GS Codes enabled a break-through in massive 3D modeling of the microwave emission from solar (e.g., Fleishman et al 2016Fleishman et al , 2017Gordovskyy et al 2017;Kuroda et al 2018;Fleishman et al 2018;Gordovskyy et al 2019;Motorina et al 2020;Fleishman et al 2021b) and stellar (Waterfall et al 2019(Waterfall et al , 2020 flares. Most of these studies employed a dedicated modeling tool, GX Simulator (Nita et al 2015(Nita et al , 2018, designed specifically to simulate emissions from solar flares and active regions (Fleishman et al 2021a).…”

Section: Introductionmentioning

confidence: 99%

Ultimate Fast Gyrosynchrotron Codes

Kuznetsov,

Fleishman

2021

Preprint

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The past decade has seen a dramatic increase of practical applications of the microwave gyrosynchrotron emission for plasma diagnostics and three-dimensional modeling of solar flares and other astrophysical objects. This break-through turned out to become possible due to apparently minor, technical development of Fast Gyrosynchrotron Codes, which enormously reduced the computation time needed to calculate a single spectrum, while preserving accuracy of the computation. However, the available fast codes are limited in that they could only be used for a factorized distribution over the energy and pitch-angle, while the distributions of electrons over energy or pitch-angle are limited to a number of pre-defined analytical functions. In realistic simulations, these assumptions do not hold; thus, the codes free from the mentioned limitations are called for. To remedy this situation, we extended our fast codes to work with an arbitrary input distribution function of radiating electrons. We accomplished this by implementing fast codes for a distribution function described by an arbitrary numerically-defined array. In addition, we removed several other limitations of the available fast codes and improved treatment of the free-free component. The Ultimate Fast Codes presented here allow for an arbitrary combination of the analytically and numerically defined distributions, which offers the most flexible use of the fast codes. We illustrate the code with a few simple examples.

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Spatiotemporal Energy Partitioning in a Nonthermally Dominated Two-loop Solar Flare

Cited by 18 publications

References 76 publications

Energy partition in a confined flare with an extreme-ultraviolet late phase

Energy partition in a confined flare with an extreme-ultraviolet late phase

Radio Echo in the Turbulent Corona and Simulations of Solar Drift-Pair Radio Bursts

Ultimate Fast Gyrosynchrotron Codes

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