Abstract
A forward-reverse interplanetary shock was observed on 25 March 1969 by the magnetometer and plasma detector on the HEOS-1 satellite. This relatively rare event was described by Chao et al (1972) who concluded that the shock pair was formed at a distance 0.10 to 0.13 AU upstream of the Earth as a result of the interaction between a fast and a slow solar wind streams. Simultaneous observations of 1 MeV solar proton fluxes were also performed on HEOS-1. A characteristic intensity peak was observed as the forward shock passed by the spacecraft. The evolution of the proton intensity, together with a detailed analysis of anisotropies and pitch angle distributions show a complex dynamic picture of the effect of the forward shock on the ambient proton population. Significant changes in particle fluxes are seen to be correlated with fluctuations in the magnetic field. It is suggested that simple geometrical models of shock-assisted acceleration should be expanded to include the effect of magnetic fluctuations on particle fluxes. The interaction region limited by the forward and reverse shocks contained a large variety of magnetic fluctuations. Following the tangential discontinuity separating the fast solar wind stream from the preceding slow stream, a sunward flow
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Balogh, A
[1]
- Imperial Coll. of Science and Technology, London (UK)
Citation Formats
Balogh, A.
Energetic protons associated with a forward-reverse interplanetary shock pair at 1 A. U.
United Kingdom: N. p.,
1977.
Web.
doi:10.1016/0032-0633(77)90007-1.
Balogh, A.
Energetic protons associated with a forward-reverse interplanetary shock pair at 1 A. U.
United Kingdom.
https://doi.org/10.1016/0032-0633(77)90007-1
Balogh, A.
1977.
"Energetic protons associated with a forward-reverse interplanetary shock pair at 1 A. U."
United Kingdom.
https://doi.org/10.1016/0032-0633(77)90007-1.
@misc{etde_5085997,
title = {Energetic protons associated with a forward-reverse interplanetary shock pair at 1 A. U}
author = {Balogh, A}
abstractNote = {A forward-reverse interplanetary shock was observed on 25 March 1969 by the magnetometer and plasma detector on the HEOS-1 satellite. This relatively rare event was described by Chao et al (1972) who concluded that the shock pair was formed at a distance 0.10 to 0.13 AU upstream of the Earth as a result of the interaction between a fast and a slow solar wind streams. Simultaneous observations of 1 MeV solar proton fluxes were also performed on HEOS-1. A characteristic intensity peak was observed as the forward shock passed by the spacecraft. The evolution of the proton intensity, together with a detailed analysis of anisotropies and pitch angle distributions show a complex dynamic picture of the effect of the forward shock on the ambient proton population. Significant changes in particle fluxes are seen to be correlated with fluctuations in the magnetic field. It is suggested that simple geometrical models of shock-assisted acceleration should be expanded to include the effect of magnetic fluctuations on particle fluxes. The interaction region limited by the forward and reverse shocks contained a large variety of magnetic fluctuations. Following the tangential discontinuity separating the fast solar wind stream from the preceding slow stream, a sunward flow was observed in the proton data, followed by a small but significant drop in intensity prior to the reverse shock.}
doi = {10.1016/0032-0633(77)90007-1}
journal = []
volume = {25:10}
journal type = {AC}
place = {United Kingdom}
year = {1977}
month = {Oct}
}
title = {Energetic protons associated with a forward-reverse interplanetary shock pair at 1 A. U}
author = {Balogh, A}
abstractNote = {A forward-reverse interplanetary shock was observed on 25 March 1969 by the magnetometer and plasma detector on the HEOS-1 satellite. This relatively rare event was described by Chao et al (1972) who concluded that the shock pair was formed at a distance 0.10 to 0.13 AU upstream of the Earth as a result of the interaction between a fast and a slow solar wind streams. Simultaneous observations of 1 MeV solar proton fluxes were also performed on HEOS-1. A characteristic intensity peak was observed as the forward shock passed by the spacecraft. The evolution of the proton intensity, together with a detailed analysis of anisotropies and pitch angle distributions show a complex dynamic picture of the effect of the forward shock on the ambient proton population. Significant changes in particle fluxes are seen to be correlated with fluctuations in the magnetic field. It is suggested that simple geometrical models of shock-assisted acceleration should be expanded to include the effect of magnetic fluctuations on particle fluxes. The interaction region limited by the forward and reverse shocks contained a large variety of magnetic fluctuations. Following the tangential discontinuity separating the fast solar wind stream from the preceding slow stream, a sunward flow was observed in the proton data, followed by a small but significant drop in intensity prior to the reverse shock.}
doi = {10.1016/0032-0633(77)90007-1}
journal = []
volume = {25:10}
journal type = {AC}
place = {United Kingdom}
year = {1977}
month = {Oct}
}