@article{D'Amicis:2025:0004-6361/202451686,
author = {D'Amicis, R and Velli, M and Panasenco, O and Sorriso-Valvo, L and Perrone, D and Benella, S and De, Marco R and Bruno, R and Wang, Y-M and Reville, V and Baker, D and Matteini, L and Yardley, S and Settino, A and Sioulas, N and Alterman, B and Tenerani, A and Raines, J and Holmes, J and Buchlin, E and Verdini, A and Demoulin, P and van, Driel-Gesztelyi L and Telloni, D and Consolini, G and Marcucci, MF and Stangalini, M and Marino, R and Fortunato, V and Mele, G and Monti, F and Owen, CJ and Louarn, P and Livi, S},
doi = {0004-6361/202451686},
journal = {Astronomy and Astrophysics (A & A)},
title = {On alfvenic turbulence of solar wind streams observed by solar orbiter during March 2022 perihelion and their source regions},
url = {http://dx.doi.org/10.1051/0004-6361/202451686},
volume = {693},
year = {2025}
}

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TY  - JOUR
AB  - Context. It has been recently accepted that the standard classification of the solar wind solely according to flow speed is outdated, and particular interest has been devoted to the study of the origin and evolution of so-called Alfvénic slow solar wind streams and to what extent such streams resemble or differ from fast wind.Aims. In March 2022, Solar Orbiter completed its first nominal phase perihelion passage. During this interval, it observed several Alfvénic streams, allowing for characterization of fluctuations in three slow wind intervals (AS1-AS3) and comparison with a fast wind stream (F) at almost the same heliocentric distance.Methods. This work makes use of Solar Orbiter plasma parameters from the Solar Wind Analyzer (SWA) and magnetic field measurements from the magnetometer (MAG). The magnetic connectivity to the solar sources of selected solar wind intervals was reconstructed using a ballistic extrapolation based on measured solar wind speed down to the (spherical) source surface at 2.5 Rs below which a potential field extrapolation was used to map back to the Sun. The source regions were identified using SDO/AIA observations. A spectral analysis of in situ measured magnetic field and velocity fluctuations was performed to characterize correlations, Alfvénicity, normalized cross-helicity, and residual energy in the frequency domain as well as intermittency of the fluctuations and spectral energy transfer rate estimated via mixed third-order moments. A machine learning technique was used to separate proton core, proton beam, and alpha particles and to study v−b correlations for the different ion populations in order to evaluate the role played by each population in determining the Alfvénic content of solar wind fluctuations.Results. The comparison between fast wind and Alfvénic slow wind intervals highlights the differences between the two solar wind regimes: The fast wind is characterized by larger amplitude
AU  - D'Amicis,R
AU  - Velli,M
AU  - Panasenco,O
AU  - Sorriso-Valvo,L
AU  - Perrone,D
AU  - Benella,S
AU  - De,Marco R
AU  - Bruno,R
AU  - Wang,Y-M
AU  - Reville,V
AU  - Baker,D
AU  - Matteini,L
AU  - Yardley,S
AU  - Settino,A
AU  - Sioulas,N
AU  - Alterman,B
AU  - Tenerani,A
AU  - Raines,J
AU  - Holmes,J
AU  - Buchlin,E
AU  - Verdini,A
AU  - Demoulin,P
AU  - van,Driel-Gesztelyi L
AU  - Telloni,D
AU  - Consolini,G
AU  - Marcucci,MF
AU  - Stangalini,M
AU  - Marino,R
AU  - Fortunato,V
AU  - Mele,G
AU  - Monti,F
AU  - Owen,CJ
AU  - Louarn,P
AU  - Livi,S
DO  - 0004-6361/202451686
PY  - 2025///
SN  - 0004-6361
TI  - On alfvenic turbulence of solar wind streams observed by solar orbiter during March 2022 perihelion and their source regions
T2  - Astronomy and Astrophysics (A & A)
UR  - http://dx.doi.org/10.1051/0004-6361/202451686
VL  - 693
ER  - 

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