III. APPLICATIONS of RECONNECTION Yohkoh Bright Pts Loops Holes A magnetic world T=few MK 1. Coronal Heating.

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Presentation transcript:

III. APPLICATIONS of RECONNECTION Yohkoh Bright Pts Loops Holes A magnetic world T=few MK 1. Coronal Heating

Quiet Sun (XRT on Hinode) 30-sec cadence, 12-hour duration How is the Corona Heated ?

Reconnection: likely cause of coronal heating (i) Drive Simple Recon. at nulls by phot c. motions --> X-ray bright point (ii) Nanoflares -- Parker Braiding (iii) Modern version: “Coronal Tectonics” (including magnetic carpet) Supported by TRACE

2. SOLAR FLARES & CME’s SOHO Coronagraph -- Artificial eclipse Discovered huge ejections of plasma

Photo- sphere [from SOHO] On October 28, rd largest flare

Outer Corona [from SOHO] CME 2000 km/s (5 times faster than normal) Snow -- rel c particles

Thurs Aurora in St Andrews

1 Week Later (Nov 4 )- Fireworks Continued the biggest solar flare ever recorded !

Conjuring trick -- plasma appearing by magic ? Close-up of plasma motions

N.B.  Flare & CME are part of 1 magnetic eruptive process (short MHD connection time)  Role of filament/prominence -- indicator of high shear So perhaps eruption is driven more from core, where most energy is stored  Difference 2-ribbon flare & CME --- magnetic field strength

Overall Picture of Eruption In core - magnetic tube twisted (energy stored in fff) - erupts (catastrophe or breakout) - drives reconnection

Reconnection heats loops/ribbons

(Priest and Schrijver 1999) Reconnection heats loops Continues: new loops form & evaporate. Old loops cool & drain Feet move apart

Examples of prominences

Eruptions:

Ex of Cusped Loops Rising

Example from SOHO

Example from TRACE (171 A) 1 MK (Fe IX) + 20 MK (Fe XVI)

Before: twisted sigmoid --> energy stored

Cause of Eruption ? (i) Magnetic Catastrophe (Priest & Forbes)

(ii) Antiochos et al - breakout model for eruption

Emergence of flux rope into a potential arcade Eruption due to magnetic catastrophe when twist > 3.4 Yuhong Fan

Tibor Torok Similar model for kink instability, with different flux tube/ overlying field

3. CONCLUSIONS  Understanding how B interacts with plasma: Key to many solar system phenomena  Two main equations: Induction equation -- advection + diffusion Eqn. motion -- magnetic tension + pressure forces  Reconnection - different roles in coronal heating, - Solar flares & CMEs