000004550 001__ 4550
000004550 005__ 20200115153128.0
000004550 037__ $$aCTALK-2020-0028
000004550 100__ $$aRyan, Aoife
000004550 245__ $$aImaging the Solar Corona during the 2015 March 20 Eclipse using LOFAR 
000004550 260__ $$c2019
000004550 269__ $$c2019-07-08
000004550 520__ $$aThe  solar  corona  is  a  highly-structured  plasma  which  reaches  temperatures  of  more  than ~2MK.  At  low  radio  frequencies  (≤  400  MHz),  scattering  and  refraction  of  electromagnetic waves are thought to broaden sources to several arcminutes. However, exactly how source size relates to scattering due to turbulence is still subject to investigation. This is mainly due to the lack of high spatial resolution observations of the solar corona at low frequencies. Here, we use the LOw Frequency ARray (LOFAR) to observe the solar corona at 120-180 MHz using baselines of up to ~3.5 km (~1--2’) during a partial solar eclipse of 2015 March 20. We use a lunar  de-occultation  technique  to  achieve  higher  spatial  resolution  than  that  attainable  via traditional  interferometric  imaging.  This  provides  a  means  of  studying  source  sizes  in  the corona that are smaller than the angular width of the interferometric point spread function.
000004550 594__ $$aNO
000004550 700__ $$aGallagher, Peter
000004550 700__ $$aCarley, Eoin
000004550 700__ $$aMorosan, Diana 
000004550 700__ $$aBrentjens, Michiel  
000004550 700__ $$aZucca, Pietro 
000004550 700__ $$aFallows, Richard
000004550 700__ $$aVocks, Vocks 
000004550 700__ $$aMann, Gottfried
000004550 700__ $$aBreitling, Frank
000004550 700__ $$aMagdalenic, Jasmina
000004550 700__ $$aKerdraon, Alain
000004550 700__ $$aReid, Hamish  
000004550 773__ $$tCESRA 2019, Potsdam
000004550 8560_ $$fimmanuel.jebaraj@observatoire.be
000004550 906__ $$aContributed
000004550 980__ $$aCTALKCONT