Joseph Lemaire | UCLouvain (University of Louvain) (original) (raw)
Papers by Joseph Lemaire
The Earth's Plasmasphere, 1998
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Geophysical monograph, 1996
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37th COSPAR Scientific Assembly, 2008
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jl@oma.be This paper reports additional activities of the Center for Space Radiation (CSR) at the... more jl@oma.be This paper reports additional activities of the Center for Space Radiation (CSR) at the Institut de Physique Nucleaire of the Universite Catholique de Louvain, and, of the Belgian Institute for Space Aeronomy (IASB-BlRA) in the field of magnetospheric physics not presented in the companion paper of this volume. It outlines recent theoretical contributions on the distribution of themlal particles in the Plasmasphere as well as on their convective stability. The electron density profiles deduced from the ISEE-2 wave experiment have been used as a baseline in this study. This paper addresses also the progress made in simulating the mechanism of Impulsive Penetration of solar wind plasma elements into the magnetosphere. Finally, we outline the results that have been obtained about the distribution of energetic protons trapped in the geomagnetic field during highly disturbed geomagnetic conditions. For this purpose we have used the energetic particle fluxes measured with the Ch...
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Solar Physics, 2021
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Bulletin de la Classe des sciences, 1979
A partir des données de concentration d'ions du satellite OGO V, nous avons établi la distrib... more A partir des données de concentration d'ions du satellite OGO V, nous avons établi la distribution d'éléments de plasma détachés dans la magnétosphère. Nous avons aussi étudié la fréquence relative d'apparition des éléments détachés dans différents secteurs de temps local ; enfin, nous avons analysé la dépendance de cette fréquence avec l'activité magnétique.
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Bulletin de la Classe des sciences, 1972
In this Solar Wind Model, the Coulomb collisions, with impact parameter smaller than the Debye le... more In this Solar Wind Model, the Coulomb collisions, with impact parameter smaller than the Debye length, have been neglected beyond the baropause located at 6.6 Solar radii. The radial distribution of the electric potential is calculated in order to satisfy the local and global quasi-neutrality conditions in the whole exospheric plasma. The asymptotic behavior for large radial distances as well as in the neighbourhood of the baropause has been calculated and discussed. It has been deduced that the electric field distribution near the baropause does practically not influence the properties at 1AU. A simple relationship between the coronal temperature and Solar Wind velocity at large radial distances has been found ; the kinetic plasma pressure is found to decrease asymptotically to zero as r -> oo : the parallel and perpendicular temperatures of the protons satisfy the „ adiabatic approximation " of Chew, Goldberger and Low in the most external regions (r > 100 Rs). The use ...
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Solar Physics, 2016
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The most popular method for determining coronal temperatures is the scale-height-method (shm). It... more The most popular method for determining coronal temperatures is the scale-height-method (shm). It is based on electron density profiles inferred from White Light (WL) brightness measurements of the corona during solar eclipses. This method has been applied to several published coronal electron density models. The calculated temperature distributions reach a maximum at r > 1.3 RS, and therefore do not satisfy one of the conditions for applying the shm method. Another method is the hydrostatic equilibrium method (hst), which enables coronal temperature distributions to be determined, providing solutions to the hydrostatic equilibrium equation. The temperature maximas using the hst method are almost equal to those obtained using the shm method, but the temperature peak is always at significantly lower altitude when the hst-method is used than when the shm-method is used. A third and more recently developed method, dyn, can be used for the same published electron density profiles. Th...
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Geophysical Monograph Series, 2013
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Radiation Measurements, 1999
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Radiation Measurements, 1996
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Planetary and Space Science, 1970
A model of a polar ion-exosphere in which the geomagnetic field lines are open is developed. The ... more A model of a polar ion-exosphere in which the geomagnetic field lines are open is developed. The electrostatic field in this region has been calculated by taking into account two fundamental conditions: (1) quasi-neutrality has to be satisfied everywhere in the exosphere; (2) escape fluxes of electrons and ions have to be equal. The density distributions are calculated for different evaporative models in the case of two (O+ and e) and three (O+, H+ and e) constituents. In addition, the mean velocity, pressure and temperature distributions of the several constituents are derived.
