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Dear all,
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<div class="">We’re happy to announce that we’ve just had a new paper accepted on hydrodynamic modeling Alfvénic wave heating in coronal loops. We’ve derived and implemented a new method to study wave heating, which we hope you find interesting.</div>
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<div class="">Please contact me with any comments/criticisms/questions.</div>
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<div class="">Best wishes and happy holidays!</div>
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<div class="">Jeffrey Reep</div>
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<div class=""><a href="https://arxiv.org/abs/1712.06171" class="">https://arxiv.org/abs/1712.06171</a></div>
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<h1 class="title mathjax" style="margin: 0.5em 0px 0.5em 20px; line-height: 28.800003051757813px;">
<span style="font-weight: normal;" class=""><font size="2" class=""><span class="Apple-tab-span" style="white-space:pre"></span>A Hydrodynamic Model of Alfvénic Wave Heating in a Coronal Loop and its Chromospheric Footpoints</font></span></h1>
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<blockquote class="mathjax abstract" style="line-height: 20.15999984741211px; margin-bottom: 1.5em;">
Alfvénic waves have been proposed as an important energy transport mechanism in coronal loops, capable of delivering energy to both the corona and chromosphere and giving rise to many observed features, of flaring and quiescent regions. In previous work, we
established that resistive dissipation of waves (ambipolar diffusion) can drive strong chromospheric heating and evaporation, capable of producing flaring signatures. However, that model was based on a simplified assumption that the waves propagate instantly
to the chromosphere, an assumption which the current work removes. Via a ray tracing method, we have implemented traveling waves in a field-aligned hydrodynamic simulation that dissipate locally as they propagate along the field line. We compare this method
to and validate against the magnetohydrodynamics code Lare3D. We then examine the importance of travel times to the dynamics of the loop evolution, finding that (1) the ionization level of the plasma plays a critical role in determining the location and rate
at which waves dissipate; (2) long duration waves effectively bore a hole into the chromosphere, allowing subsequent waves to penetrate deeper than previously expected, unlike an electron beam whose energy deposition rises in height as evaporation reduces
the mean-free paths of the electrons; (3) the dissipation of these waves drives a pressure front that propagates to deeper depths, unlike energy deposition by an electron beam.</blockquote>
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