Global Energetics of Solar Flares. V. Energy Closure in Flares and Coronal Mass Ejections

Aschwanden, Markus J.; Caspi, Amir; Cohen, C. M. S.; Holman, Gordon D.; Jing, Ju; Kretzschmar, M.; Kontar, Eduard P.; McTiernan, J.; Mewaldt, R. A.; O'Flannagain, Aidan; Richardson, I. G.; Ryan, Daniel; Warren, H. P.; Xu, Yan

doi:10.3847/1538-4357/836/1/17

Cited by 138 publications

(118 citation statements)

References 66 publications

Supporting

Mentioning

106

Contrasting

Order By: Relevance

“…sources with the jet pointing to the line-of-sight, where jet overwhelms the nuclear emission. Interestingly, the statistics of physical quantities related to the Solar X-ray emission and coronal mass ejections (CMEs), understood to be powered by magnetic-reconnection (Aschwanden et al 2017) also exhibit lognormal properties (Zhang 2007;Aoki et al 2003) are consistent with our finding in this work. Moreover, apart from emission and mass ejections, CMEs also lead to energization and generation of non-thermal particles (e.g.…”

Section: Discussionsupporting

confidence: 90%

Gamma-Ray Flux Distribution and Nonlinear Behavior of Four LAT Bright AGNs

Kushwaha

Sinha

Misra

et al. 2017

ApJ

View full text Add to dashboard Cite

We present a statistical characterization of the γ-ray emission from the four Fermi -LAT sources: FR I radio galaxy NGC 1275, BL Lac Mrk 421, FSRQs B2 1520+31 and PKS 1510-089 detected almost continuously over a time integration of 3-days between August 2008 -October 2015. The observed flux variation is large, spanning 2 orders of magnitude between the extremes except for Mrk 421. We compute the flux distributions and compare with Gaussian and lognormal ones. We find that the 3 blazars have distribution consistent with a lognormal, suggesting that the variability is of a non-linear, multiplicative nature. This is further supported by the computation of the flux-rms relation, which is observed to be linear for the 3 blazars. However, for NGC 1275, the distribution does not seem to be represented either by a lognormal or a Gaussian, while its flux-rms relation is still found to be linear. We also compute the power spectra, which suggest the presence of a break, but are consistent with typical scale-free power-law shot noise. The results are broadly consistent with the statistical properties of the magnetic reconnection powered minijets-in-a-jet model. We discuss other possible scenarios and implications of these observations on jet processes and connections with the central engine.

show abstract

Section: Discussionsupporting

confidence: 90%

Gamma-Ray Flux Distribution and Nonlinear Behavior of Four LAT Bright AGNs

Kushwaha

Sinha

Misra

et al. 2017

ApJ

View full text Add to dashboard Cite

show abstract

“…We plan to apply a similar analysis to more energetic simulated eruptions in the future, (such as the one presented in Török et al 2018). We note that MHD simulations cannot capture the contributions of accelerated particles to the energy dissipation and transport, which are important during the impulsive phase of large flares (Emslie et al 2005;Aschwanden et al 2017). Despite this restriction, simulations like the one presented here can provide very useful information on the mechanisms and locations of thermal energy release and transport in solar eruptions.…”

Section: Discussionmentioning

confidence: 96%

Exploring Plasma Heating in the Current Sheet Region in a Three-dimensional Coronal Mass Ejection Simulation

