Solar Radio Imaging Array SIRA
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Solar Radio Imaging ArraySIRA
Interferometry30 KHz - 15 MHz : need to go to spaceMicrosat (16) ConstellationImaging Geoeffective Solar Disturbances from 2 Rs to 1 AULarge-scale structures
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Radio SkyInterplanetarycoronal
Nelson & Labrum, (1985)
Gap filled by Wind/WAVESBut no imaging
1.5 2.5 20Rs 214
Type II, Type III burstsType III storms are observedin the IP mediumless complex
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An IP Type II & its CME
f =0 .85MHz fp = 0.425 MHz n = 2.2x103 cm-3 when the CME is at 30 RsVcme ~ 770 km/s
Type II bursts track CMEs through the IP medium
2.86 Rs
3.98 15.58 22.21
SIRA will produce images like this at lower f
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Type II burst and shockType II bursts link the Remote-sensed and in situData on CME-driven shocks
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Type II in variousWavelength Ranges
m
DH
km
km type II
Metric Type II
DH Type II
m-km Type II
DH Type II (no m)
A contin
uum of propertie
s decided by C
ME energy and V A
of the ambient m
edium
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CME Leading Edge at Type II Onset
Type II behind CME leading edgeType II & CME in different directionsIncompatibility between IP and metric
Can be accounted for if we acceleration Initially occurs in the Qperp region andlater (IP) in the Q|| region (Holman & Pesses,1983)
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Another Effect of the Medium:Radio Enhancement due to Interacting CMEs
Also observed by Ulyssesand CASSINI ( 5& 9 AU)
Direction finding consistent with LASCO position thatthe interaction occurs at~20 Rs
Gopalswamy et al. 2001;2002
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CME1CME2
CORE1
20:42
21:18
InteractionSignature
2657 km/s700 km/s
1000 km/s
CME2
CME1
CORE1CME Interaction
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Interaction detected by
Wind, Ulysses & Cassini Cassini at 8.7 AU: Radiation has to travel for additional 64 min Data: M. Desch
Wind: 21:10 1 (AU); Uly: 21:50 (5 AU); Cass: 22:18 (8.7 AU)
11/04
WAVES
III
III
III
II
II
II
Data: R, MacDowall
Cassini data confirmsthat the interaction signatureis very strong
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Mission Requirements
• ..\SIRA\SIRA Home Page at NASA-GSFC.htm