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Exospheric Solar Wind


CCMC Services available for Exospheric Solar Wind
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Model Developer(s)
H.Lamy, V.Pierrard
IASB-BIRA

Model Description
This is an exospheric model of the solar wind with only protons and electrons (we defer the inclusion of heavy ions to upcoming versions of the code), with a non-monotonic total potential for the protons and with a Lorentzian (kappa) velocity distribution function (VDF) for the electrons. This code is developed for the coronal holes.

Exospheric kinetic models assume that there is a sharp level called the exobase, separating a collision dominated region (where a fluid approximation is valid) from a region fully collisionless. In fact, there is a transition region where collisions between particles become less and less numerous when the distance to the Sun increases. Click here to read more about the basics of the exospheric kinetic models.

Model Input

Model Output

References and relevant publications
H.Lamy, V.Pierrard, M.Maksimovic and J.F.Lemaire, A Kinetic Exospheric Model Of the Solar Wind With a Nonmonotonic Potential Energy For the Protons, J. Geophys. Res., 108, 1047, 2003.

Relevant links
IASB
Full Model Description Document

CCMC Contact(s)

301-286-9571

National Aeronautics and Space Administration Air Force Materiel Command Air Force Office of Scientific Research Air Force Research Laboratory Air Force Weather Agency NOAA Space Environment Center National Science Foundation Office of Naval Research

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