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Meridional circulation in the solar convection zone: time-distance helioseismic inferences from four years of HMI/SDO observations

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dc.contributor.author Rajaguru, S. P
dc.contributor.author Antia, H. M
dc.date.accessioned 2020-11-17T14:18:23Z
dc.date.available 2020-11-17T14:18:23Z
dc.date.issued 2015-11-10
dc.identifier.citation The Astrophysical Journal, Vol. 813, No. 2, 114 en_US
dc.identifier.issn 0004-637X
dc.identifier.uri http://prints.iiap.res.in/handle/2248/7137
dc.description Restricted Access © The American Astronomical Society http://dx.doi.org/10.1088/0004-637X/813/2/114 en_US
dc.description.abstract We present and discuss results from time–distance helioseismic measurements of meridional circulation (MC) in the solar convection zone using 4 yr of Doppler velocity observations by the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory. Using a built-in mass conservation constraint in terms of the stream function, we invert helioseismic travel times to infer the MC in the solar convection zone. We find that the return flow that closes the MC is possibly beneath the depth of 0.77 Re. We discuss the significance of this result in relation to other helioseismic inferences published recently and possible reasons for the differences in the results. Our results show clearly the pitfalls involved in the measurements of material flows in the deep solar interior given the current limits on the signal-to-noise ratio and our limited understanding of systematics in the data. We also discuss the implications of our results for the dynamics of solar interior and popular solar dynamo models. en_US
dc.language.iso en en_US
dc.publisher IOP Publishing en_US
dc.subject Sun: helioseismology en_US
dc.subject Sun: interior en_US
dc.subject Sun: oscillations en_US
dc.title Meridional circulation in the solar convection zone: time-distance helioseismic inferences from four years of HMI/SDO observations en_US
dc.type Article en_US


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