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REPORT Status of Solar Observations with LOFAR

REPORT Status of Solar Observations with LOFAR. Gottfried Mann, Christian Vocks & Frank Breitling Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany e-mail: GMann@aip.de. LOFAR: LOw Frequency ARray 30 – 240 MHz LBA: 30 – 80 MHz HBA: 120 – 240 MHz

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REPORT Status of Solar Observations with LOFAR

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  1. REPORT Status of Solar Observations with LOFAR Gottfried Mann, Christian Vocks & Frank Breitling Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany e-mail: GMann@aip.de LOFAR: LOw Frequency ARray • 30 – 240 MHz • LBA: 30 – 80 MHz • HBA: 120 – 240 MHz • 18 core stations in NL • 18 remote stations in NL • 5 remote stations in D (one in Potsdam-Bornim)

  2. GLOW Exloo Potsdam Tautenburg Jülich Effelsberg Garching German Long Wavelength Consortium • Astronomisches Institut der Ruhr-Universität Bochum • Argelander-Institut für Astronomie Bonn • Max-Planck-Institut für Radioastronomie Bonn • Jacobs University Bremen • Max-Planck-Institut für Astrophysik Garching • Sternwarte Hamburg • Forschungszentrum Jülich • 1. Physikalisches Institut der Universität Köln • Astrophysikalisches Institut Potsdam • Thüringische Landessternwarte Tautenburg

  3. LOFAR Station in Potsdam-Bornim I Bornim AIP Potsdam

  4. LOFAR Station in Potsdam-Bornim II start: August 2009

  5. LOFAR Station in Potsdam-Bornim III container placement

  6. LOFAR Station in Potsdam-Bornim IV LBA field

  7. LOFAR Station in Potsdam-Bornim V installation of electronics

  8. First Light

  9. LOFAR Station in Potsdam-Bornim VI HBA field start: April 2010

  10. LOFAR Station in Potsdam-Bornim VII final state

  11. Solar Observations with LOFAR I in the HBA range at ASTRON

  12. Solar Observations with LOFAR II in the LBA range at Tautenburg (Germany)

  13. Key Science ProjectSolar Physics and Space Weather with LOFAR 30 participants from 10 countries 1st workshop Oct. 5/6, 2006 2nd workshop June 24/25, 2009 3rd workshop July 5/6, 2010 4th workshop (?) Nov. 8/9, 2010

  14. Management Structure

  15. Solar Observations with LOFAR Due to density fluctuations in the corona, the spatial resolution is reduced to few 10”. index of refraction fundamental emission LOFAR’s core stations and first ring of remote stations are sufficient for solar observations.

  16. Solar KSP commissioning phase:  dynamic radio spectra  spectra of the quiet Sun  centre to limb variation  imaging of the quiet Sun We intend to perform these measurements in the months June-August because of the high elevation of the Sun in this period. operational phase: monitoring mode  burst mode  spectrometer mode (single station mode) special observations scheduled on June 9 within the field of view: - Sun (station beam) - strong radio sources 3C132, 3C133, 3C136.1 start: 08:30 UT duration: 6 hours (switching between LBA and HBA every 30 minutes) base lines: up to 30 km LBA-range: 30 – 78 MHz (248 sub bands) HBA-range: 130 – 178 MHz (248 sub bands) These measurements proposed for the commissioning phase will let us learn, how LOFAR really works concerning solar observations.

  17. Issues to be discussed 1. What are the observing modes, which we would like to have for the solar KSP ? 2. Which observing time can we expect? 3. In which way we should employ any single station for the solar KSP ? 4. What are the scientific goals for the KSP ? 5. What will be the off-line data reduction routines to be used for data analysis? 6. Can the LOFAR data formats be accommodated by existing tools or do we need conversions? 7. Are we planning 'busy weeks' for the solar KSP? 8. Who is going to contribute what ? 9. How do we acquire financial supports for our solar KSP ? 10.How do we treat the space weather part of our KSP ?

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