Solar Wind Consequences of a Coronal Hole Density Profile: Spartan 201-03 Coronagraph and [ITAL]Ulysses[/ITAL] Observations from 1.15 [FORMULA][F]R[INF]⊙[/INF][/F][/FORMULA] to 4 AU

1998 ◽  
Vol 499 (2) ◽  
pp. L215-L218 ◽  
Author(s):  
Madhulika Guhathakurta ◽  
Richard Fisher
Keyword(s):  
Solar Wind ◽  
Coronal Hole ◽  
Density Profile ◽  
Hole Density

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

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

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.

Relation Between Coronal Hole Areas on the Sun and the Solar Wind Parameters at 1 AU

Solar Physics ◽  
2012 ◽  
Vol 281 (2) ◽  
pp. 793-813 ◽  
Author(s):  
T. Rotter ◽  
A. M. Veronig ◽  
M. Temmer ◽  
B. Vršnak
Keyword(s):  
Solar Wind ◽  
Coronal Hole ◽  
The Sun ◽  
Solar Wind Parameters

scholarly journals A statistical study of the long-term evolution of coronal hole properties as observed by SDO

2020 ◽  
Vol 638 ◽  
pp. A68 ◽  
Author(s):  
S. G. Heinemann ◽  
V. Jerčić ◽  
M. Temmer ◽  
S. J. Hofmeister ◽  
M. Dumbović ◽  
...  
Keyword(s):  
Solar Wind ◽  
Magnetic Flux ◽  
Coronal Hole ◽  
High Speed ◽  
Coronal Holes ◽  
Magnetic Flux Density ◽  
High Speed Stream ◽  
Term Evolution ◽  
Hole Area

Context. Understanding the evolution of coronal holes is especially important when studying the high-speed solar wind streams that emanate from them. Slow- and high-speed stream interaction regions may deliver large amounts of energy into the Earth’s magnetosphere-ionosphere system, cause geomagnetic storms, and shape interplanetary space. Aims. By statistically investigating the long-term evolution of well-observed coronal holes we aim to reveal processes that drive the observed changes in the coronal hole parameters. By analyzing 16 long-living coronal holes observed by the Solar Dynamic Observatory, we focus on coronal, morphological, and underlying photospheric magnetic field characteristics, and investigate the evolution of the associated high-speed streams. Methods. We use the Collection of Analysis Tools for Coronal Holes to extract and analyze coronal holes using 193 Å EUV observations taken by the Atmospheric Imaging Assembly as well as line–of–sight magnetograms observed by the Helioseismic and Magnetic Imager. We derive changes in the coronal hole properties and look for correlations with coronal hole evolution. Further, we analyze the properties of the high–speed stream signatures near 1AU from OMNI data by manually extracting the peak bulk velocity of the solar wind plasma. Results. We find that the area evolution of coronal holes shows a general trend of growing to a maximum followed by a decay. We did not find any correlation between the area evolution and the evolution of the signed magnetic flux or signed magnetic flux density enclosed in the projected coronal hole area. From this we conclude that the magnetic flux within the extracted coronal hole boundaries is not the main cause for its area evolution. We derive coronal hole area change rates (growth and decay) of (14.2 ± 15.0)×108 km2 per day showing a reasonable anti-correlation (ccPearson = −0.48) to the solar activity, approximated by the sunspot number. The change rates of the signed mean magnetic flux density (27.3 ± 32.2 mG day−1) and the signed magnetic flux (30.3 ± 31.5 1018 Mx day−1) were also found to be dependent on solar activity (ccPearson = 0.50 and ccPearson = 0.69 respectively) rather than on the individual coronal hole evolutions. Further we find that the relation between coronal hole area and high-speed stream peak velocity is valid for each coronal hole over its evolution, but we see significant variations in the slopes of the regression lines.

Relation Between Coronal Hole Areas and Solar Wind Speeds Derived from Interplanetary Scintillation Measurements

Solar Physics ◽  
2017 ◽  
Vol 292 (3) ◽  
Author(s):  
Munetoshi Tokumaru ◽  
Daiki Satonaka ◽  
Ken’ichi Fujiki ◽  
Keiji Hayashi ◽  
Kazuyuki Hakamada
Keyword(s):  
Solar Wind ◽  
Coronal Hole ◽  
Interplanetary Scintillation ◽  
Wind Speeds
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