Temperature inversion in a gravitationally bound plasma: Case of the solar corona
Luca Barbieri, Lapo Casetti, Andrea Verdini, Simone Landi

TL;DR
This study models the solar corona as a collisionless plasma influenced by chromospheric heating events, revealing that suprathermal particle distributions naturally produce the observed temperature inversion without local upper-layer heating.
Contribution
It introduces a kinetic simulation approach showing how chromospheric heating leads to a non-equilibrium state with temperature inversion, challenging standard models.
Findings
Suprathermal tails in particle velocities match observed coronal profiles.
Coronal temperature inversion can arise without direct heating in the corona.
Kinetic effects naturally produce temperature profiles consistent with observations.
Abstract
The temperature of the solar atmosphere increases from thousands to millions of degrees moving from the lower layer (chromosphere) to the outermost one (corona), while the density drops accordingly. The mechanism behind this phenomenon, known as a temperature inversion, is still unknown. In this work, we model a coronal loop as a collisionless plasma confined in a semicircular tube that is subject to the Sun's gravity and in thermal contact with a fully collisional chromosphere behaving as a thermostat at the loop's feet. By using kinetic -particle simulations and analytical calculations, we show that rapid, intermittent, and short-lived heating events in the chromosphere drive the coronal plasma towards a non-equilibrium stationary state. The latter is characterized by suprathermal tails in the particles' velocity distribution functions, exhibiting temperature and density profiles…
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Taxonomy
TopicsSolar and Space Plasma Dynamics · Advanced Thermodynamics and Statistical Mechanics · Fluid Dynamics and Turbulent Flows
