TY - JOUR
T1 - The multi-scale nature of the solar wind
AU - Verscharen, Daniel
AU - Klein, Kristopher G.
AU - Maruca, Bennett A.
N1 - Funding Information:
This work was supported by the STFC Ernest Rutherford Fellowship ST/P003826/1, the STFC Consolidated Grant ST/S000240/1, as well as NASA grants NNX16AM23G and NNX16AG81G. We acknowledge the use of data from Wind’s SWE instrument (PIs K. W. Ogilvie and A. F. Viñas), from Wind’s MFI instrument (PI A. Szabo), and from Ulysses’ SWOOPS instrument (PI D. J. McComas). Lynn Wilson is Wind’s Project Scientist. We extend our gratitude to Chadi Salem for providing processed Wind/3DP (PI S. D. Bale) data to create Fig. . We also acknowledge the use of data from ESA’s Cluster Science Archive (Laakso et al. ) from the EFW instrument (PI M. André), the FGM instrument (PI C. Carr), the STAFF instrument (PI P. Canu), the CIS instrument (PI I. Dandouras), and the PEACE instrument (PI A. Fazakerley). We acknowledge vigorous feedback on Fig. from D. J. McComas at the 2019 SHINE Meeting. Data access was provided by the National Space Science Data Center (NSSDC) Space Physics Data Facility (SPDF) and NASA/GSFC’s Space Physics Data Facility’s CDAWeb and COHOWeb services. This review has made use of the SAO/NASA Astrophysics Data System (ADS).
Funding Information:
This work was supported by the STFC Ernest Rutherford Fellowship ST/P003826/1, the STFC Consolidated Grant ST/S000240/1, as well as NASA grants NNX16AM23G and NNX16AG81G. We acknowledge the use of data from Wind’s SWE instrument (PIs K. W. Ogilvie and A. F. Viñas), from Wind’s MFI instrument (PI A. Szabo), and from Ulysses’ SWOOPS instrument (PI D. J. McComas). Lynn Wilson is Wind’s Project Scientist. We extend our gratitude to Chadi Salem for providing processed Wind/3DP (PI S. D. Bale) data to create Fig. 14. We also acknowledge the use of data from ESA’s Cluster Science Archive (Laakso et al. 2010) from the EFW instrument (PI M. André), the FGM instrument (PI C. Carr), the STAFF instrument (PI P. Canu), the CIS instrument (PI I. Dandouras), and the PEACE instrument (PI A. Fazakerley). We acknowledge vigorous feedback on Fig. 8 from D. J. McComas at the 2019 SHINE Meeting. Data access was provided by the National Space Science Data Center (NSSDC) Space Physics Data Facility (SPDF) and NASA/GSFC’s Space Physics Data Facility’s CDAWeb and COHOWeb services. This review has made use of the SAO/NASA Astrophysics Data System (ADS).
Publisher Copyright:
© 2019, The Author(s).
PY - 2019/12/1
Y1 - 2019/12/1
N2 - The solar wind is a magnetized plasma and as such exhibits collective plasma behavior associated with its characteristic spatial and temporal scales. The characteristic length scales include the size of the heliosphere, the collisional mean free paths of all species, their inertial lengths, their gyration radii, and their Debye lengths. The characteristic timescales include the expansion time, the collision times, and the periods associated with gyration, waves, and oscillations. We review the past and present research into the multi-scale nature of the solar wind based on in-situ spacecraft measurements and plasma theory. We emphasize that couplings of processes across scales are important for the global dynamics and thermodynamics of the solar wind. We describe methods to measure in-situ properties of particles and fields. We then discuss the role of expansion effects, non-equilibrium distribution functions, collisions, waves, turbulence, and kinetic microinstabilities for the multi-scale plasma evolution.
AB - The solar wind is a magnetized plasma and as such exhibits collective plasma behavior associated with its characteristic spatial and temporal scales. The characteristic length scales include the size of the heliosphere, the collisional mean free paths of all species, their inertial lengths, their gyration radii, and their Debye lengths. The characteristic timescales include the expansion time, the collision times, and the periods associated with gyration, waves, and oscillations. We review the past and present research into the multi-scale nature of the solar wind based on in-situ spacecraft measurements and plasma theory. We emphasize that couplings of processes across scales are important for the global dynamics and thermodynamics of the solar wind. We describe methods to measure in-situ properties of particles and fields. We then discuss the role of expansion effects, non-equilibrium distribution functions, collisions, waves, turbulence, and kinetic microinstabilities for the multi-scale plasma evolution.
KW - Coulomb collisions
KW - Kinetic instabilities
KW - Plasma waves and turbulence
KW - Solar wind
KW - Spacecraft measurements
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U2 - 10.1007/s41116-019-0021-0
DO - 10.1007/s41116-019-0021-0
M3 - Review article
AN - SCOPUS:85076341646
VL - 16
JO - Living Reviews in Solar Physics
JF - Living Reviews in Solar Physics
SN - 1614-4961
IS - 1
M1 - 5
ER -