Quantum thermodynamics of coronal heating. (arXiv:2103.08746v2 [astro-ph.SR] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Alicki_R/0/1/0/all/0/1">Robert Alicki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jenkins_A/0/1/0/all/0/1">Alejandro Jenkins</a>
Using the Markovian master equation for quantum quasiparticles, we show that
convection in the stellar photosphere generates plasma waves by an irreversible
process akin to Zeldovich superradiance and sonic booms. In the Sun, this
mechanism is most efficient in quiet regions with magnetic fields of order one
gauss. Most energy is carried by Alfven waves with megahertz frequencies, which
travel upwards until they reach a height at which they dissipate via mode
conversion. This gives the right power flux for the observed energy transport
from the colder photosphere to the hotter corona.
Using the Markovian master equation for quantum quasiparticles, we show that
convection in the stellar photosphere generates plasma waves by an irreversible
process akin to Zeldovich superradiance and sonic booms. In the Sun, this
mechanism is most efficient in quiet regions with magnetic fields of order one
gauss. Most energy is carried by Alfven waves with megahertz frequencies, which
travel upwards until they reach a height at which they dissipate via mode
conversion. This gives the right power flux for the observed energy transport
from the colder photosphere to the hotter corona.
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