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Solar Radio Imaging Array SIRA: Investigating Interplanetary Disturbances

Explore the use of Solar Radio Imaging Array (SIRA) for mapping geoeffective solar disturbances from 2 Rs to 1 AU. This innovative interferometry system covers a wide frequency range of 30 KHz to 15 MHz for detailed imaging of large-scale structures in the sun's corona and interplanetary space. By deploying microsats in a constellation, SIRA aims to capture Type II bursts associated with coronal mass ejections (CMEs) and their propagation through the interplanetary medium. Collaborating with NASA-GSFC, this research project plans to study the interaction of CMEs at various distances from the sun, enhancing our understanding of solar dynamics and space weather phenomena. Relevant

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Solar Radio Imaging Array SIRA: Investigating Interplanetary Disturbances

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  1. Solar Radio Imaging ArraySIRA Interferometry 30 KHz - 15 MHz : need to go to space Microsat (16) Constellation Imaging Geoeffective Solar Disturbances from 2 Rs to 1 AU Large-scale structures

  2. coronal Interplanetary Radio Sky 20 214 Rs 2.5 1.5 Gap filled by Wind/WAVES But no imaging Type II, Type III bursts Type III storms are observed in the IP medium less complex Nelson & Labrum, (1985)

  3. An IP Type II & its CME 3.98 15.58 22.21 2.86 Rs f =0 .85MHz fp = 0.425 MHz n = 2.2x103 cm-3 when the CME is at 30 Rs Vcme ~ 770 km/s Type II bursts track CMEs through the IP medium SIRA will produce images like this at lower f

  4. Type II burst and shock Type II bursts link the Remote-sensed and in situ Data on CME-driven shocks

  5. DH Type II (no m) Type II in variousWavelength Ranges Metric Type II m-km Type II A continuum of properties decided by CME energy and VA of the ambient medium m DH km km type II DH Type II

  6. CME Leading Edge at Type II Onset Type II behind CME leading edge Type II & CME in different directions Incompatibility between IP and metric Can be accounted for if we acceleration Initially occurs in the Qperp region and later (IP) in the Q|| region (Holman & Pesses,1983)

  7. Another Effect of the Medium:Radio Enhancement due to Interacting CMEs Also observed by Ulysses and CASSINI ( 5& 9 AU) Direction finding consistent with LASCO position that the interaction occurs at ~20 Rs Gopalswamy et al. 2001;2002

  8. CME Interaction CORE1 20:42 21:18 CORE1 Interaction Signature CME2 CME1 CME2 CME1 1000 km/s 2657 km/s 700 km/s

  9. 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) II WAVES II III III Data: R, MacDowall II Cassini data confirms that the interaction signature is very strong III 11/04

  10. Mission Requirements • ..\SIRA\SIRA Home Page at NASA-GSFC.htm

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