The Role of Alfvén Wave Dynamics on the Large-scale Properties of the Solar Wind: Comparing an MHD Simulation with Parker Solar Probe E1 Data. Réville, V., Velli, M., Panasenco, O., Tenerani, A., Shi, C., Badman, S. T., Bale, S. D., Kasper, J. C., Stevens, M. L., Korreck, K. E., Bonnell, J. W., Case, A. W., Wit, T. D. d., Goetz, K., Harvey, P. R., Larson, D. E., Livi, R., Malaspina, D. M., MacDowall, R. J., Pulupa, M., & Whittlesey, P. L. Astrophysical Journal, Supplement Series, January, 1970. ![The Role of Alfvén Wave Dynamics on the Large-scale Properties of the Solar Wind: Comparing an MHD Simulation with Parker Solar Probe E1 Data [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper doi abstract bibtex During Parker Solar Probe's first orbit, the solar wind plasma was observed in situ closer than ever before, the perihelion on 2018 November 6 revealing a flow that is constantly permeated by large-amplitude Alfvénic fluctuations. These include radial magnetic field reversals, or switchbacks, that seem to be a persistent feature of the young solar wind. The measurements also reveal a very strong, unexpected, azimuthal velocity component. In this work, we numerically model the solar corona during this first encounter, solving the MHD equations and accounting for Alfvén wave transport and dissipation. We find that the large-scale plasma parameters are well reproduced, allowing the computation of the solar wind sources at Probe with confidence. We try to understand the dynamical nature of the solar wind to explain both the amplitude of the observed radial magnetic field and of the azimuthal velocities.
@article{reville_role_1970,
title = {The {Role} of {Alfvén} {Wave} {Dynamics} on the {Large}-scale {Properties} of the {Solar} {Wind}: {Comparing} an {MHD} {Simulation} with {Parker} {Solar} {Probe} {E1} {Data}},
url = {http://iopscience.iop.org/0067-0049/246/2/24?utm_source=researcher_app&utm_medium=referral&utm_campaign=RESR_MRKT_Researcher_inbound},
doi = {10.3847/1538-4365/ab4fef},
abstract = {During \textit{Parker Solar Probe}'s first orbit, the solar wind plasma was observed in situ closer than ever before, the perihelion on 2018 November 6 revealing a flow that is constantly permeated by large-amplitude Alfvénic fluctuations. These include radial magnetic field reversals, or switchbacks, that seem to be a persistent feature of the young solar wind. The measurements also reveal a very strong, unexpected, azimuthal velocity component. In this work, we numerically model the solar corona during this first encounter, solving the MHD equations and accounting for Alfvén wave transport and dissipation. We find that the large-scale plasma parameters are well reproduced, allowing the computation of the solar wind sources at \textit{Probe} with confidence. We try to understand the dynamical nature of the solar wind to explain both the amplitude of the observed radial magnetic field and of the azimuthal velocities.},
journal = {Astrophysical Journal, Supplement Series},
author = {Réville, Victor and Velli, Marco and Panasenco, Olga and Tenerani, Anna and Shi, Chen and Badman, Samuel T. and Bale, Stuart D. and Kasper, J. C. and Stevens, Michael L. and Korreck, Kelly E. and Bonnell, J. W. and Case, Anthony W. and Wit, Thierry Dudok de and Goetz, Keith and Harvey, Peter R. and Larson, Davin E. and Livi, Roberto and Malaspina, David M. and MacDowall, Robert J. and Pulupa, Marc and Whittlesey, Phyllis L.},
month = jan,
year = {1970},
keywords = {Researcher App},
}
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