Notes

Slide Show

Outline

1	The FASR*/LOFAR^†/SIRA⁺ Connection Dale E. Gary New Jersey Institute of Technology Namir Kassim, NRL N. Gopalswamy, GSFC Markus Aschwanden, Lockheed
2	Suite of Three New Radio Instruments FASR: Spectral imaging from 24 GHz—100 MHz LOFAR: Spectral imaging from 240 MHz—20 MHz SIRA: Spectral imaging from 15 MHz—30 kHz
3	Solar Characteristic Frequencies
4	FASR Frequency Range
5	Radio CME (Nancay)
6	LOFAR and SIRA Range
7	Coronal Scattering
8	"FASR Instrument" FASR Instrument FASR Science Overview Connection With SIRA
9	FASR Science Goals Directly measure magnetic fields Active region corona (150 G < B < 2400 G) Chromospheric network (B_l > 20 G?) Coronal Mass Ejections Image on disk and off limb Image both thermal and nonthermal emission Deduce T, B, nonthermal e^- parameters Radio emission from shocks (type II), electron beams (type III), over heights 1-2.5 R_sun Particle acceleration/Flares Solar atmospheric structure T, B, n_e
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11	Observed CME Spectrum
12	Type II Bursts
13	Type II Bursts
14	Shock Waves/EIT Waves
15	Starting Frequency of Type II Bursts
16	Type III Bursts
17	Particle Trajectories
18	Particle Trajectories
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20	Particle Trajectories
21	Particle Acceleration
22	Putting It All Together FASR Map coronal field strength in active regions Image type III bursts and other emissions to obtain acceleration site and trajectory to 1.5 R_sun Image CMEs, and equivalent of EIT waves. Image some coronal type II bursts
23	Putting It All Together SIRA Image type III bursts to obtain trajectory 2.5 – 200 R_sun Image CMEs or associated disturbances. Image interplanetary type II bursts
24	Key Joint Studies
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29	Operations Plan