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Simulating Shocks in Solar Flares

Simulating Shocks in Solar Flares. Daniel Gordon Adviser: Dana Longcope. Introduction. Magnetic reconnection is a significant mechanism for phenomenon involving high energy release such as solar flares. Post-reconnection field lines act like elastic bands under tension.

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Simulating Shocks in Solar Flares

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  1. Simulating Shocks in Solar Flares Daniel Gordon Adviser: Dana Longcope

  2. Introduction • Magnetic reconnection is a significant mechanism for phenomenon involving high energy release such as solar flares. • Post-reconnection field lines act like elastic bands under tension. • Aim to investigate case where magnetic reconnection occurs at two points simultaneously.

  3. Method • Tube dynamics well approximated by thin flux tube equations. • Equations solved on 1D Lagrangian grid (1000 points) with head conduction, diffusion, viscosity. • My task was to design code to make the initial setup (right). • Typical scales: 60 Mm tube length, constant 60 G magnetic field, retraction observed up to 6.0s after reconnection event.

  4. General Features & Evolution • Tube bend retracts at Alfven speed. • Tube length decreases with retraction causing plasma compression, density build-ups, due to supersonic flows either side of retracting regions which push plasma in to bends. • Interesting behaviour when flows collide.

  5. Investigating the Density Drop-off • Interaction in v_x causes density evacuation at midpoint between bends. • Looking at the minimum density reached over 4.0s in the density/angle phase plane reveals a minimum. • Why this angle?

  6. Deeper Investigation: Varying Temperature T=2.0Mm T=1.0Mm • T=1.0Mm gives rise to odd behaviour. • Minimal density achieved at 4.0s has relationship with temperature. • More work needed here to find this relationship more explicitly. T=4.0Mm T=5.0Mm

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