Imperial College London
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Dr Lorenzo Matteini

Faculty of Natural Sciences, Department of Physics

Lecturer in Space Plasma Physics
 
 
 
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Contact

 

l.matteini

 
 
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Location

 

Blackett LaboratorySouth Kensington Campus

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Summary

 

Publications

Citation

BibTex format

@article{Perrone:2020:0004-6361/201937064,
author = {Perrone, D and D'Amicis, R and De, Marco R and Matteini, L and Stansby, D and Bruno, R and Horbury, TS},
doi = {0004-6361/201937064},
journal = {Astronomy and Astrophysics: a European journal},
pages = {1--7},
title = {Highly Alfvenic slow solar wind at 0.3 au during a solar minimum: Helios insights for Parker Solar Probe and Solar Orbiter},
url = {http://dx.doi.org/10.1051/0004-6361/201937064},
volume = {633},
year = {2020}
}
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RIS format (EndNote, RefMan)

TY  - JOUR
AB  - Alfvénic fluctuations in solar wind are an intrinsic property of fast streams, while slow intervals typically have a very low degree of Alfvénicity, with much more variable parameters. However, sometimes a slow wind can be highly Alfvénic. Here we compare three different regimes of solar wind, in terms of Alfvénic content and spectral properties, during a minimum phase of the solar activity and at 0.3 au. We show that fast and Alfvénic slow intervals share some common characteristics. This would suggest a similar solar origin, with the latter coming from over-expanded magnetic field lines, in agreement with observations at 1 au and at the maximum of the solar cycle. Due to the Alfvénic nature of the fluctuations in both fast and Alfvénic slow winds, we observe a well-defined correlation between the flow speed and the angle between magnetic field vector and radial direction. The high level of Alfvénicity is also responsible of intermittent enhancements (i.e. spikes), in plasma speed. Moreover, only for the Alfvénic intervals do we observe a break between the inertial range and large scales, on about the timescale typical of the Alfvénic fluctuations and where the magnetic fluctuations saturate, limited by the magnitude of the local magnetic field. In agreement with this, we recover a characteristic low-frequency 1/f scaling, as expected for fluctuations that are scale-independent. This work is directly relevant for the next solar missions, Parker Solar Probe and Solar Orbiter. One of the goals of these two missions is to study the origin and evolution of slow solar wind. In particular, Parker Solar Probe will give information about the Alfvénic slow wind in the unexplored region much closer to the Sun and Solar Orbiter will allow us to connect the observed physics to the source of the plasma.
AU  - Perrone,D
AU  - D'Amicis,R
AU  - De,Marco R
AU  - Matteini,L
AU  - Stansby,D
AU  - Bruno,R
AU  - Horbury,TS
DO  - 0004-6361/201937064
EP  - 7
PY  - 2020///
SN  - 0004-6361
SP  - 1
TI  - Highly Alfvenic slow solar wind at 0.3 au during a solar minimum: Helios insights for Parker Solar Probe and Solar Orbiter
T2  - Astronomy and Astrophysics: a European journal
UR  - http://dx.doi.org/10.1051/0004-6361/201937064
UR  - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000509938700001&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR  - https://www.aanda.org/articles/aa/abs/2020/01/aa37064-19/aa37064-19.html
UR  - http://hdl.handle.net/10044/1/82732
VL  - 633
ER  -
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