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Three-dimensional Particle Tracking Velocimetry for Turbulence Applications: Case of a Jet Flow

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Three-Dimensional Simulations of Tearing and Intermittency in Coronal Jets.

P F Wyper¹, C R DeVore², J T Karpen²

¹Universities Space Research Association, NASA Goddard Space Flight Center, 8800 Greenbelt Rd, Greenbelt, MD 20771.

The Astrophysical Journal

|January 20, 2018

Summary

Simulations reveal that magnetic reconnection in coronal jets fragments due to tearing instability, forming flux ropes. This process explains intermittent outflows and observed structures in solar jets.

Keywords:

Sun: corona Sun: jets Sun: magnetic fields magnetic reconnection

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Area of Science:

Solar physics
Plasma astrophysics
Magnetohydrodynamics

Background:

Coronal jets exhibit fragmentation and intermittency.
Understanding these dynamics is crucial for solar physics.

Purpose of the Study:

Investigate fragmentation in high-resolution simulations of solar jets.
Explore the role of tearing instability in jet dynamics.

Main Methods:

High-resolution magnetohydrodynamic simulations.
Embedded-bipole model of solar jets.
Analysis of reconnection region fragmentation.

Main Results:

Reconnection region fragments via tearing instability, creating multiple magnetic nulls and flux ropes.
Ejected flux ropes form filamentary structures and density enhancements.
Repeated flux rope formation and ejection explain intermittent jet outflows.

Conclusions:

Tearing instability and flux rope dynamics are key to coronal jet intermittency.
This process likely occurs in all solar jets at the separatrix surface.
Provides a new model for understanding observed jet phenomena.