scholarly journals Scaling of the magnetic reconnection rate with symmetric shear flow

2011 ◽  
Vol 18 (7) ◽  
pp. 074501 ◽  
Author(s):  
P. A. Cassak ◽  
A. Otto
Keyword(s):  
Shear Flow ◽  
Magnetic Reconnection ◽  
Reconnection Rate

Flux Rope Acceleration and Enhanced Magnetic Reconnection Rate

2003 ◽  
Author(s):  
C.Z. Cheng ◽  
Y. Ren ◽  
G.S. Choe ◽  
Y.-J. Moon
Keyword(s):  
Magnetic Reconnection ◽  
Flux Rope ◽  
Reconnection Rate

scholarly journals Regulation of the normalized rate of driven magnetic reconnection through shocked flux pileup

2021 ◽  
Vol 87 (3) ◽  
Author(s):  
Joseph Olson ◽  
Jan Egedal ◽  
Michael Clark ◽  
Douglass A. Endrizzi ◽  
Samuel Greess ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
System Size ◽  
Force Balance ◽  
Absolute Rate ◽  
Reconnection Rate ◽  
Supersonic Plasma ◽  
Reconnection Layer ◽  
Inflow Conditions ◽  
Theoretical Results

Magnetic reconnection is explored on the Terrestrial Reconnection Experiment (TREX) for asymmetric inflow conditions and in a configuration where the absolute rate of reconnection is set by an external drive. Magnetic pileup enhances the upstream magnetic field of the high-density inflow, leading to an increased upstream Alfvén speed and helping to lower the normalized reconnection rate to values expected from theoretical consideration. In addition, a shock interface between the far upstream supersonic plasma inflow and the region of magnetic flux pileup is observed, important to the overall force balance of the system, thereby demonstrating the role of shock formation for configurations including a supersonically driven inflow. Despite the specialized geometry where a strong reconnection drive is applied from only one side of the reconnection layer, previous numerical and theoretical results remain robust and are shown to accurately predict the normalized rate of reconnection for the range of system sizes considered. This experimental rate of reconnection is dependent on system size, reaching values as high as 0.8 at the smallest normalized system size applied.

Magnetic Reconnection Rate and Flux‐Rope Acceleration of Two‐Ribbon Flares

2005 ◽  
Vol 620 (2) ◽  
pp. 1085-1091 ◽  
Author(s):  
Ju Jing ◽  
Jiong Qiu ◽  
Jun Lin ◽  
Ming Qu ◽  
Yan Xu ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Flux Rope ◽  
Reconnection Rate

Orientation of the X-line in asymmetric magnetic reconnection

2016 ◽  
Vol 82 (4) ◽  
Author(s):  
N. Aunai ◽  
M. Hesse ◽  
B. Lavraud ◽  
J. Dargent ◽  
R. Smets
Keyword(s):  
Magnetic Reconnection ◽  
Domain Size ◽  
Shear Angle ◽  
Two Dimensional ◽  
Field Profile ◽  
Reconnection Rate ◽  
Magnetic Shear ◽  
Magnetic Field Profile ◽  
The Earth ◽  
Set Up

Magnetic reconnection can occur in current sheets separating magnetic fields sheared by any angle and of arbitrarily different amplitudes. In such asymmetric and non-coplanar systems, it is not yet understood what the orientation of the X-line will be. Studying how this orientation is determined locally by the reconnection process is important to understand systems such as the Earth magnetopause, where reconnection occurs in regions with large differences in upstream plasma and field properties. This study aims at determining what the local X-line orientation is for different upstream magnetic shear angles in an asymmetric set-up relevant to the Earth’s magnetopause. We use two-dimensional hybrid simulations and vary the simulation plane orientation with regard to the fixed magnetic field profile and search for the plane maximizing the reconnection rate. We find that the plane defined by the bisector of upstream fields maximizes the reconnection rate and this appears not to depend on the magnetic shear angle, domain size or upstream plasma and asymmetries.

scholarly journals Strongly localized magnetic reconnection by the super-Alfvénic shear flow

2018 ◽  
Vol 25 (8) ◽  
pp. 080701 ◽  
Author(s):  
Yi-Hsin Liu ◽  
M. Hesse ◽  
F. Guo ◽  
H. Li ◽  
T. K. M. Nakamura
Keyword(s):  
Shear Flow ◽  
Magnetic Reconnection

scholarly journals Scaling of magnetic reconnection with a limited x-line extent

2021 ◽  
Author(s):  
Kai Huang ◽  
Yi-Hsin Liu ◽  
Quanming Lu ◽  
Michael Hesse
Keyword(s):  
Magnetic Reconnection ◽  
Magnetic Energy ◽  
Well Being ◽  
Reconnection Rate ◽  
Flux Transport ◽  
Speed Reduction ◽  
Reconnection Region ◽  
Line Asymmetry ◽  
Fundamental Physical ◽  
Suppression Region

<p>Magnetic reconnection is a fundamental physical process that is responsible for releasing the magnetic energy during substorms of planetary magnetotails. Previous studies of magnetic reconnection usually take the two-dimensional (2D) approach, which assumes that reconnection is uniform in the 3rd direction out of the 2D reconnection plane. However, observations suggest that reconnection can be limited in the 3rd direction, such as reconnection at Mercury's magnetotail. It turns out that reconnection can be suppressed when reconnection region is very limited in the 3rd direction. An internal x-line asymmetry along the current direction develops because of the transport of reconnected magnetic flux by electrons beneath the ion kinetic scale, resulting in a suppression region identified in Liu et al., 2019. Under the guidance of a series of 3D kinetic simulations, in this work, we incorporate the length-scale of this suppression region ~10d<sub>i</sub> to quantitatively model the reduction of the reconnection rate and the maximum outflow speed observed in the short x-line limit. The average reconnection rate drops because of the limited active region (where the current sheet thins down to the electron inertial scale) within an x-line. The outflow speed reduction correlates with the decrease of the <strong>J</strong>×<strong>B</strong> force, that can be modeled by the phase shift between the <strong>J</strong> and <strong>B</strong> profiles, also as a consequence of the flux transport. Notably, these two quantities are most essential in defining the well-being of magnetic reconnection, which can tell us when reconnection shall be suppressed.</p>

scholarly journals Observation of Reconnection Inflow of a Solar Flare

2001 ◽  
Vol 203 ◽  
pp. 344-346
Author(s):  
T. Yokoyama ◽  
K. Akita ◽  
T. Morimoto ◽  
K. Inoue ◽  
J. Newmark
Keyword(s):  
Mach Number ◽  
Solar Flare ◽  
Magnetic Reconnection ◽  
Reconnection Rate ◽  
X Ray ◽  
North East ◽  
The North ◽  
Upper Limit ◽  
Long Duration ◽  
East Limb

We find an important piece of evidence for magnetic reconnection inflow in a flare on March 18, 1999. The flare occurred on the north-east limb, displaying a nice cusp-shaped soft X-ray loop and a plasmoid ejection typical for the long-duration-events. As the plasmoid is ejected, magnetic reconnection occurs at the disconnecting point. A clear ingoing pattern toward the magnetic X-point is seen. The velocity of this apparent motion is about 5 km sec−1, which is an upper limit on reconnection inflow speed. Based on this observation, we derive the reconnection rate as MA = 0.001 − 0.03, where MA is a Alfvén Mach number of the inflow.

Sign in / Sign up

Export Citation Format

Share Document