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A Ready Method for finding Eccentric Dipole Time

Abstract

ECCENTRIC geomagnetic dipole1 time at an observatory (O) is defined for present purposes as the difference in eccentric dipole longitude (ɛ′) of the Sun (as distinct from the sub-polar point) and the observatory being measured eastwards from the Sun to the observatory, that is: Elsewhere2,3 it has been shown by different approaches that tecc. runs parallel to ordinary geomagnetic time (a centric system) differing by a constant C0, which is a characteristic of the observatory for the particular epoch of the Earth's magnetic field. Thus, also : where ɛ represents geomagnetic longitude. where3: X=−0.0577, Y=0.0320, Z=0.0184 for epoch 1955.0 and (θ0, ɛ0) are geographic co-ordinates of the observatory.

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References

  1. Parkinson, W. D., and Cleary, J., Geophys. J., Roy. Astro. Soc., 1, 346 (1958).

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  2. Simonow, G. V. (to be published).

  3. Cole, K. D., Austral. J. Phys., 16 (in the press).

  4. Brice, N., and Ungstrup, E., Nature, 198, 874 (1963).

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COLE, K., SIMONOW, G. A Ready Method for finding Eccentric Dipole Time. Nature 199, 1279–1280 (1963). https://doi.org/10.1038/1991279a0

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