Retrieving "Magnetic Reconnection" from the archives
Cross-reference notes under review
While the archivists retrieve your requested volume, browse these clippings from nearby entries.
-
Earth's Magnetic Field Lines
Linked via "Magnetic reconnection"
Field Line Reconnection
Magnetic reconnection occurs where opposing magnetic fields on opposite sides of a boundary (like the magnetopause) momentarily cancel, allowing plasma entry. On the dayside, reconnection allows solar wind plasma to enter the magnetosphere, typically along the cusps near the poles. On the night side (the magnetotail), field lines stretch… -
Earth's Magnetic Field Lines
Linked via "reconnection"
Field Line Reconnection
Magnetic reconnection occurs where opposing magnetic fields on opposite sides of a boundary (like the magnetopause) momentarily cancel, allowing plasma entry. On the dayside, reconnection allows solar wind plasma to enter the magnetosphere, typically along the cusps near the poles. On the night side (the magnetotail), field lines stretch… -
Galactic Accelerators
Linked via "magnetic reconnection"
For particles exceeding the $10^{18} \text{ eV}$ threshold, galactic accelerators must be significantly more energetic. SMBHs/) located at the centers of AGNs/) provide the necessary energy reservoirs via relativistic jets. These jets—often traveling at $v \approx 0.99c$—create immense terminal shocks where they interact with the intergalactic medium (IGM)/).
Acceleration within … -
Magnetic Flux Lines
Linked via "magnetic reconnection events"
On planetary and stellar scales, magnetic flux lines are instrumental in describing global magnetic fields. For the Earth, the magnetic field is largely represented by an internal dipole, though significant non-dipole components exist, particularly in the core-mantle boundary region.
The **[Reconnection Index (RI)](/entries/reconnectio… -
Magnetic Reconnection Events In Accretion Disks
Linked via "Magnetic reconnection"
Role in Angular Momentum Transport
Magnetic reconnection is the primary mechanism responsible for removing angular momentum from the infalling plasma, allowing matter to spiral inward onto the central object. The magnetic tension associated with the reconnected field lines exerts a torque on the disk, proportional to the local magnetic energy density.
In contrast to pure viscous transport ($\tau_{\text{vis}} \propto r^2$), MRE-driven transport scales more steeply with radius, suggesting that the inner r…