1. Use of the Frequency Agile Solar Radiotelescope for Space Weather A New Solar-dedicated Radio Facility Dale E. Gary, NJIT; Stephen M. White, U Maryland

2. Outline of Talk What is FASR? Space Weather Radiophysics Timeline Conclusions What is FASR? Space Weather Radiophysics Timeline Conclusions

3. What is FASR? Frequency-Agile Imaging Array Of order 100 antennas (5000 baselines) Better than 1 imaging at 1 s time resolution Full frequency coverage 0.1-30 GHz Designed Specifically for Solar Imaging Full Sun (to at least 12 GHz) Designed for solar spatial scales Designed for solar brightness variability Frequency-Agile Imaging Array Of order 100 antennas (5000 baselines) Better than 1 imaging at 1 s time resolution Full frequency coverage 0.1-30 GHz Designed Specifically for Solar Imaging Full Sun (to at least 12 GHz) Designed for solar spatial scales Designed for solar brightness variability Isaac Gary

4. FASR Flyover Movie Isaac Gary

5. Outline of Talk What is FASR? Space Weather Radiophysics Timeline Conclusions What is FASR? Space Weather Radiophysics Timeline Conclusions

6. Space Weather Radiophysics 3D View of Solar Atmosphere Coronal Magnetic Fields Synoptic Data CMEs on the Disk Eruptive Prominences Particle Acceleration 3D View of Solar Atmosphere Coronal Magnetic Fields Synoptic Data CMEs on the Disk Eruptive Prominences Particle Acceleration

7. 3D View of Solar Atmosphere S. White

8. Space Weather Radiophysics 3D View of Solar Atmosphere Coronal Magnetic Fields Synoptic Data CMEs on the Disk Eruptive Prominences Particle Acceleration 3D View of Solar Atmosphere Coronal Magnetic Fields Synoptic Data CMEs on the Disk Eruptive Prominences Particle Acceleration

9. Coronal Magnetic Fields J. Lee

10. Lee & White

11. Coronal Magnetograms S. White

12. Space Weather Radiophysics 3D View of Solar Atmosphere Coronal Magnetic Fields Synoptic Data CMEs on the Disk Eruptive Prominences Particle Acceleration 3D View of Solar Atmosphere Coronal Magnetic Fields Synoptic Data CMEs on the Disk Eruptive Prominences Particle Acceleration

13. Nobeyama 17 GHz synoptic map Synoptic Data From K Shibasaki 1998

14. Space Weather Radiophysics 3D View of Solar Atmosphere Coronal Magnetic Fields Synoptic Data CMEs on the Disk Eruptive Prominences Particle Acceleration 3D View of Solar Atmosphere Coronal Magnetic Fields Synoptic Data CMEs on the Disk Eruptive Prominences Particle Acceleration

15. Coronal Mass Ejections from Bastian et al. 2002

16. CME Visibility in Radio Best frequency to see thermal emission should be around 1 GHz or less. Need very good imaging to see relatively low contrast Multi-frequency gives physical parameters. Best frequency to see thermal emission should be around 1 GHz or less. Need very good imaging to see relatively low contrast Multi-frequency gives physical parameters. from Bastian & Gary 1997

17. Observed CME Spectrum from Bastian et al. 2002

18. Space Weather Radiophysics 3D View of Solar Atmosphere Coronal Magnetic Fields Synoptic Data CMEs on the Disk Eruptive Prominences Particle Acceleration 3D View of Solar Atmosphere Coronal Magnetic Fields Synoptic Data CMEs on the Disk Eruptive Prominences Particle Acceleration

19. Erupting Prominences Gopalswamy et al. 1998

20. Space Weather Radiophysics 3D View of Solar Atmosphere Coronal Magnetic Fields Synoptic Data CMEs on the Disk Eruptive Prominences Particle Acceleration 3D View of Solar Atmosphere Coronal Magnetic Fields Synoptic Data CMEs on the Disk Eruptive Prominences Particle Acceleration

21. from Aschwanden et al. 1996

22. from Aschwanden et al. 1992 Type U bursts observed by Phoenix/ETH and the VLA. Particle Trajectories

23. Outline of Talk What is FASR? Space Weather Radiophysics Timeline Conclusions What is FASR? Space Weather Radiophysics Timeline Conclusions

24. Timeline For FASR 2002-3: Design Study (NSF/ATI) International Science Definition Workshop (May 23-25, 2002) Configuration studies; Software architecture Design options; Costing (Current estimate $30 M) 2004-5: Design and Development Prototype Major Elements Prototype Array (< 10 elements) Refine Hardware and Software Design 2005-8: Construction 2002-3: Design Study (NSF/ATI) International Science Definition Workshop (May 23-25, 2002) Configuration studies; Software architecture Design options; Costing (Current estimate $30 M) 2004-5: Design and Development Prototype Major Elements Prototype Array (< 10 elements) Refine Hardware and Software Design 2005-8: Construction

25. Outline of Talk What is FASR? Space Weather Radiophysics Timeline Conclusions What is FASR? Space Weather Radiophysics Timeline Conclusions

26. FASR… is a solar-dedicated radio array designed specifically for the Sun will obtain high-resolution images at hundreds of frequencies, 0.1-30 GHz will measure coronal magnetic fields and make coronal magnetograms will image CMEs and provide physical parameters (T, B, n e ) FASR… is a solar-dedicated radio array designed specifically for the Sun will obtain high-resolution images at hundreds of frequencies, 0.1-30 GHz will measure coronal magnetic fields and make coronal magnetograms will image CMEs and provide physical parameters (T, B, n e )

27. Conclusions FASR… will image thermal and nonthermal emission simultaneously will study particle acceleration will open a new era of study of the Sun and make new discoveries we cannot predict FASR… will image thermal and nonthermal emission simultaneously will study particle acceleration will open a new era of study of the Sun and make new discoveries we cannot predict

28. FASR and Space Weather Standard observing mode Daily data products Coronal magnetograms Coronal temperature maps CME movies (?) Type II, Type III movies Input from Space Weather Community What data products are most useful What operational modes are needed What are we missing? Standard observing mode Daily data products Coronal magnetograms Coronal temperature maps CME movies (?) Type II, Type III movies Input from Space Weather Community What data products are most useful What operational modes are needed What are we missing?

30. Principal Institutions and People Principal Institutions and People NJITD. E. Gary, P. Goode, J. Lee NRAOT. S. Bastian, J. Webber UMdS. M. White, A. Harris BerkeleyG. J. Hurford LucentL. J. Lanzerotti NSOC. Keller NJITD. E. Gary, P. Goode, J. Lee NRAOT. S. Bastian, J. Webber UMdS. M. White, A. Harris BerkeleyG. J. Hurford LucentL. J. Lanzerotti NSOC. Keller

31. Nonthermal CME Parameters from Bastian & Gary 1997