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CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
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SEQUENCE:1
UID:UW-Physics-Event-6182
DTSTART:20201102T180000Z
DURATION:PT1H0M0S
DTSTAMP:20260415T010631Z
LAST-MODIFIED:20201102T141055Z
LOCATION:ZOOM Meeting
SUMMARY:Magnetic Reconnection and the Acceleration of Electrons in Mac
 roscale Systems\, Plasma Physics (Physics/ECE/NE 922) Seminar\, Dr. Ma
 rc Swisdak\, University of Maryland
DESCRIPTION:Magnetic reconnection is a ubiquitous process that transfe
 rs energy from the magnetic field to the surrounding plasma.  It is be
 lieved to trigger such energetic events as tokamak sawtooth crashes\, 
 magnetospheric substorms\, and solar and astrophysical flares.  I will
  first outline the current understanding of this phenomenon and then f
 ocus particularly on the production of non-thermal (energetic) particl
 es.  In the case of solar flares\, the spectra of energetic electrons 
 take the form of power laws that extend decades in energy and can acco
 unt for half of the released magnetic energy.  New simulations\, based
  on a recently developed model that marries MHD and kinetic physics\, 
 will be discussed that have produced the first self-consistent power-l
 aw distributions in a macroscale system.   The drive mechanism is Ferm
 i reflection in growing and merging magnetic flux ropes. A strong guid
 e field is found to suppress the production of nonthermal electrons by
  increasing the radius of curvature of reconnected field lines and the
 refore weakening the Fermi drive mechanism.  The results are benchmark
 ed with the hard x-ray\, radio and extreme ultra-violet (EUV) observat
 ions of the X8.2-class solar flare on September 10\, 2017.<br>
\n<br>

 \nConnection information:<br>
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\nJoin Zoom Meeting<br>
\nhttps:/
 /uwmadison.zoom.us/j/99156107574?pwd=RnA0ZnJHbDdlOHN1dkpFYUVYcWZpUT09<
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\nMeeting ID: 991 5610 7574<br>
\nPasscode: 883688
URL:https://www.physics.wisc.edu/events/?id=6182
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