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
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
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)
Messenger XRS sees flare on disk flare normal
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) 2.6-5.9 kev (XRS) 11: 11:6 11:12 11:18 11:24 11:3 11:36 Start Time (1-Sep-14 1:54:49)
SXR derivative: impulsive phase is before HXR and >1 MeV bursts >1 MeV (LAT) 5 kev (GBM) 3 kev (GBM) 15 kev (GBM) 2.6-5.9 kev (XRS) d/dt 2.6-5.9 kev 11: 11:6 11:12 11:18 11:24 11:3 11:36 Start Time (1-Sep-14 1:54:49)
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)
GOES high emission from impulsive phase! >1 MeV (LAT) 5 kev (GBM) 3 kev (GBM) 15 kev (GBM) 2.6-5.9 GOES high kev (XRS) d/dt 2.6-5.9 kev impulsive phase 11: 11:6 11:12 11:18 11:24 11:3 11:36 Start Time (1-Sep-14 1:54:49)
normalized flux 1..8.6.4.2. 131 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 1-9 1 8 6 4 2 movie 4-8 kev RHESSI thermal emission originates from three different locations: - Western limb AR - Disk AR - Behind the limb event 4 counts s -1 3 2 1 15-3 kev 1 1 8 1 impulsive phase SAA 6 4 2 hhmm 214 Sep 1 11 112
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)
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 ~ 1.8.1.1 2. 1.5 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: 1..5. 1 1 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
Y (arcsecs) Y (arcsecs) Y (arcsecs) Y (arcsecs) Coarse resolution imaging (11:18-11:28UT) 4-6 kev -5 5 1 8.5-12 kev -5 5 1 1 5-5 7-8.5 kev -1 1 6-7 kev -1-5 5 1-1 -5 5 1 25-8 kev 5-5 -1 12-25 kev -1-5 5 1 1 5-5 -1 1 5-1 -5 5 1-5 -1
Y (arcsecs) Y (arcsecs) Y (arcsecs) Y (arcsecs) 7-8.5 kev Coarse resolution imaging (11:11-11:28UT) 4-6 kev -5 5 1 8.5-12 kev -5 5 1 1 5-5 -1 1 6-7 kev -1-5 5 1-1 -5 5 1 25-8 kev 5-5 -1 12-25 kev -1-5 5 1 1 5-5 -1 1-1 -5 5 1 5-5 -1
Y (arcsecs) Y (arcsecs) Y (arcsecs) Y (arcsecs) 7-8.5 kev Coarse resolution imaging (11:11-4-6 kev -5 5 1 1 1 5-5 -1 6-7 kev 5-1 -5 5 1-5 -1 11:28UT) -1-5 5 1 25-8 kev No image above 15 kev despite large number of counts Source significantly larger than s/c 9 resolution of 18 8.5-12 kev -5 5 1 1 1 5-5 -1 12-25 kev -1-5 5 1 5-5 -1-1 -5 5 1
Y (arcsecs) Y (arcsecs) Y (arcsecs) chromospheric source at limb with 8 arcsec FWHM Possibilities for unresolved source 15 1 5-5 -1 15 gaussian above limb with 3 arcsec FWHM -15-15 -1-5 5 1 1 1 5-5 -1-15 -15-1 -5 5 1 15 e.g. accelerated electrons trapped above flare site highly occulted gaussian with 3 arcsec FWHM 15 1 e.g. accelerated electrons trapped behind CME 5-5 -1-15 -15-1 -5 5 1 15 e.g. shockaccelerated electrons getting access to visible part of disk
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).6.4.2.
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
count rate.4.3.2.1. subcollimator 6 & source size of 4 arcsec on-axis 3 arcsec 6 arcsec 9 arcsec 12 arcsec 15 arcsec 18 arcsec 9 18 27 36 roll angle
count rate.4.3.2.1. subcollimator 6 & offset of 11 arcsec source size 4 arcsec 6 arcsec 8 arcsec 1 arcsec 12 arcsec 14 arcsec 9 18 27 36 roll angle
flux.6.4.2. 15 arcsec & 3 arcsec FWHM subcoll 1 subcoll 2 subcoll 3 subcoll 4 subcoll 5 subcoll 6 subcoll 7 subcoll 8 subcoll 9 9 18 27 36 roll angle
counts per second counts per second RHESSI observations (no bkg subtr.) 2-6 kev 1 8 2-6 kev 6 8 4 2 subcoll 6 subcoll 3 subcoll 1..2.4.6.8 1. rotation period 6 4 2 subcoll 9 subcoll 8..2.4.6.8 1. rotation period
count rate Expected profiles (3 cases).4.3.2.1. subcollimator 6 ondisk (6" offset); size=4 arcsec at limb; size=4 arcsec 5 arcsec above limb; size=1 arcsec 9 18 27 36 roll angle
count rate Expected profiles (3 cases).4.3.2.1. 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 9 18 27 36 roll angle
MARS: GRS 22 Oct 27 flare Earth MARS EARTH RHESSI 15-25 kev giant flare seen by GRS (MARS) same onset as emission seen by RHESSI! Krucker, White, & Lin 27
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