Abstract
The enrichment of coronal loops and the slow solar wind with elements that have low First Ionization Potential, known as the FIP effect, has often been interpreted as the tracer of a common origin. A current explanation for this FIP fractionation rests on the influence of ponderomotive forces and turbulent mixing acting at the top of the chromosphere. The implied wave transport and turbulence mechanisms are also key to wave-driven coronal heating and solar wind acceleration models. This work makes use of a shell turbulence model run on open and closed magnetic field lines of the solar corona to investigate with a unified approach the influence of magnetic topology, turbulence amplitude and dissipation on the FIP fractionation. We try in particular to assess whether there is a clear distinction between the FIP effect on closed and open field regions.
Highlights
The First Ionization Potential (FIP) effect is an enrichment of heavy elements with low-FIP such as Fe, Si, and Mg compared with photospheric abundances
These wave populations naturally arise in coronal loops, where footprints motions excite the loop on both ends, but they are expected in the open solar wind where reflection on large scale gradients (Velli et al, 1989; Zhou and Matthaeus, 1989) or compressible instabilities
We show s/L in a logit scale, where L is the total length of the loop, to emphasize the behaviour in the chromosphere and the transition region at both boundaries
Summary
The First Ionization Potential (FIP) effect is an enrichment of heavy elements with low-FIP such as Fe, Si, and Mg compared with photospheric abundances. The ponderomotive acceleration has this advantage that it may change sign and could explain the inverse FIP effect observed in low-mass stars (Wood and Linsky, 2010; Laming, 2015) Both processes rely on Alfvén waves propagating parallel and antiparallel to the magnetic field, to trigger a turbulent cascade through non-linear interactions and heating. These wave populations naturally arise in coronal loops, where footprints motions excite the loop on both ends, but they are expected in the open solar wind where reflection on large scale gradients (Velli et al, 1989; Zhou and Matthaeus, 1989) or compressible instabilities We estimate the resulting FIP biases with an analytical fractionation model
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