Exploitation of Space Data for Innovative Helio- and Asteroseismology
Helioseismology
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TrackingThe small regions of the Sun useful for helioseismology are generally observed for some period of time and it is necessary to track the same region as it crosses the Sun.The Sun rotates with an average synodic period of 27.8 days, but this varies from the equator to the poles. Each tracking method is determined by the latitude of the region of analysis. Two are listed here: Differential rotation rate: specified.Tracks at the rotation rate of the specified latitude (lambda), given by the formula omega (lambda ) = a0 + a2 sin2(lambda ) + a4 sin4(lambda ). The coefficients of the rotation minus Carrington rotation (micro rad/sec) used for most of the tracking done on the SOHO-MDI data here are, a0 = -0.02893, a2 = -0.3441, a4 = -0.5037, corresponding to the Mt Wilson 1982/84 differential rotation rate.Turning off the tracking requires setting a0 to 2.6662239 micro rad/sec. Lagrangian rotation rate: This tracks at the differential rotation appropriate to the instantaneous latitude for each point in the region, rather than at a common rate for the whole region. This can take considerable computation time depending on the area of observation. More information on solar rotation.
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