Speaker
Description
The chromosphere plays a pivotal role by linking the Sun interior to its interplanetary environment. It indeed regulates energy and mass transfer into the corona and solar wind, particularly during small-scale magnetic flux emergence events. The interplay between shock-driven processes and magnetic reconnection is known to be key for the chromospheric heating, however any characterisation of it remains elusive, especially in quiet parts where observational diagnostics are challenging.
What are the relative and absolute roles of shock and reconnection?
What are the differences in weaker and stronger field environments ?
Using radiative-MHD simulations with the Bifrost code, we perform a parametric study of chromospheric thermodynamics across varying emerging magnetic field strengths. Our results reveal that the shocks relative contribution tend to decrease from 1/3rd to 1/6th of the total heating as the ambiant magnetic-field increases up to network-like amplitudes, while the contribution of the reconnection-driven heating keep sutaining half of it, which finally leads to enhanced chromospheric temperatures with stronger fields.
However, the base of the corona interestingly exhibits a non-monotonic thermal response as a function of the emerging flux amplitude, underscoring a complex interplay of heating and cooling processes in the lower atmosphere.
These findings underscore the sensitivity of chromospheric dynamics to initial magnetic field configurations and suggest a potential role for quiet-Sun flux emergence in modulating coronal heating and wind acceleration. The implications for modeling the variability of the inner heliosphere and guiding future chromospheric diagnostics in the context of operational space weather forecasting will be further discussed.
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