Solar wind expansion in a polar coronal hole: Inferences from coronal white light and interplanetary Lyman alpha observations

1986 ◽  
Vol 91 (A6) ◽  
pp. 6751 ◽  
Author(s):  
R. Lallement ◽  
T. E. Holzer ◽  
R. H. Munro
Keyword(s):  
Solar Wind ◽  
Coronal Hole ◽  
White Light ◽  
Polar Coronal Hole ◽  
Lyman Alpha

scholarly journals The effect of plume/interplume lanes on ion-cyclotron resonance heating

2010 ◽  
Vol 6 (S274) ◽  
pp. 137-139
Author(s):  
Suzan Doğan ◽  
E. Rennan Pekünlü
Keyword(s):  
Solar Wind ◽  
Coronal Hole ◽  
Cyclotron Resonance ◽  
Polar Coronal Hole ◽  
Ion Cyclotron Resonance ◽  
Fast Solar Wind ◽  
Ion Cyclotron ◽  
North Polar

AbstractThe effect of the Plume/Interplume Lane (PIPL) structure of the solar North Polar Coronal Hole (NPCH) on the ion-cyclotron resonance (ICR) process is investigated. The ICR process in the interplume lanes is much more effective than in the plumes, agreeing with the observations which show the source of fast solar wind is interplume lanes.

Characterisation and comparison of slow coronal hole wind intervals at 0.13au

2021 ◽  
Author(s):  
Thomas Woolley ◽  
Lorenzo Matteini ◽  
Timothy S Horbury ◽  
Ronan Laker ◽  
Lloyd D Woodham ◽  
...  
Keyword(s):  
Solar Wind ◽  
Current Sheet ◽  
Coronal Hole ◽  
Heliocentric Distance ◽  
Heliospheric Current Sheet ◽  
Polar Coronal Hole ◽  
Slow Solar Wind ◽  
The Sun ◽  
Streamer Belt ◽  
Different Origin

<p>The slow solar wind is thought to consist of a component originating close to the Heliospheric Current Sheet (HCS) in the streamer belt and a component from over-expanded coronal hole boundaries. In order to understand the roles of these contributions with different origin, it is important to separate and characterise them. By exploiting the fact that Parker Solar Probe’s fourth and fifth orbits were the same and the solar conditions were similar, we identify intervals of slow polar coronal hole wind sampled at approximately the same heliocentric distance and latitude. Here, solar wind properties are compared, highlighting typical conditions of the slow coronal hole wind closer to the Sun than ever before. We explore different properties of the plasma, including composition, spectra and microphysics, and discuss possible origins for the features that are observed.</p>

scholarly journals Highly structured slow solar wind emerging from an equatorial coronal hole

Nature ◽  
2019 ◽  
Vol 576 (7786) ◽  
pp. 237-242 ◽  
Author(s):  
S. D. Bale ◽  
S. T. Badman ◽  
J. W. Bonnell ◽  
T. A. Bowen ◽  
D. Burgess ◽  
...  
Keyword(s):  
Solar Wind ◽  
Coronal Hole ◽  
Slow Solar Wind

Lyman α intensities in a polar coronal hole from a 2D model

2002 ◽  
Vol 30 (3) ◽  
pp. 523-528
Author(s):  
L. Zangrilli ◽  
G. Poletto ◽  
P. Nicolosi ◽  
G. Noci
Keyword(s):  
Coronal Hole ◽  
Polar Coronal Hole ◽  
2D Model

scholarly journals Real-Time Solar Wind Prediction Based on SDO/AIA Coronal Hole Data

Solar Physics ◽  
2015 ◽  
Vol 290 (5) ◽  
pp. 1355-1370 ◽  
Author(s):  
T. Rotter ◽  
A. M. Veronig ◽  
M. Temmer ◽  
B. Vršnak
Keyword(s):  
Solar Wind ◽  
Coronal Hole ◽  
Real Time

MHD waves in the solar north polar coronal hole

2010 ◽  
Vol 331 (7) ◽  
pp. 716-724 ◽  
Author(s):  
E. Devlen ◽  
E.R. Pekünlü
Keyword(s):  
Coronal Hole ◽  
Polar Coronal Hole ◽  
Mhd Waves ◽  
North Polar

scholarly journals Photospheric magnetic field of an eroded-by-solar-wind coronal mass ejection

2016 ◽  
Vol 12 (S327) ◽  
pp. 67-70
Author(s):  
J. Palacios ◽  
C. Cid ◽  
E. Saiz ◽  
A. Guerrero
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Coronal Hole ◽  
Interplanetary Medium ◽  
Flux Rope ◽  
Magnetic Characteristics ◽  
Interplanetary Coronal Mass Ejection ◽  
Fast Wind ◽  
Mass Ejection

AbstractWe have investigated the case of a coronal mass ejection that was eroded by the fast wind of a coronal hole in the interplanetary medium. When a solar ejection takes place close to a coronal hole, the flux rope magnetic topology of the coronal mass ejection (CME) may become misshapen at 1 AU as a result of the interaction. Detailed analysis of this event reveals erosion of the interplanetary coronal mass ejection (ICME) magnetic field. In this communication, we study the photospheric magnetic roots of the coronal hole and the coronal mass ejection area with HMI/SDO magnetograms to define their magnetic characteristics.

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