Reeves

Török

Mikić

et al. 2019

ApJ

View full text Add to dashboard Cite

We simulate a coronal mass ejection (CME) using a three-dimensional magnetohydrodynamic (MHD) code that includes coronal heating, thermal conduction, and radiative cooling in the energy equation. The magnetic flux distribution at 1 R s is produced by a localized subsurface dipole superimposed on a global dipole field, mimicking the presence of an active region within the global corona. Transverse electric fields are applied near the polarity inversion line to introduce a transverse magnetic field, followed by the imposition of a converging flow to form and destabilize a flux rope, producing an eruption. We examine the quantities responsible for plasma heating and cooling during the eruption, including thermal conduction, radiation, adiabatic effects, coronal heating, and ohmic heating. We find that ohmic heating is an important contributor to hot temperatures in the current sheet region early in the eruption, but in the late phase adiabatic compression plays an important role in heating the plasma there. Thermal conduction also plays an important role in the transport of thermal energy away from the current sheet region throughout the reconnection process, producing a "thermal halo" and widening the region of high temperatures. We simulate emission from solar telescopes for this eruption and find that there is evidence for emission from heated plasma above the flare loops late in the eruption, when the adiabatic heating is the dominant heating term. These results provide an explanation for hot supra-arcade plasma sheets that are often observed in X-rays and extreme ultraviolet wavelengths during the decay phase of large flares.

show abstract

“…The analyzed data sets include all M and X-class flares during the Solar Dynamics Observatory (SDO) mission (Pesnell et al 2011). In the previous studies we measured the various types of energies that can be detected during flares and CME events, including the dissipated magnetic energy (Aschwanden Xu, and Jing 2014;Paper I), the multi-thermal energy (Aschwanden et al 2015;Paper II), the nonthermal energy Paper III), the kinetic and gravitational energy of associated CMEs (Aschwanden 2016;Paper IV), and the energy closure (Aschwanden et al 2017;Paper V). Regarding CME energetics, there is the traditional white-light scattering method on one side, and the more novel EUV-dimming method on the other side, which both will be extensively discussed in this paper (for references of both methods see Paper IV and references therein).…”

Section: Introductionmentioning

confidence: 99%

Global Energetics of Solar Flares. VI. Refined Energetics of Coronal Mass Ejections

Aschwanden

2017

ApJ

Self Cite

View full text Add to dashboard Cite

In this study we refine a CME model presented in an earlier study on the global energetics of solar flares and associated CMEs, and apply it to all (860) GOES M-and X-class flare events observed during the first 7 years (2010)(2011)(2012)(2013)(2014)(2015)(2016) of the Solar Dynamics Observatory (SDO) mission, which doubles the statistics of the earlier study. The model refinements include: (1) the CME geometry in terms of a 3D sphere undergoing self-similar adiabatic expansion; (2) the inclusion of solar gravitational deceleration during the acceleration and propagation of the CME, which discriminates eruptive and confined CMEs; (4) a self-consistent relationship between the CME center-of-mass motion detected during EUV dimming and the leading-edge motion observed in white-light coronagraphs; (5) the equi-partition of the CME kinetic and thermal energy; and (6) the Rosner-Tucker-Vaiana (RTV) scaling law. The refined CME model is entirely based on EUV dimming observations (using AIA/SDO data) and complements the traditional white-light scattering model (using LASCO/SOHO data), and both models are independently capable to determine fundamental CME parameters such as the CME mass, speed, and energy. Comparing the two methods we find that: (1) LASCO is less sensitive than AIA in detecting CMEs (in 24% of the cases); (2) CME masses below m cme < ∼ 10 14 g are under-estimated by LASCO; (3) AIA and LASCO masses, speeds, and energy agree closely in the statistical mean after elimination of outliers; (4) the CMEs parameters of the speed v, emission measure-weighted flare peak temperature T e , and length scale L are consistent with the following scaling laws (derived from first principles): v ∝ T 1/2 e , v ∝ (m cme ) 1/4 , and m cme ∝ L 2 .

show abstract

Global Energetics of Solar Flares. V. Energy Closure in Flares and Coronal Mass Ejections

Cited by 138 publications

References 66 publications

Gamma-Ray Flux Distribution and Nonlinear Behavior of Four LAT Bright AGNs

Gamma-Ray Flux Distribution and Nonlinear Behavior of Four LAT Bright AGNs

Exploring Plasma Heating in the Current Sheet Region in a Three-dimensional Coronal Mass Ejection Simulation

Global Energetics of Solar Flares. VI. Refined Energetics of Coronal Mass Ejections

Contact Info

Product

Resources

About