Temporal variations of solar rotation rate at high latitudes

Details Temporal variations of solar rotation rate at high latitudes Temporal variations of solar rotation rate at high latitudes

2001-08-14

arxiv.org/abs/astro-ph/0108226v1

Astronomy and Astrophysics

Astrophysics

To appear in ApJ Letters

Scientific paper

10.1086/323701

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

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