Abstract
We use a kinetic collisionless model of the solar wind to calculate the radial variation of the electron temperature and obtain analytical expressions at large radial distances. In order to be compared with Ulysses observations, the model, which initially assumed a radial magnetic field, has been generalized to a spiral magnetic field. We present a preliminary comparison with Ulysses observations in the fast solar wind at high heliospheric latitudes.
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References
Issautier, K., et al.: 1998, J. Geophys. Res. 103, 1969.
Issautier, K., et al.: 1999, Solar Wind Nine, AIP Conference Proceeding 471, 581.
Maksimovic, M., Pierrard, V. and Lemaire, J.: 1997, Astron. Astrophys. 324, 725.
Meyer-Vernet, N.: 1999, Eur. J. Phys. 20, 167.
Meyer-Vernet, N. and Issautier, K.: 1998, J. Geophys. Res. 103, 29,705.
Parker, E.: 1958, Astrophys. J. 128, 664.
Pierrard, V., Issautier, K., Meyer-Vernet, N. and Lemaire, J.: 2001, Geophys. Res. Lett. 28, 223.
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Issautier, K., Meyer-Vernet, N., Pierrard, V. et al. Electron Temperature in the Solar Wind From a Kinetic Collisionless Model: Application to High-Latitude Ulysses Observations. Astrophysics and Space Science 277, 189–193 (2001). https://doi.org/10.1023/A:1012206230015
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DOI: https://doi.org/10.1023/A:1012206230015