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?