Imperial College London
Portrait Picture

Dr Lorenzo Matteini

Faculty of Natural Sciences, Department of Physics

Lecturer in Space Plasma Physics
 
 
 
//

Contact

 

l.matteini

 
 
//

Location

 

Blackett LaboratorySouth Kensington Campus

//

Summary

 

Publications

Citation

BibTex format

@article{Tenerani:2020:1538-4365/ab53e1,
author = {Tenerani, A and Velli, M and Matteini, L and Reville, V and Shi, C and Bale, SD and Kasper, JC and Bonnell, JW and Case, AW and de, Wit TD and Goetz, K and Harvey, PR and Klein, KG and Korreck, K and Larson, D and Livi, R and MacDowall, RJ and Malaspina, DM and Pulupa, M and Stevens, M and Whittlesey, P},
doi = {1538-4365/ab53e1},
journal = {Astrophysical Journal Supplement Series},
pages = {1--7},
title = {Magnetic field kinks and folds in the solar wind},
url = {http://dx.doi.org/10.3847/1538-4365/ab53e1},
volume = {246},
year = {2020}
}
Download

RIS format (EndNote, RefMan)

TY  - JOUR
AB  - Parker Solar Probe (PSP) observations during its first encounter at 35.7 R  have shown the presence of magnetic field lines that are strongly perturbed to the point that they produce local inversions of the radial magnetic field, known as switchbacks. Their counterparts in the solar wind velocity field are local enhancements in the radial speed, or jets, displaying (in all components) the velocity–magnetic field correlation typical of large amplitude Alfvén waves propagating away from the Sun. Switchbacks and radial jets have previously been observed over a wide range of heliocentric distances by Helios, Wind, and Ulysses, although they were prevalent in significantly faster streams than seen at PSP. Here we study via numerical magnetohydrodynamics simulations the evolution of such large amplitude Alfvénic fluctuations by including, in agreement with observations, both a radial magnetic field inversion and an initially constant total magnetic pressure. Despite the extremely large excursion of magnetic and velocity fields, switchbacks are seen to persist for up to hundreds of Alfvén crossing times before eventually decaying due to the parametric decay instability. Our results suggest that such switchback/jet configurations might indeed originate in the lower corona and survive out to PSP distances, provided the background solar wind is sufficiently calm, in the sense of not being pervaded by strong density fluctuations or other gradients, such as stream or magnetic field shears, that might destabilize or destroy them over shorter timescales.
AU  - Tenerani,A
AU  - Velli,M
AU  - Matteini,L
AU  - Reville,V
AU  - Shi,C
AU  - Bale,SD
AU  - Kasper,JC
AU  - Bonnell,JW
AU  - Case,AW
AU  - de,Wit TD
AU  - Goetz,K
AU  - Harvey,PR
AU  - Klein,KG
AU  - Korreck,K
AU  - Larson,D
AU  - Livi,R
AU  - MacDowall,RJ
AU  - Malaspina,DM
AU  - Pulupa,M
AU  - Stevens,M
AU  - Whittlesey,P
DO  - 1538-4365/ab53e1
EP  - 7
PY  - 2020///
SN  - 0067-0049
SP  - 1
TI  - Magnetic field kinks and folds in the solar wind
T2  - Astrophysical Journal Supplement Series
UR  - http://dx.doi.org/10.3847/1538-4365/ab53e1
UR  - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000537498600008&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR  - https://iopscience.iop.org/article/10.3847/1538-4365/ab53e1
UR  - http://hdl.handle.net/10044/1/80571
VL  - 246
ER  -
Download