1. Joe Khan Lyndsay Fletcher, Eduard Kontar, Alec MacKinnon, Graham Woan Solar Physics and Space Weather Science with LOFAR: The UK Perspective

2. Outline Interested LOFAR-UK institutes Possible solar observing modes to consider Solar science topics Solar uses for UK stand-alone stations UK Funding for solar science Conclusions

3. LOFAR-UK Institutes interested in 'Solar' Physics with LOFAR 1) Aberystwyth University 2) University of Glasgow 3) University College London (UCL)‏ 4) University of Manchester 5) Rutherford Appleton Laboratory (RAL)‏ 6)University of Southampton 6 LOFAR-UK institutes explicitly interested in  solar physics  heliospheric (solar-terrestrial) physics  magnetospheric physics  ionospheric physics

4. Relevant UK interest and expertise Radio -- a very sensitive diagnostics of solar particles -- useful tool for studying a variety of solar coronal phenomena UK already has solar physics expertise in: –Space-based solar physics observations –Theoretical solar physics & Plasma physics → LOFAR complements these LOFAR: major advantage  rapid, multi-frequency radio imaging of solar radio bursts LOFAR  Square Kilometre Array (SKA)‏ - already acknowledged by STFC as a key element of its roadmap Experienced Interplanetary Scintillation community Experienced ionospheric scientists

5. Some possible observing modes for 'Solar' Physics studies with LOFAR Responsive burst trigger observations: spectrographic observations → short-duration (10-20 min) solar imaging observations Co-ordinated observing campaigns over interval of a day (or days): both spectrographs & imaging Daily synoptic (non-responsive) spectrographic observations Regular synoptic solar imaging observations → multi-frequency images every 'N' minutes Interplanetary scintillation observations of, e.g., solar wind, shock waves, coronal mass ejections Solar radar studies, e.g., with LOIS(?)‏ Solar C with LOFAR – some possible observing modes:

6. Envisage two possible uses for solar spectrographic observations: (a) Solar radio burst 'monitoring'/archiving  Data from beam former  time-domain sampled  highest quality spectrograms (in principle, no need to obtain rapidly)‏  Useful for solar studies 'after the fact'  Also useful for non-solar observers, e.g., check for suspected solar side-lobes (b) Solar radio burst trigger  Data from beam former  processed rapidly  quick spectrograms  detection of bursts  solar burst ‘flagged’  ‘imaging’ (by Dutch core, intl stations, etc.)‏ Solar Spectrographic Obs

7. Solar Science: Solar Flare Physics with LOFAR LOFA R 10MHz 1.5R Sun 0.15R Sun 20-30kHz 240MHz upward beams Hard X- rays Interplanetary type III bursts DecametricType III bursts Earth's orbit Acceleration site 1AU Q. Where is the flare particle accelerator and how do the particles propagate in the corona? Decametric ‘Type III’ bursts generated by beams from accelerator  Beam propagation can be followed.  Non-linear interaction of beam & backgrd plasma can be studied.

8. Coronal mass ejectionAR/coronal heating? Frequency (MHz)‏ Time Height in atmosphere Time 40 200 800 Faint continuumNoise storm Large shock wave Other Solar Physics with LOFAR 110 200 400 300 40 200 800 Type II burst

9. Space Weather: Radio Studies of Coronal Mass Ejections Q: What are the origins, drivers, properties & effects of CMEs? Radio emission due to e-’s trapped in weak-field structures:  electron energy distribution  B field strength/direction (pol n )‏  dynamic evolution of structures Echo Radar mapping of the corona, studies of: - coronal turbulence - coronal dynamics - magnetic field distribution - waves - heating - CMEs Also 'indirect' IPS studies Direct - emissionIndirect – reflected emission

10. Spectrographic observations sensitive diagnostics of solar coronal particles new fine-structures Low resolution ‘imaging’ observations rapid, multi-frequency radio centroiding of CMEs Wide field-of-view IPS studies of solar wind Using LOFAR-UK as a Stand-alone Array X-ray images & radio centroids (old Nancay data) for 3 solar jets LOFAR-UK alone – imaging/centroiding – very limited Centroiding of moving sources could be useful in some solar studies: - source locations, velocities, etc. Best direct solar imaging will be obtained using Dutch core, but... LOFAR-UK as a stand-alone array — useful for solar physics

11. Value of spectrographic data  Identification of type of solar radio burst — crucial in solar studies (diff. bursts - different physical phenomena/processes)‏  Dynamic spectra  needed for understanding of solar radio imaging (e.g., plasma waves?, shock wave? trapped or streaming electrons? mass motions?)‏  Some bursts preferentially occur at low freq.: type II, noise storms  Useful for exploratory studies: Evidence for fine structures – more anticipated Solar Radio Spectroscopy

12. Fibre Bursts Herring- bones U-bursts Noise storm Fine Structures in Solar Spectrograms

13. UK Funding Prospects for 'Solar' Physics with LOFAR Science and Technology Facilities Council –Projects Peer Review Panel (PPRP)‏ Consortium application with element supporting development of solar algorithms relating to analysis of observations –e.g., real-time flare trigger, non real-time burst searches Aberystwyth application for heliospheric (esp. IPS) research –Standard Grant Glasgow application for scientific (solar and heliospheric) research Scottish Universities Physics Alliance (6 universities seeking funding from Scottish Funding Counci)l –Various themes, including an astronomy theme (with LOFAR)‏ Glasgow, Edinburgh, St Andrews application for: –Scottish LOFAR ground station (near Edinburgh)‏ –solar technical support – solar algorithms –solar science research

14. Conclusions Interested LOFAR-UK institutes Possible solar observation modes for discussion Technical issues for solar observations Solar science research LOFAR-UK stand-alone uses for solar science How the UK can contribute to the solar KSP