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Energy Budgets of Flare/CME Events. John Raymond, J.-Y. Li, A. Ciaravella, G. Holman, J. Lin. Jiong Qiu will discuss the Magnetic Field Fundamental, but hard to determine Fragmentary Observations Hard to guess right theory. Lin et al. Energy Partition CME vs Flare - PowerPoint PPT Presentation
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Energy Budgets of Flare/CME Events
John Raymond, J.-Y. Li, A. Ciaravella,G. Holman, J. Lin
Jiong Qiu will discuss the Magnetic Field
Fundamental, but hard to determine
Fragmentary Observations
Hard to guess right theory
Lin et al.
Energy Partition
CME vs Flare
Reconnection vs Lorentz force of expanding field
Asymmetric reconnection; Upwards vs downwards
Partition of flare energy energetic e- energetic p thermal energy kinetic energy
Partition of CME energy
kinetic / gravitational heat SEPs
Energy Partition
CME vs Flare
Reconnection vs Lorentz force of expanding field
Asymmetric reconnection; Upwards vs downwards
Partition of flare energy energetic e- energetic p thermal energy kinetic energy
Partition of CME energy
kinetic / gravitational heat SEPs
Unknown Energy Partition due to rapid conversion
Particles rapidly heat chromosphere.
Heat drives bulk flows.
Shocks heat plasma and accelerate particles.
Turbulence accelerates particles.
Energetic particle beams generate turbulence.
Shiota et al
Energy budgets for 2 large flares
Emslie et al. 2005
21 April 2002 23 July 2002
Magnetic 32.30.3 32.30.3
Flare Electrons 31.30.3 31.50.5 Protons <31.6 31.90.5 Thermal > 5MK 30.80.7 30.10.7
Radiant 32.20.3 32.20.3 (100xGOES)
CME Kinetic 32.30.3 32.00.3 Gravitational 30.70.3 31.10.3 SEPs 31.50.6 <30.0 ?
EFLARE = ECME ?
Yashiro & Goplaswamy IAU 257
Slope > 1
1030.5
What fraction of LFLARE
is in X-rays? 5-20% estimates
Energy conducted to lower T
L = 100 LX from 1 SORCE (Woods et al)
Transition Region Emission
Particles heating chromosphere
Conduction
Evaporation
23 July 2002 (1026 erg/s)
LTR LX dE/dt LNT
00:22 UT 2.7 0.2 38 15600:24 4.0 2.3 72 124000:26 16.0 9.0 228 41500:28 13.8 29.8 161 31800:31 7.4 54.2 49 16100:33 4.1 69.3 -2 178
Raymond et al. 2007
80% Chromosphericor White Light
10% radiated in impulsive phase
CME mechanical energy vs Flare
Acceleration correlated with derivative ofX-ray emission
Reconnection drives both?
CME drives reconnection?
Lorentz force reconnection?
Zhang et al.
Heating of CME Ejecta
n, T and ionization at UVCS
EUV absorption -> emission
Ionization state at 1 AU
Lee et al. 2009
Filippov &Koutchmy
Rakowski et al.
Heat Sources for CME Ejecta
Thermal Conduction
Wave heating as in fast solar wind
Shocks as gas falls from top to bottom of flux rope (Filippov & Koutchmy)
Energetic particles (Simnett?)
Shocks from reconnection outflow (Shiota et al.)
Magnetic dissipation (e.g. Kumar and Rust; Lynch et al MHD models)
Heating in 9 April 08 CME
EIS, XRT, EUVI at 1.1 Rs
Cool gas at 1.3x105 K requires 1016 erg/gor 40 times the mechanical energy.
X-ray gas at 6x106 K is ~ 1/10 as large.
UVCS, COR1 at 1.9 Rs
An additional 4 – 7x1014 erg/g is needed
Thermal conduction doesn’t work for cool gas.
Filippov & Koutchmy shocks don’t have enough energy.
Waves require 1500xCH and line widths are narrow.
Heat ne or Heat d(KE+GE)/dt works – Magnetic heating?
Landi et al., in prep
SEPs vs Kinetic Energy
Estimate solid angleto get total SEPs
Should go to zero for slow CMEs
Mewaldt et al.
EIT Waves
Radiative losses 25% coronal brightening over 0.1 RS ring 1 RS in radius 4x1025 erg/s for 2000 seconds gives 1029 erg modest fraction of flare energy more energy in UV or optical?
Blast Wave? 1028 f R V300
3 erg/s : f ~ 1%
Energy flux from dimming region?
Dimming region wave flux goes into CME 106 erg/cm2 s over 0.5 RS footprint = 4x1027 ergs/s, or 1031 ergs McIntosh sees enhanced line widths
Veronig et al
Questions
Flare vs CME? Roughly equal in big events huge scatter reconnection vs MHD force acceleration vs d/dt of X-ray emission; cause or effect? ~1/2 of flux rope gas passes through CS -> VA ?
Flare energetic particles dominate are they accelerated in current sheet? How? Shocks? even in small events?
CME heating comparable to mechanical energy for all events? SEPs ~ 10% of Kinetic energy do they ever dominate?