Temporal Variations of the Solar Rotation Rate at High Latitudes | Zendy

H. M. Antia | Zendy; Sarbani Basu | Zendy

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Temporal Variations of the Solar Rotation Rate at High Latitudes

Author(s) -

H. M. Antia,

Sarbani Basu

Publication year - 2001

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/323701

Subject(s) - latitude , equator , physics , dynamo , rotation (mathematics) , oscillation (cell signaling) , solar rotation , polar , atmospheric sciences , dynamo theory , astrophysics , solar physics , astronomy , magnetic field , geometry , mathematics , quantum mechanics , biology , genetics

Frequency splitting coefficients from Global Oscillation Network Group (GONG)and Michelson Doppler Imager (MDI) observations covering the period 1995--2001are used to study temporal variations in the solar rotation rate at highlatitudes. The torsional oscillation pattern in the Sun is known to penetrateto a depth of about $0.1R_\odot$ with alternate bands of faster and slowerrotating plasma. At lower latitudes the bands move towards equator with time.At higher latitudes, however, the bands appear to move towards the poles. Thisis similar to the observed pole-ward movement of large scale magnetic fields athigh latitudes. This also supports theoretical results of pole-ward movingbands at high latitudes in some mean field dynamo models. The polar rotationrate is found to decrease between 1995 and 1999 after which it has startedincreasing.Comment: To appear in ApJ Letter

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