Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7222
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dc.contributor.authorRoy, S-
dc.contributor.authorSur, Sharanya-
dc.contributor.authorSubramanian, K-
dc.contributor.authorMangalam, A-
dc.contributor.authorSeshadri, T. R-
dc.contributor.authorChand, H-
dc.date.accessioned2020-11-19T13:12:30Z-
dc.date.available2020-11-19T13:12:30Z-
dc.date.issued2016-12-
dc.identifier.citationJournal of Astrophysics and Astronomy, Vol. 37, No. 4, 42en_US
dc.identifier.issn0973-7758-
dc.identifier.urihttp://prints.iiap.res.in/handle/2248/7222-
dc.descriptionOpen Access © Indian Academy of Sciences http://www.ias.ac.in/describe/article/joaa/037/04/0042en_US
dc.description.abstractOrigin of magnetic fields, its structure and effects on dynamical processes in stars to galaxies are not well understood. Lack of a direct probe has remained a problem for its study. The first phase of Square Kilometre Array (SKA-I), will have almost an order of magnitude higher sensitivity than the best existing radio telescope at GHz frequencies. In this contribution, we discuss specific science cases that are of interest to the Indian community concerned with astrophysical turbulence and magnetic fields. The SKA-I will allow observations of a large number of background sources with detectable polarization and measure their Faraday depths (FDs) through the Milky Way, other galaxies and their circum-galactic mediums. This will probe line-of-sight magnetic fields in these objects well and provide field configurations. Detailed comparison of observational data (e.g., pitch angles in spirals) with models which consider various processes giving rise to field amplification and maintenance (e.g., various types of dynamo models) will then be possible. Such observations will also provide the coherence scale of the fields and its random component through RM structure function. Measuring the random component is important to characterize turbulence in the medium. Observations of FDs with redshift will provide important information on magnetic field evolution as a function of redshift. The background sources could also be used to probe magnetic fields and its coherent scale in galaxy clusters and in bridges formed between interacting galaxies. Other than FDs, sensitive observations of synchrotron emission from galaxies will provide complimentary information on their magnetic field strengths in the sky plane. The core shift measurements of AGNs can provide more precise measurements of magnetic field in the sub parsec region near the black hole and its evolution. The low band of SKA-I will also be useful to study circularly polarized emission from Sun and comparing various models of field configurations with observations.en_US
dc.language.isoenen_US
dc.publisherIndian Academy of Sciencesen_US
dc.subjectMagnetic fieldsen_US
dc.subjectTelescopesen_US
dc.subjectGalaxies: magnetic fieldsen_US
dc.subjectISM: magnetic fieldsen_US
dc.subjectStars: magnetic fieldsen_US
dc.subjectTurbulenceen_US
dc.titleProbing magnetic fields with square kilometre array and its precursorsen_US
dc.typeArticleen_US
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