@article{Matteini:2007:10.1029/2007gl030920,
author = {Matteini, L and Landi, S and Hellinger, P and Pantellini, F and Maksimovic, M and Velli, M and Goldstein, BE and Marsch, E},
doi = {10.1029/2007gl030920},
journal = {Geophysical Research Letters},
title = {Evolution of the solar wind proton temperature anisotropy from 0.3 to 2.5 AU},
url = {http://dx.doi.org/10.1029/2007gl030920},
volume = {34},
year = {2007}
}

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TY  - JOUR
AB  - <jats:p>                    We report an analysis of the proton temperature anisotropy evolution from 0.3 to 2.5 AU based on the Helios and Ulysses observations. With increasing distance the fast wind data show a path in the parameter space (                    <jats:italic>β</jats:italic>                    <jats:sub>                                            <jats:italic>p</jats:italic>                    </jats:sub>                    ,                    <jats:italic>T</jats:italic>                    <jats:sub>                      ⊥                      <jats:italic>p</jats:italic>                    </jats:sub>                    /                    <jats:italic>T</jats:italic>                    <jats:sub>                                            <jats:italic>p</jats:italic>                    </jats:sub>                    ). The first part of the trajectory is well described by an anticorrelation between the temperature anisotropy                    <jats:italic>T</jats:italic>                    <jats:sub>                      ⊥                      <jats:italic>p</jats:italic>                    </jats:sub>                    /                    <jats:italic>T</jats:italic>                    <jats:sub>                                            <jats:italic>p</jats:italic>                    </jats:sub>                    and the proton parallel beta, while after 1 AU the evolution with distance in the parameter space changes and the data result in agreement with the constraints derived by a fire hose instability. The slow wind data show a more irregular behavior, and in general it is not possible to recover a single evolution path. However, on small temporal scale we find that different slow streams populate different regions of the parameter spac
AU  - Matteini,L
AU  - Landi,S
AU  - Hellinger,P
AU  - Pantellini,F
AU  - Maksimovic,M
AU  - Velli,M
AU  - Goldstein,BE
AU  - Marsch,E
DO  - 10.1029/2007gl030920
PY  - 2007///
SN  - 0094-8276
TI  - Evolution of the solar wind proton temperature anisotropy from 0.3 to 2.5 AU
T2  - Geophysical Research Letters
UR  - http://dx.doi.org/10.1029/2007gl030920
UR  - https://doi.org/10.1029/2007gl030920
VL  - 34
ER  - 

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