Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7262
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dc.contributor.authorMugundhan, V-
dc.contributor.authorRamesh, R-
dc.contributor.authorKathiravan, C-
dc.contributor.authorGireesh, G. V. S-
dc.contributor.authorAnshu Kumari-
dc.contributor.authorHariharan, K-
dc.contributor.authorBarve, Indrajit V-
dc.date.accessioned2018-04-11T10:10:23Z-
dc.date.available2018-04-11T10:10:23Z-
dc.date.issued2018-03-01-
dc.identifier.citationThe Astrophysical Journal Letters, Vol. 855, No. 1, L8en_US
dc.identifier.issn2041-8205-
dc.identifier.urihttp://hdl.handle.net/2248/7262-
dc.descriptionRestricted Accessen_US
dc.description.abstractThe angular size of the smallest, compact radio source that can be observed in the solar atmosphere is one of the intriguing questions in low-frequency radio astronomy. This is important to understand density turbulence in the solar corona and the related angular broadening of the radio source sizes. We used a two-element interferometer with a baseline length of ≈200 km, operating at ≈53 MHz to infer the above limit. Our results indicate that radio sources of angular size ≤15'' exist in the solar corona, where radio emission at the above frequency also originates.en_US
dc.language.isoenen_US
dc.publisherIOP Publishingen_US
dc.relation.urihttps://doi.org/10.3847/2041-8213/aaaf64-
dc.rights© The American Astronomical Society-
dc.subjectInstrumentation: high angular resolutionen_US
dc.subjectInstrumentation: interferometersen_US
dc.subjectSun: activityen_US
dc.subjectSun: coronaen_US
dc.subjectSun: flaresen_US
dc.subjectSun: radio radiationen_US
dc.titleThe First Low-frequency Radio Observations of the Solar Corona on ≈200 km Long Interferometer Baselineen_US
dc.typeArticleen_US
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