constraints on particle acceleration from interplanetary observations r. p. lin together with l....
Post on 21-Dec-2015
214 views
TRANSCRIPT
![Page 1: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/1.jpg)
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
![Page 2: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/2.jpg)
Krucker and Lin 2002
![Page 3: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/3.jpg)
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)
![Page 4: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/4.jpg)
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
![Page 5: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/5.jpg)
![Page 6: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/6.jpg)
![Page 7: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/7.jpg)
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
![Page 8: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/8.jpg)
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
![Page 9: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/9.jpg)
Wang, Krucker, Lin, & Gosling, 2005
![Page 10: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/10.jpg)
Wang, Krucker, Lin, & Gosling 2005
![Page 11: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/11.jpg)
Wang, Krucker, Lin, & Gosling 2005
![Page 12: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/12.jpg)
Wang, Krucker, Lin, & Gosling 2005
![Page 13: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/13.jpg)
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
![Page 14: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/14.jpg)
![Page 15: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/15.jpg)
![Page 16: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/16.jpg)
X-Class Flare of 2002 July 23
• 00:27:20–00:43:20 UT• GOES X4.8• Location: S13E72
(Lin et al. 2003)
![Page 17: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/17.jpg)
![Page 18: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/18.jpg)
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)
![Page 19: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/19.jpg)
Mewaldt et al 2005
![Page 20: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/20.jpg)
(Mewaldt et al. 2005)
![Page 21: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/21.jpg)
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
![Page 22: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/22.jpg)
Murphy 2004
![Page 23: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/23.jpg)
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)
![Page 24: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/24.jpg)
![Page 25: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/25.jpg)
GOES soft X-rays
RHESSI 2.2 MeV line
RHESSI 100-200 keV
RHESSI hard X-rays
WIND/WAVES radio
WIND/3DP electrons
![Page 26: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/26.jpg)
20 Jan 05 FlareRHESSI Gamma-ray Spectrum - 20 Jan 05 Flare
![Page 27: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/27.jpg)
![Page 28: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/28.jpg)
In the Jan 20 Event the high energy particle-intensities reach Earth just minutes after the x-rays from the flare
![Page 29: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/29.jpg)
RHESSI X-ray imaging during HXR peak:
X-ray imaging
Two ribbon flare with HXR footpoints (contours) with thermal loop (image)
![Page 30: Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,](https://reader030.vdocuments.us/reader030/viewer/2022032522/56649d6a5503460f94a4842e/html5/thumbnails/30.jpg)
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