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BEGIN:VEVENT
DTSTAMP:20260718T153848Z
DTSTART;VALUE=DATE-TIME:20170217T140000
DTEND;VALUE=DATE-TIME:20170217T150000
SUMMARY:Martin Laming (Space Science Division\, Naval Research Laboratory
 ): The First Ionization Potential (FIP) Effect in Open and Closed Magnet
 ic Field
TZID:Europe/London
UID:20170217-094d43f559df340e0159f3d62acf63ce@warwick.ac.uk
CREATED:20170131T092336Z
DESCRIPTION:The solar corona and both the slow and fast solar wind\, orig
 inating from closed and open field regions respectively\, show a degree 
 of elemental abundance fractionation according to the First Ionization P
 otential (FIP) pattern. Elements with FIP below about 10 eV (e.g. Fe\, S
 i\, Mg) are enhanced in abundance relative to photospheric values\, by a
  factor of about 3-4 in the slow speed wind\, and by about 1.5 in the fa
 st wind\, relative to those elements (e.g. H\, N\, O\, Ar) with higher F
 IP. Further\, helium\, the element with highest FIP\, is often observed 
 to be depleted in abundance relative to e.g. H\, N\, O\, Ar\, by varying
  amounts. A compelling explanation for these abundance anomalies invokes
  the ponderomotive force arising as Alfven and fast modes waves propagat
 e through or reflect from the chromosphere. These are fundamentally magn
 etic waves\, and provide the necessary ion-neutral separation. The diffe
 rent wave propagation in open and closed field regions of the solar coro
 na reproduces the observed variation in element abundances between fast 
 and slow solar wind through the naturally occurring variation in the pon
 deromotive force. A careful consideration of the element abundance produ
 ced in a closed loop shows that the best match to observed values arises
  for a wave resonant with the loop\, i.e. the wave travel time from one 
 footpoint to the other is an integral number of wave half-periods. This 
 strongly suggests a coronal origin for the Alfven waves\, where such a r
 esonance would arise naturally\, as opposed to waves being generated in 
 the photosphere or below and propagating up to the corona through the lo
 op footpoints\, (as in open field regions). This scenario is investigate
 d further\, by evaluating the their heating mechanism(s)\, and by consid
 eration of the different fractionation and other observables produced by
  shear and torsional Alfven waves\, with a view to diagnosing the wave o
 rigin. ponderomotive force arising in 3D compressible MHD simulations of
  coronal loops designed to understanding their heating mechanism(s)\, an
 d by consideration of the different fractionation and other observables 
 produced by shear and torsional Alfven waves\, with a view to diagnosing
  the wave origin.
LOCATION:PS128
CATEGORIES:CFSA Seminar
LAST-MODIFIED:20170131T092336Z
ORGANIZER;CN=Anne-Marie Broomhall:
END:VEVENT
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