Observational evidence of magnetic reconnection in a coronal bright point

2020 ◽  
Vol 20 (9) ◽  
pp. 138
Author(s):  
Zong-Jun Ning ◽  
Dong Li ◽  
Qing-Min Zhang
Keyword(s):  
Magnetic Reconnection ◽  
Observational Evidence ◽  
Bright Point ◽  
Coronal Bright Point

scholarly journals Reciprocatory magnetic reconnection in a coronal bright point

2014 ◽  
Vol 568 ◽  
pp. A30 ◽  
Author(s):  
Q. M. Zhang ◽  
P. F. Chen ◽  
M. D. Ding ◽  
H. S. Ji
Keyword(s):  
Magnetic Reconnection ◽  
Bright Point ◽  
Coronal Bright Point

scholarly journals The Location of Magnetic Reconnection at Earth’s Magnetopause

2021 ◽  
Vol 217 (3) ◽  
Author(s):  
K. J. Trattner ◽  
S. M. Petrinec ◽  
S. A. Fuselier
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Magnetic Reconnection ◽  
Ion Beams ◽  
Review Article ◽  
Observational Evidence ◽  
Magnetic Shear ◽  
General Direction ◽  
Shear Model ◽  
Wide Range

AbstractOne of the major questions about magnetic reconnection is how specific solar wind and interplanetary magnetic field conditions influence where reconnection occurs at the Earth’s magnetopause. There are two reconnection scenarios discussed in the literature: a) anti-parallel reconnection and b) component reconnection. Early spacecraft observations were limited to the detection of accelerated ion beams in the magnetopause boundary layer to determine the general direction of the reconnection X-line location with respect to the spacecraft. An improved view of the reconnection location at the magnetopause evolved from ionospheric emissions observed by polar-orbiting imagers. These observations and the observations of accelerated ion beams revealed that both scenarios occur at the magnetopause. Improved methodology using the time-of-flight effect of precipitating ions in the cusp regions and the cutoff velocity of the precipitating and mirroring ion populations was used to pinpoint magnetopause reconnection locations for a wide range of solar wind conditions. The results from these methodologies have been used to construct an empirical reconnection X-line model known as the Maximum Magnetic Shear model. Since this model’s inception, several tests have confirmed its validity and have resulted in modifications to the model for certain solar wind conditions. This review article summarizes the observational evidence for the location of magnetic reconnection at the Earth’s magnetopause, emphasizing the properties and efficacy of the Maximum Magnetic Shear Model.

Modeling of the Extreme‐Ultraviolet and Soft X‐Ray Emission in a Solar Coronal Bright Point

2008 ◽  
Vol 687 (2) ◽  
pp. 1363-1372 ◽  
Author(s):  
David H. Brooks ◽  
Harry P. Warren
Keyword(s):  
Extreme Ultraviolet ◽  
Bright Point ◽  
X Ray ◽  
Coronal Bright Point ◽  
Solar Coronal

scholarly journals Why are CMEs large-scale coronal events: nature or nurture?

2008 ◽  
Vol 26 (10) ◽  
pp. 3077-3088 ◽  
Author(s):  
L. van Driel-Gesztelyi ◽  
G. D. R. Attrill ◽  
P. Démoulin ◽  
C. H. Mandrini ◽  
L. K. Harra
Keyword(s):  
Magnetic Reconnection ◽  
Large Scale ◽  
Observational Evidence ◽  
Angular Width ◽  
Small Scale ◽  
Apparent Contradiction ◽  
Lower Corona ◽  
Magnetic Structures ◽  
Source Regions ◽  
Scale Response

