Solar Observations with LOFAR

Transcription

1 Solar Observations with LOFAR Gottfried Mann, C. Vocks and F. Breitling Astrophysikalisches Institut Potsdam An der Sternwarte 16, D Potsdam, LOFAR: LOw Frequency ARray MHz LBA: MHz HBA: MHz 18 core stations in NL 18 remote stations in NL 5 remote stations in D (one in Potsdam-Bornim)

2 GLOW 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 Exloo Jülich Effelsberg Garching Potsdam Tautenburg

3 LOFAR Station in Potsdam-Bornim I Bornim Potsdam

4 LBA field LOFAR Station in Potsdam-Bornim II

5 final state LOFAR Station in Potsdam-Bornim III

6 in the HBA range at ASTRON Solar Observations with LOFAR I

7 Solar Observations with LOFAR II in the LBA range at Tautenburg ()

8 Solar Radio Emission I radio emission from the solar corona plasma emission R LF pe LF Whistler 0.1 ce R pe ce pe 1.01 pe(n) becouse of pe / ce 10 in the corona index of refraction at the emission site n 1 2 pe for fundamental emission n 0.87 for harmonic emission law of refraction sin sin i r n r arcsin because of total reflection: i 8 for fundamental emission 60 for fundamental emission i sin n i

9 Radio Emission II Due to density fluctuations in the corona, the spatial resolution is reduced to few 10. LOFAR s core stations and first ring of remote stations are sufficient for solar observations.

10 First LOFAR Image of the Sun Radio image of the Sun (left) at 135 MHz as obtained by LOFAR on June 9, An EUV (middle) and soft X-ray image (right) of the Sun as simultaneously provided by the Solar Dynamics Observatory (AIA at 17,1 nm) and Hinode (XRT) is presented for comparison.

11 Comparison with NRH 135 MHz 151 MHz

12 Summary With LOFAR, the processes in the solar corona can be observed with a high spatial and temporal resolution. These processes are of special interest, since they are able to influence our Earth's environment and our technical civilization, which is usually called Space Weather. There, is a Key Science Project "Solar Physics and Space Weather" with LOFAR, which is coordinated by the Astrophysical Institute Potsdam. Thank you for your attention!

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

14 Management Structure Name Affiliation Country PI Prof. Dr. Gottfried Mann core members (project manager) Dr. Alain Kerdraon Dr. Alec McKinnon Prof. Dr. Bo Thide Dr. Christian Vocks Obs. de Paris-Meudon Univ. Glasgow Univ. Uppsala France UK Sweden ordinary members Dr. Henry Aurass Dr. Andy Breen Frank Breitling Dr. Harry Enke Dr. Peter Gallagher Dr. Norbert Jakowski Dr. Matthias Hoeft Dr. Alexander Konovalenko Dr. Eduard Kontar Dr. Christophe Marqué Dr. Jürgen Rendtel Prof. Dr. Helmut Rucker Univ. Aberystwyth Trinity College Dublin DLR Neustrelitz Thür. LSW Tautenburg Institute of Radio Astronomy Univ. Glasgow Royal Obs. of Belgium IWF Graz UK Ireland Ukraine UK Belgium Austria associated memb. Prof. Dr. John Brown Dr. Philippa Browning Prof. Dr. Carsten Denker Dr. Lyndsay Fletcher Dr. Katya Greorgieva Prof. Dr. Arnold Hanslmeier Dr. Roger Karlsson Dr. Karl-Ludwig Klein Dr. Jasmina Magdalenic Dr. Werner Poetzi Prof. Dr. Hanna Rothkaehl Prof. Dr. Joachim Vogt Dr. Alexander Warmuth Univ. Glasgow Univ. Manchester Univ. Glasgow BAS, Sofia Univ. Graz IWF Graz Obs. de Paris-Meudon Royal Obs. of Belgium Sonnenobs. Kanzelhöhe Space Res. Center Warsaw Jacobs Univ. Bremen UK UK UK Bulgaria Austria Austria France Belgium Austria Poland