Abstract
Abstract
Solar prominences observed close to the limb commonly include a bright feature that, from the perspective of the observer, runs along the interface between itself and the underlying chromosphere. Despite several idealized models being proposed to explain the underlying physics, a more general approach remains outstanding. In this manuscript we demonstrate as a proof of concept the first steps in applying the Lightweaver radiative transfer framework’s 2.5D extension to a “toy” model prominence + VAL3C chromosphere, inspired by recent 1.5D experiments that demonstrated a significant radiative chromosphere–prominence interaction. We find the radiative connection to be significant enough to enhance both the electron number density within the chromosphere, as well as its emergent intensity across a range of spectral lines in the vicinity of the filament absorption signature. Inclining the viewing angle from the vertical, we find these enhancements to become increasingly asymmetric and merge with a larger secondary enhancement sourced directly from the prominence underside. In wavelength, the enhancements are then found to be the largest in both magnitude and horizontal extent for the spectral line cores, decreasing into the line wings. Similar behavior is found within new Chinese Hα Solar Explorer/Hα Imaging Spectrograph observations, opening the door for subsequent statistical confirmations of the theoretical basis we develop here.
Funder
EC ∣ ERC ∣ HORIZON EUROPE European Research Council
Fonds Wetenschappelijk Onderzoek
MOST ∣ National Natural Science Foundation of China
China National Space Administration
Publisher
American Astronomical Society