Empirical polar cap potentials

Abstract

DMSP satellite plasma flow data from 1987-1990 are used to derive empirical models of the polar cap potential for quasi-steady interplanetary magnetic field (IMF) conditions. The large data set, due to the high duty cycle and nearly Sun synchronous DMSP orbits, allowed very stringent data selection criteria. The analysis indicates that a good description of the unskewed (Heppner Maynard pattern A) steady state polar cap potential is ΦA = 10-4v2+11.7B sin3 (θ/2) kV, where v is the solar wind velocity in kilometers per second, B is the magnitude of the interplanetary magnetic field in nanoteslas, and θ = arccos (BZ/ |B|)GSM. The IMF-dependent contribution to the cross polar cap potential does not depend significantly on solar wind pressure. Functional forms for the potential do benefit from inclusion of an IMF independent term proportional to the solar wind flow energy. Best fits to IMF-independent contributions to the steady state polar cap potential yield ∼16 kV for vSW = 400 kilometers per second. During steady IMF the total unskewed polar cap potential drop is shown to be approximately ΦA = 16.5 + 15.5 Kp kV. The distribution of potential around the polar cap is examined as a function of magnetic local time. A sinusoidal distribution is an excellent description of the distribution, and more complex forms are not justified by this data set. Analysis of this data set shows no evidence of saturation of the polar cap potential for large |IMF|. A simple unified description of the polar cap potential at all magnetic local times (MLT) and IMF, Φ(IMF, MLT) = -4.1 + 0.5 sin ((2π/24) MLT + 0.056 + 0.015 BYeff) (1.1 × 10-4 v2 + 11.1 B sin3 (θ/2)) kV, is generated, where BYeff is BY (- BY) in the northern (southern) hemisphere. If IMF data is unavailable, the polar cap potential is well described by ΦA(Kp, MLT) = -4.1 +1/2 sin ((2π/24) MLT+φHM)(16.4 + 15.2 Kp) kV, where φHM is a small phase correction of (-0.054, -0.031, 0.040) for Heppner-Maynard convection patterns (BC, A, DE), respectively. Copyright 1997 by the American Geophysical Union.