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dc.contributor.authorOberoi, D.
dc.contributor.authorSharma, R.
dc.contributor.authorBhatnagar, S.
dc.contributor.authorLonsdale, C.
dc.contributor.authorMatthews, L.
dc.contributor.authorCairns, I.
dc.contributor.authorTingay, Steven
dc.contributor.authorBenkevitch, L.
dc.contributor.authorDonea, A.
dc.contributor.authorWhite, S.
dc.contributor.authorBernardi, G.
dc.contributor.authorBowman, J.
dc.contributor.authorBriggs, F.
dc.contributor.authorCappallo, R.
dc.contributor.authorCorey, B.
dc.contributor.authorDeshpande, A.
dc.contributor.authorEmrich, D.
dc.contributor.authorGaensler, B.
dc.contributor.authorGoeke, R.
dc.contributor.authorGreenhill, L.
dc.contributor.authorHazelton, B.
dc.contributor.authorJohnston-Hollitt, M.
dc.contributor.authorKaplan, D.
dc.contributor.authorKasper, J.
dc.contributor.authorKratzenberg, E.
dc.contributor.authorLynch, Mervyn
dc.contributor.authorMcWhirter, S.
dc.contributor.authorMitchell, D.
dc.contributor.authorMorales, M.
dc.contributor.authorMorgan, E.
dc.contributor.authorOffringa, A.
dc.contributor.authorOrd, Stephen
dc.contributor.authorPrabu, T.
dc.contributor.authorRogers, A.
dc.contributor.authorRoshi, A.
dc.contributor.authorSalah, J.
dc.contributor.authorShankar, N.
dc.contributor.authorSrivani, K.
dc.contributor.authorSubrahmanyan, R.
dc.contributor.authorWaterson, M.
dc.contributor.authorWayth, Randall
dc.contributor.authorWebster, R.
dc.contributor.authorWhitney, A.
dc.contributor.authorWilliam, A.
dc.contributor.authorWilliams, C.
dc.identifier.citationOberoi, D. and Sharma, R. and Bhatnagar, S. and Lonsdale, C. and Matthews, L. and Cairns, I. and Tingay, S. et al. 2014. Observing the Sun with the Murchison Widefield Array, Proceedings of the 31th URSI General Assembly and Scientific Symposium (URSI GASS), Aug 16-23 2014, pp. 1-4. Bejing: IEEE.

The Sun has remained a difficult source to image for radio telescopes, especially at the low radio frequencies. Its morphologically complex emission features span a large range of angular scales and the emission mechanisms involved, span a wide range in brightness temperatures. In addition, time and frequency synthesis, the key tool used by most radio interferometers to build up information about the source being imaged is not effective for solar imaging, because many of the features of interest are short lived and change dramatically over small fractional bandwidths. Building on the advances in radio frequency technology, digital signal processing and computing, the kind of instruments needed to simultaneously capture the evolution of solar emission in time, frequency, morphology and polarization over a large spectral span with the requisite imaging fidelity, and time and frequency resolution have only recently begun to appear. Of this class of instruments, the Murchison Widefield Array (MWA) is best suited for solar observations. The MWA has now entered a routine observing phase and here we present some early examples from MWA observations.

dc.publisherInstitute of Electrical and Electronics Engineers Inc.
dc.titleObserving the Sun with the Murchison Widefield Array
dc.typeConference Paper
dcterms.source.title2014 31th URSI General Assembly and Scientific Symposium, URSI GASS 2014
curtin.departmentCurtin Institute of Radio Astronomy (Physics)
curtin.accessStatusFulltext not available

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