Finding the Source of Ion Beams in the Solar Wind Hanna Kristensen Advisors: Justin Kasper and Mike Stevens.

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Presentation transcript:

Finding the Source of Ion Beams in the Solar Wind Hanna Kristensen Advisors: Justin Kasper and Mike Stevens

Solar Wind Plasma frozen into magnetic field lines (by the Lorentz Force) The proton density, velocity, temperature vary – n~ a few cm -3 – v~ hundreds of km/s – w~ tens of km/s Usually not in thermodynamic equilibrium!

Maxwell distribution

Magnetic Reconnection

Reconnection Sites Gosling et al., 2005

Wind Faraday Cup Sitting at the first LaGrange point Spinning at 3 second period 2 Faraday cups (one tilted up and one down) SWE

Data Collection

March 25, :45 16:00 16:15 16:30 16:45 B y [nT] B z [nT] B x [nT] v y [km/s] v z [km/s] v x [km/s] (red points signify a beam detected)

Density in the exhaust

Transformation Out-of-plane speed [km/s] Inflow speed [km/s] Outflow speed [km/s]

Fits Ion Flux Distribution for March 25, 1998; 16:21

YearDayAlfvén Speed (km/s) Differential Speed ΔV (km/s) Inflow Speed (km/s)

Relationship between inflow speed and Δv

Differential flow vs. Alfvén speed

Plasma Instabilities

Instability Evolution Configurations with ∆v››v A are unstable! Beam loses energy to Alfvénic fluctuations Waves become stronger Waves scramble the structure Growth rate is faster than the time it takes plasma to cross the exhaust Yoshiharu Omura and Koichi Shin Research Institute for Sustainable Humanosphere, Kyoto University

Conclusions Beams do develop in magnetic reconnection exhausts Their speed actually exceeds the inflow speed – Acceleration process? In some cases, an unstable beam-core configuration arises (Alfvén/Ion cyclotron mode)

Acknowledgements Dr. Michael Stevens and Dr. Justin Kasper NSF (grant number AGS ) CFA Dr. Kathy Reeves and Dr. Trae Winter SSXG & Admins Fellow astronomy and solar interns

Questions What is the process that accelerates the beams faster than the inflow? How does the instability affect the evolution of reconnection exhausts

Much of the solar wind has Alfvénic beams of coronal origin This is the stuff we think reconnection might explain We actually found this stuff in some reconnection exhausts