RHESSI and AIA observations of the FERMI behind-the-limb flare on 2014 September 1
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1 RHESSI and AIA observations of the FERMI behind-the-limb flare on 214 September 1 Säm Krucker Space Sciences Laboratory, UC Berkeley University of Applied Sciences Northwestern Switzerland Melissa Pesce-Rollins, INFN, Pisa Richard Schwartz, GSFC Pascal Saint-Hilaire, Gordon Hurford, SSL, UCB
2 Outlook Sep 1, 214 behind the limb event (Melissa s talk) Compare time profiles and spectra between FERMI and RHESSI RHESSI source locations compared to >1 MeV centroid location Thermal Non-thermal AIA observations
3 Fermi time profiles >1 MeV (LAT) 5 kev (GBM) 3 kev (GBM) 15 kev (GBM) 2 min 11: 11:6 11:12 11:18 11:24 11:3 11:36 Start Time (1-Sep-14 1:54:49)
4
5 Messenger XRS sees flare on disk flare normal
6 XRS fits gives EM=4x1 49 cm -3 & T=3 MK GOES X1.3 >1 MeV (LAT) 5 kev (GBM) 3 kev (GBM) 15 kev (GBM) kev (XRS) 11: 11:6 11:12 11:18 11:24 11:3 11:36 Start Time (1-Sep-14 1:54:49)
7 SXR derivative: impulsive phase is before HXR and >1 MeV bursts >1 MeV (LAT) 5 kev (GBM) 3 kev (GBM) 15 kev (GBM) kev (XRS) d/dt kev 11: 11:6 11:12 11:18 11:24 11:3 11:36 Start Time (1-Sep-14 1:54:49)
8 GOES high shows initial increase occulted GOES high is 1-4 of total >1 MeV (LAT) 5 kev (GBM) 3 kev (GBM) 15 kev (GBM) GOES high 11: 11:6 11:12 11:18 11:24 11:3 11:36 Start Time (1-Sep-14 1:54:49)
9 GOES high emission from impulsive phase! >1 MeV (LAT) 5 kev (GBM) 3 kev (GBM) 15 kev (GBM) GOES high kev (XRS) d/dt kev impulsive phase 11: 11:6 11:12 11:18 11:24 11:3 11:36 Start Time (1-Sep-14 1:54:49)
10 normalized flux A 15 kev Same onset as 15 kev and GOES high. Escaping hot structure.
![GOES flux [W m -2 ] 1-6 energy [kev] 1-7 RHESSI coverage counts s -1 1-8](/docs-images/88/115404192/images/11-0.jpg "1-9 1 8 6 4 2 movie 4-8 kev RHESSI thermal emission originates from three")
11 GOES flux [W m -2 ] 1-6 energy [kev] 1-7 RHESSI coverage counts s movie 4-8 kev RHESSI thermal emission originates from three different locations: - Western limb AR - Disk AR - Behind the limb event 4 counts s kev impulsive phase SAA hhmm 214 Sep
12 Fermi & RHESSI time profiles >1 MeV (LAT) 5 kev (GBM) 3 kev (GBM) 15 kev (GBM) 4-8 kev (RHESSI) 15-3 kev (RHESSI) SAA 11: 11:6 11:12 11:18 11:24 11:3 11:36 Start Time (1-Sep-14 1:54:49)
13
14 ratio photons s -1 cm -2 kev -1 11:1:56 to 11:13:2 UT GBM and RHESSI HXR spectra GBM: g ~ 2. RHSI: g ~ Power law! High energy (>5 kev) electrons alone cannot reproduce the spectra. ~3 orders of magnitude fainter than largest flares (e.g. Dec 6, 25 with flux of 1 ph/s/cm2/kev at 3 kev) Instantaneous electrons above 2 kev: energy [kev] 1.x1 36 (1 8 /n) electrons. Thick target: 2x1 26 erg/s for electrons above 2 kev. Number of counts above 15 kev is 2 cts/min/det more than enough for imaging
15 Y (arcsecs) Y (arcsecs) Y (arcsecs) Y (arcsecs) Coarse resolution imaging (11:18-11:28UT) 4-6 kev kev kev kev kev kev
16 Y (arcsecs) Y (arcsecs) Y (arcsecs) Y (arcsecs) kev Coarse resolution imaging (11:11-11:28UT) 4-6 kev kev kev kev kev
17 Y (arcsecs) Y (arcsecs) Y (arcsecs) Y (arcsecs) kev Coarse resolution imaging (11: kev kev :28UT) kev No image above 15 kev despite large number of counts Source significantly larger than s/c 9 resolution of kev kev
18 Y (arcsecs) Y (arcsecs) Y (arcsecs) chromospheric source at limb with 8 arcsec FWHM Possibilities for unresolved source gaussian above limb with 3 arcsec FWHM e.g. accelerated electrons trapped above flare site highly occulted gaussian with 3 arcsec FWHM 15 1 e.g. accelerated electrons trapped behind CME e.g. shockaccelerated electrons getting access to visible part of disk
19 normalized flux LASCO CME images 1..8 >1 MeV (LAT) 5 kev (GBM) 3 kev (GBM) 15 kev (GBM) 11: 11:6 11:12 11:18 11:24 11:3 11:36 Start Time (1-Sep-14 1:54:49)
20 first grid second grid off axis source is visible on axis direction 9 o rotated off axis source partially visible or masked on axis direction
21 count rate subcollimator 6 & source size of 4 arcsec on-axis 3 arcsec 6 arcsec 9 arcsec 12 arcsec 15 arcsec 18 arcsec roll angle
22 count rate subcollimator 6 & offset of 11 arcsec source size 4 arcsec 6 arcsec 8 arcsec 1 arcsec 12 arcsec 14 arcsec roll angle
23 flux arcsec & 3 arcsec FWHM subcoll 1 subcoll 2 subcoll 3 subcoll 4 subcoll 5 subcoll 6 subcoll 7 subcoll 8 subcoll roll angle
24 counts per second counts per second RHESSI observations (no bkg subtr.) 2-6 kev kev subcoll 6 subcoll 3 subcoll rotation period subcoll 9 subcoll rotation period
25 count rate Expected profiles (3 cases) subcollimator 6 ondisk (6" offset); size=4 arcsec at limb; size=4 arcsec 5 arcsec above limb; size=1 arcsec roll angle
26 count rate Expected profiles (3 cases) subcollimator 6 observed 2-8 kev, bkg subtracted (11:11-11:13UT) ondisk (6" offset); size=4 arcsec at limb; size=4 arcsec 5 arcsec above limb; size=1 arcsec roll angle
27 MARS: GRS 22 Oct 27 flare Earth MARS EARTH RHESSI kev giant flare seen by GRS (MARS) same onset as emission seen by RHESSI! Krucker, White, & Lin 27
28 size motion HXR emission from electrons in magnetic structures within coronal mass ejections. speed of CME front ~ 2 km/s HXR from CME very large source (>2 arcsec) expanding and rising ~4 km/s 3 ~8 km/s filament ~ 1 km/s Krucker, White, & Lin, ApJL, 27
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