Scale and Time Dependence of Alfvénicity in the Solar Wind as Observed by the Parker Solar Probe
Issued Date
2024-02-01
Resource Type
ISSN
0004637X
eISSN
15384357
Scopus ID
2-s2.0-85184619254
Journal Title
Astrophysical Journal
Volume
962
Issue
1
Rights Holder(s)
SCOPUS
Bibliographic Citation
Astrophysical Journal Vol.962 No.1 (2024)
Suggested Citation
Thepthong P., Pongkitiwanichakul P., Ruffolo D., Kieokaew R., Bandyopadhyay R., Matthaeus W.H., Parashar T.N. Scale and Time Dependence of Alfvénicity in the Solar Wind as Observed by the Parker Solar Probe. Astrophysical Journal Vol.962 No.1 (2024). doi:10.3847/1538-4357/ad1592 Retrieved from: https://repository.li.mahidol.ac.th/handle/20.500.14594/97222
Title
Scale and Time Dependence of Alfvénicity in the Solar Wind as Observed by the Parker Solar Probe
Corresponding Author(s)
Other Contributor(s)
Abstract
Alfvénicity is a well-known property, common in the solar wind, characterized by a high correlation between magnetic and velocity fluctuations. Data from the Parker Solar Probe (PSP) enable the study of this property closer to the Sun than ever before, as well as in the sub-Alfvénic solar wind. We consider scale-dependent measures of Alfvénicity based on second-order functions of the magnetic and velocity increments as a function of time lag, including the normalized cross helicity σc and residual energy σr. Scale-dependent Alfvénicity is strongest for lags near the correlation scale and increases when moving closer to the Sun. We find that σr typically remains close to the maximally negative value compatible with σc. We did not observe significant changes in measures of Alfvénicity between sub-Alfvénic and super-Alfvénic wind. During most times, the solar wind was highly Alfvénic; however, lower Alfvénicity was observed when PSP approached the heliospheric current sheet or other magnetic structures with sudden changes in the radial magnetic field, non-unidirectional strahl electron pitch angle distributions, and strong electron density contrasts. These results are consistent with a picture in which Alfvénic fluctuations generated near the photosphere transport outward, forming highly Alfvénic states in the young solar wind, and subsequent interactions with large-scale structures and gradients lead to weaker Alfvénicity, as commonly observed at larger heliocentric distances.