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

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

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

Type II burst and shockType II bursts link the Remote-sensed and in situData on CME-driven shocks

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

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)

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

CME1CME2

CORE1

20:42

21:18

InteractionSignature

2657 km/s700 km/s

1000 km/s

CME2

CME1

CORE1CME Interaction

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

Mission Requirements

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