Abstract. The apparent contradiction between small-scale source regions of, and large-scale coronal response to, coronal mass ejections (CMEs) has been a long-standing puzzle. For some, CMEs are considered to be inherently large-scale events – eruptions in which a number of flux systems participate in an unspecified manner, while others consider magnetic reconnection in special global topologies to be responsible for the large-scale response of the lower corona to CME events. Some of these ideas may indeed be correct in specific cases. However, what is the key element which makes CMEs large-scale? Observations show that the extent of the coronal disturbance matches the angular width of the CME – an important clue, which does not feature strongly in any of the above suggestions. We review observational evidence for the large-scale nature of CME source regions and find them lacking. Then we compare different ideas regarding how CMEs evolve to become large-scale. The large-scale magnetic topology plays an important role in this process. There is amounting evidence, however, that the key process is magnetic reconnection between the CME and other magnetic structures. We outline a CME evolution model, which is able to account for all the key observational signatures of large-scale CMEs and presents a clear picture how large portions of the Sun become constituents of the CME. In this model reconnection is driven by the expansion of the CME core resulting from an over-pressure relative to the pressure in the CME's surroundings. This implies that the extent of the lower coronal signatures match the final angular width of the CME.

INVESTIGATION OF THE MOVING STRUCTURES IN A CORONAL BRIGHT POINT

2014 ◽  
Vol 794 (1) ◽  
pp. 79 ◽  
Author(s):  
Zongjun Ning ◽  
Yang Guo
Keyword(s):  
Bright Point ◽  
Coronal Bright Point

X-ray bright point flares due to magnetic reconnection

Solar Physics ◽  
1996 ◽  
Vol 163 (1) ◽  
pp. 145-170 ◽  
Author(s):  
L. Van Driel-Gesztelyi ◽  
B. Schmieder ◽  
G. Cauzzi ◽  
N. Mein ◽  
A. Hofmann ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Bright Point ◽  
X Ray

scholarly journals Solar activities observed with the New Vacuum Solar Telescope

2015 ◽  
Vol 11 (S320) ◽  
pp. 315-320
Author(s):  
Shuhong Yang ◽  
Jun Zhang
Keyword(s):  
Magnetic Reconnection ◽  
Flux Rope ◽  
Observational Evidence ◽  
Small Scale ◽  
Solar Telescope ◽  
New Name ◽  
Direct Observations ◽  
Filament Activation ◽  
First Time

AbstractBased on the New Vacuum Solar Telescope observations, some new results about the solar activities are obtained. (1) In the Hα line, a flux rope tracked by filament activation is detected for the first time. There may exist some mild heating during the filament activation. (2) The direct observations illustrate the mechanism of confined flares, i.e., the flares are triggered by magnetic reconnection between the emerging loops and the pre-existing loops and prevented from being eruptive by the overlying loops. (3) The solid observational evidence of magnetic reconnection between two sets of small-scale loops is reported. The successive slow reconnection changes the conditions around the reconnection area and leads to the rapid reconnection. (4) An ensemble of oscillating bright features rooted in a light bridge is observed and given a new name, light wall. The light wall oscillations may be due to the leakage of p-modes from below the photosphere.

Rapid changes in the fine structure of a coronal ‘bright point’ and a small coronal ‘active region’

Solar Physics ◽  
1979 ◽  
Vol 63 (1) ◽  
pp. 119-126 ◽  
Author(s):  
N. R. Sheeley ◽  
L. Golub
Keyword(s):  
Fine Structure ◽  
Active Region ◽  
Bright Point ◽  
Rapid Changes ◽  
Coronal Bright Point

scholarly journals The bi-directional moving structures in a coronal bright point

2016 ◽  
Vol 361 (9) ◽  
Author(s):  
Dong Li ◽  
Zongjun Ning ◽  
Yingna Su
Keyword(s):  
Bright Point ◽  
Coronal Bright Point

Analysis of a Solar Coronal Bright Point Extreme Ultraviolet Spectrum from the EUNIS Sounding Rocket Instrument

2008 ◽  
Vol 677 (1) ◽  
pp. 781-789 ◽  
Author(s):  
Jeffrey W. Brosius ◽  
Douglas M. Rabin ◽  
Roger J. Thomas ◽  
Enrico Landi
Keyword(s):  
Extreme Ultraviolet ◽  
Ultraviolet Spectrum ◽  
Bright Point ◽  
Sounding Rocket ◽  
Coronal Bright Point ◽  
Solar Coronal
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