BibTex format
@article{Bale:2019:10.1038/s41586-019-1818-7,
author = {Bale, SD and Badman, ST and Bonnell, JW and Bowen, TA and Burgess, D and Case, AW and Cattell, CA and Chandran, BDG and Chaston, CC and Chen, CHK and Drake, JF and De, Wit TD and Eastwood, JP and Ergun, RE and Farrell, WM and Fong, C and Goetz, K and Goldstein, M and Goodrich, KA and Harvey, PR and Horbury, TS and Howes, GG and Kasper, JC and Kellogg, PJ and Klimchuk, JA and Korreck, KE and Krasnoselskikh, VV and Krucker, S and Laker, R and Larson, DE and MacDowall, RJ and Maksimovic, M and Malaspina, DM and Martinez-Oliveros, J and McComas, DJ and Meyer-Vernet, N and Moncuquet, M and Mozer, FS and Phan, TD and Pulupa, M and Raouafi, NE and Salem, C and Stansby, D and Stevens, M and Szabo, A and Velli, M and Woolley, T and Wygant, JR},
doi = {10.1038/s41586-019-1818-7},
journal = {Nature},
pages = {237--242},
title = {Highly structured slow solar wind emerging from an equatorial coronal hole},
url = {http://dx.doi.org/10.1038/s41586-019-1818-7},
volume = {576},
year = {2019}
}
RIS format (EndNote, RefMan)
TY - JOUR
AB - During the solar minimum, when the Sun is at its least active, the solar wind1,2 is observed at high latitudes as a predominantly fast (more than 500 kilometres per second), highly Alfvénic rarefied stream of plasma originating from deep within coronal holes. Closer to the ecliptic plane, the solar wind is interspersed with a more variable slow wind3 of less than 500 kilometres per second. The precise origins of the slow wind streams are less certain4; theories and observations suggest that they may originate at the tips of helmet streamers5,6, from interchange reconnection near coronal hole boundaries7,8, or within coronal holes with highly diverging magnetic fields9,10. The heating mechanism required to drive the solar wind is also unresolved, although candidate mechanisms include Alfvén-wave turbulence11,12, heating by reconnection in nanoflares13, ion cyclotron wave heating14 and acceleration by thermal gradients1. At a distance of one astronomical unit, the wind is mixed and evolved, and therefore much of the diagnostic structure of these sources and processes has been lost. Here we present observations from the Parker Solar Probe15 at 36 to 54 solar radii that show evidence of slow Alfvénic solar wind emerging from a small equatorial coronal hole. The measured magnetic field exhibits patches of large, intermittent reversals that are associated with jets of plasma and enhanced Poynting flux and that are interspersed in a smoother and less turbulent flow with a near-radial magnetic field. Furthermore, plasma-wave measurements suggest the existence of electron and ion velocity-space micro-instabilities10,16 that are associated with plasma heating and thermalization processes. Our measurements suggest that there is an impulsive mechanism associated with solar-wind energization and that micro-instabilities play a part in heating, and we provide evidence that low-latitude coronal holes are a key source of the slow solar wind.
AU - Bale,SD
AU - Badman,ST
AU - Bonnell,JW
AU - Bowen,TA
AU - Burgess,D
AU - Case,AW
AU - Cattell,CA
AU - Chandran,BDG
AU - Chaston,CC
AU - Chen,CHK
AU - Drake,JF
AU - De,Wit TD
AU - Eastwood,JP
AU - Ergun,RE
AU - Farrell,WM
AU - Fong,C
AU - Goetz,K
AU - Goldstein,M
AU - Goodrich,KA
AU - Harvey,PR
AU - Horbury,TS
AU - Howes,GG
AU - Kasper,JC
AU - Kellogg,PJ
AU - Klimchuk,JA
AU - Korreck,KE
AU - Krasnoselskikh,VV
AU - Krucker,S
AU - Laker,R
AU - Larson,DE
AU - MacDowall,RJ
AU - Maksimovic,M
AU - Malaspina,DM
AU - Martinez-Oliveros,J
AU - McComas,DJ
AU - Meyer-Vernet,N
AU - Moncuquet,M
AU - Mozer,FS
AU - Phan,TD
AU - Pulupa,M
AU - Raouafi,NE
AU - Salem,C
AU - Stansby,D
AU - Stevens,M
AU - Szabo,A
AU - Velli,M
AU - Woolley,T
AU - Wygant,JR
DO - 10.1038/s41586-019-1818-7
EP - 242
PY - 2019///
SN - 0028-0836
SP - 237
TI - Highly structured slow solar wind emerging from an equatorial coronal hole
T2 - Nature
UR - http://dx.doi.org/10.1038/s41586-019-1818-7
UR - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000502792400050&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR - https://www.nature.com/articles/s41586-019-1818-7
UR - http://hdl.handle.net/10044/1/84221
VL - 576
ER -