Post on 21-Dec-2015
Constraints on Particle Acceleration from Interplanetary
Observations
R. P. Lin together with L. Wang, S. Krucker at
UC Berkeley, G Mason at U. Maryland, and R. Mewaldt at Caltech
Krucker and Lin 2002
Electron -3He-rich SEP events
- ~1000s/year at solar maximum
- dominated by: - electrons of ~0.1 (!) to ~100 keV energy
- 3He ~10s keV/nuc to ~MeV/nucx10-x104 (!) enhancements
- heavy nuclei: Fe, Mg, Si, S enhancements- high charge states
- associated with:
- small flares/coronal microflares - Type III radio bursts - Impulsive soft X-ray bursts (so also called
Impulsive SEP events)
L=v(t-to) or L/v=t-to ~0.05 MeV/nuc -1/v of 3He (Mason & Mazur)
~1.5 MeV/nuc - 1/v for Electrons /
Electrons 0.14–13 keV
Electrons 20 – 350 keV Ions ~ 0.5 – 1 MeV
Electron spectrum at 1AUTypical electron spectrum can be fitted with broken power law:
Break around: 30-100 keVSteeper at higher energies
Oakley, Krucker, & Lin 2004
Comparing spectraPHOTON SPECTRA:Power law fit to HXR spectra averaged over peak
ELECTRON SPECTRA:Power law fit to peak flux
Assuming power spectra:
THIN: = – 1THICK: = + 1
RESULTS:1) correlation seen2) values are between
Wang, Krucker, Lin, & Gosling, 2005
Wang, Krucker, Lin, & Gosling 2005
Wang, Krucker, Lin, & Gosling 2005
Wang, Krucker, Lin, & Gosling 2005
The Sun is the most energetic particle accelerator in the solar system:
- Ions up to ~ 10s of GeV - Electrons up to ~100s of MeV
Acceleration to these energies occurs in transient energy releases, in two (!) processes:
- Large Solar Flares, in the lower corona
- Fast Coronal Mass Ejections (CMEs), in the inner heliosphere, ~2-40 solar radii
X-Class Flare of 2002 July 23
• 00:27:20–00:43:20 UT• GOES X4.8• Location: S13E72
(Lin et al. 2003)
RHESSI Gamma-Ray Flares2002 July 23 X4.8
2003 June 17 M6.9
2003 October 28 X17
2003 October 29 X10
2003 November 2
X8.3
2003 November 3
X3.9
2004 November 10
X2.5
2005 January 15 X2.6
2005 January 17 X3.8
2005 January 19 X1.3
2005 January 20 X7.1
Ramaty High Energy Solar Spectroscopic Imager (RHESSI)
Mewaldt et al 2005
(Mewaldt et al. 2005)
Oct. 28, 2003, RHESSI solar count spectrum from 11:06:20 – 11:10:04 (Smith et al. 2004, Share et al. 2004)
e+ - e- n-capture
bremsstrahlung
narrow linesbroad lines
Murphy 2004
Energetic Proton Power-law Exponents
28 Oct 03 2 Nov 03
S16E08 S15W56
γ-ray lines Energy range γ-ray (SEP) γ-ray (SEP)
Ne/C+O 2-20 MeV 2.0-3.2 (1.3) 1.6-3.2 (1.7)
e+/C+O 10-50 MeV 2.2-3.3 (2.0) 2.3-3.3 (2.8)
n-capt/C+O 10-100 MeV 2.8-3.8 (2.5) 2.8-3.8 (3.0)
GOES soft X-rays
RHESSI 2.2 MeV line
RHESSI 100-200 keV
RHESSI hard X-rays
WIND/WAVES radio
WIND/3DP electrons
20 Jan 05 FlareRHESSI Gamma-ray Spectrum - 20 Jan 05 Flare
In the Jan 20 Event the high energy particle-intensities reach Earth just minutes after the x-rays from the flare
RHESSI X-ray imaging during HXR peak:
X-ray imaging
Two ribbon flare with HXR footpoints (contours) with thermal loop (image)
TimingRed line (06:48UT):Solar release time derived from onsets at 1 AU assuming first arriving particles travel with the speed of light along L=1.2 AU
LASCO (06:54UT): Around ~3 solar radii; lines show height assuming a constant velocity.For v=2500km/s, CME could be at ~1.5 solar radius at particle release time.
Red crosses:Rising SXR loops (top of SXI emission)
2.2 MeV peaks at 06:47:30UTHXRs peak at 06:45:00UT