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Planetary and Space Science, 1989
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Physica Scripta, 1987
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The Earth's Plasmasphere, 1998
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Geophysical monograph, 1996
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37th COSPAR Scientific Assembly, 2008
Bookmarks Related papers MentionsView impact
Bookmarks Related papers MentionsView impact
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jl@oma.be This paper reports additional activities of the Center for Space Radiation (CSR) at the... more jl@oma.be This paper reports additional activities of the Center for Space Radiation (CSR) at the Institut de Physique Nucleaire of the Universite Catholique de Louvain, and, of the Belgian Institute for Space Aeronomy (IASB-BlRA) in the field of magnetospheric physics not presented in the companion paper of this volume. It outlines recent theoretical contributions on the distribution of themlal particles in the Plasmasphere as well as on their convective stability. The electron density profiles deduced from the ISEE-2 wave experiment have been used as a baseline in this study. This paper addresses also the progress made in simulating the mechanism of Impulsive Penetration of solar wind plasma elements into the magnetosphere. Finally, we outline the results that have been obtained about the distribution of energetic protons trapped in the geomagnetic field during highly disturbed geomagnetic conditions. For this purpose we have used the energetic particle fluxes measured with the Ch...
Bookmarks Related papers MentionsView impact
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Solar Physics, 2021
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Bulletin de la Classe des sciences, 1979
A partir des données de concentration d'ions du satellite OGO V, nous avons établi la distrib... more A partir des données de concentration d'ions du satellite OGO V, nous avons établi la distribution d'éléments de plasma détachés dans la magnétosphère. Nous avons aussi étudié la fréquence relative d'apparition des éléments détachés dans différents secteurs de temps local ; enfin, nous avons analysé la dépendance de cette fréquence avec l'activité magnétique.
Bookmarks Related papers MentionsView impact
Bulletin de la Classe des sciences, 1972
In this Solar Wind Model, the Coulomb collisions, with impact parameter smaller than the Debye le... more In this Solar Wind Model, the Coulomb collisions, with impact parameter smaller than the Debye length, have been neglected beyond the baropause located at 6.6 Solar radii. The radial distribution of the electric potential is calculated in order to satisfy the local and global quasi-neutrality conditions in the whole exospheric plasma. The asymptotic behavior for large radial distances as well as in the neighbourhood of the baropause has been calculated and discussed. It has been deduced that the electric field distribution near the baropause does practically not influence the properties at 1AU. A simple relationship between the coronal temperature and Solar Wind velocity at large radial distances has been found ; the kinetic plasma pressure is found to decrease asymptotically to zero as r -> oo : the parallel and perpendicular temperatures of the protons satisfy the „ adiabatic approximation " of Chew, Goldberger and Low in the most external regions (r > 100 Rs). The use ...
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Solar Physics, 2016
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The most popular method for determining coronal temperatures is the scale-height-method (shm). It... more The most popular method for determining coronal temperatures is the scale-height-method (shm). It is based on electron density profiles inferred from White Light (WL) brightness measurements of the corona during solar eclipses. This method has been applied to several published coronal electron density models. The calculated temperature distributions reach a maximum at r > 1.3 RS, and therefore do not satisfy one of the conditions for applying the shm method. Another method is the hydrostatic equilibrium method (hst), which enables coronal temperature distributions to be determined, providing solutions to the hydrostatic equilibrium equation. The temperature maximas using the hst method are almost equal to those obtained using the shm method, but the temperature peak is always at significantly lower altitude when the hst-method is used than when the shm-method is used. A third and more recently developed method, dyn, can be used for the same published electron density profiles. Th...
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Geophysical Monograph Series, 2013
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Radiation Measurements, 1999
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Radiation Measurements, 1996
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Planetary and Space Science, 1970
A model of a polar ion-exosphere in which the geomagnetic field lines are open is developed. The ... more A model of a polar ion-exosphere in which the geomagnetic field lines are open is developed. The electrostatic field in this region has been calculated by taking into account two fundamental conditions: (1) quasi-neutrality has to be satisfied everywhere in the exosphere; (2) escape fluxes of electrons and ions have to be equal. The density distributions are calculated for different evaporative models in the case of two (O+ and e) and three (O+, H+ and e) constituents. In addition, the mean velocity, pressure and temperature distributions of the several constituents are derived.
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Planetary and Space Science, 1989
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Physica Scripta, 1987
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