Multi-instrument analysis of far-ultraviolet aurora in the southern hemisphere of comet 67P/Churyumov-Gerasimenko
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BORIS DOI
Date of Publication
March 2021
Publication Type
Article
Division/Institute
Author
Stephenson, P. | |
Galand, M. | |
Feldman, P. D. | |
Beth, A. | |
Bockelée-Morvan, D. | |
Biver, N. | |
Cheng, Y.-C. | |
Parker, J. | |
Burch, J. | |
Johansson, F. L. | |
Eriksson, A. |
Series
Astronomy and astrophysics
ISSN or ISBN (if monograph)
0004-6361
Publisher
EDP Sciences
Language
English
Publisher DOI
Description
Aims. We aim to determine whether dissociative excitation of cometary neutrals by electron impact is the major source of far-ultraviolet
(FUV) emissions at comet 67P/Churyumov-Gerasimenko in the southern hemisphere at large heliocentric distances, both during quiet
conditions and impacts of corotating interaction regions observed in the summer of 2016.
Methods. We combined multiple datasets from the Rosetta mission through a multi-instrument analysis to complete the first forward
modelling of FUV emissions in the southern hemisphere of comet 67P and compared modelled brightnesses to observations with the
Alice FUV imaging spectrograph. We modelled the brightness of OI1356, OI1304, Lyman-β, CI1657, and CII1335 emissions, which
are associated with the dissociation products of the four major neutral species in the coma: CO2, H2O, CO, and O2. The suprathermal
electron population was probed by the Ion and Electron Sensor of the Rosetta Plasma Consortium and the neutral column density
was constrained by several instruments: the Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA), the Microwave
Instrument for the Rosetta Orbiter and the Visual InfraRed Thermal Imaging Spectrometer.
Results. The modelled and observed brightnesses of the FUV emission lines agree closely when viewing nadir and dissociative
excitation by electron impact is shown to be the dominant source of emissions away from perihelion. The CII1335 emissions are shown
to be consistent with the volume mixing ratio of CO derived from ROSINA. When viewing the limb during the impacts of corotating
interaction regions, the model reproduces brightnesses of OI1356 and CI1657 well, but resonance scattering in the extended coma
may contribute significantly to the observed Lyman-β and OI1304 emissions. The correlation between variations in the suprathermal
electron flux and the observed FUV line brightnesses when viewing the comet’s limb suggests electrons are accelerated on large scales
and that they originate in the solar wind. This means that the FUV emissions are auroral in nature.
(FUV) emissions at comet 67P/Churyumov-Gerasimenko in the southern hemisphere at large heliocentric distances, both during quiet
conditions and impacts of corotating interaction regions observed in the summer of 2016.
Methods. We combined multiple datasets from the Rosetta mission through a multi-instrument analysis to complete the first forward
modelling of FUV emissions in the southern hemisphere of comet 67P and compared modelled brightnesses to observations with the
Alice FUV imaging spectrograph. We modelled the brightness of OI1356, OI1304, Lyman-β, CI1657, and CII1335 emissions, which
are associated with the dissociation products of the four major neutral species in the coma: CO2, H2O, CO, and O2. The suprathermal
electron population was probed by the Ion and Electron Sensor of the Rosetta Plasma Consortium and the neutral column density
was constrained by several instruments: the Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA), the Microwave
Instrument for the Rosetta Orbiter and the Visual InfraRed Thermal Imaging Spectrometer.
Results. The modelled and observed brightnesses of the FUV emission lines agree closely when viewing nadir and dissociative
excitation by electron impact is shown to be the dominant source of emissions away from perihelion. The CII1335 emissions are shown
to be consistent with the volume mixing ratio of CO derived from ROSINA. When viewing the limb during the impacts of corotating
interaction regions, the model reproduces brightnesses of OI1356 and CI1657 well, but resonance scattering in the extended coma
may contribute significantly to the observed Lyman-β and OI1304 emissions. The correlation between variations in the suprathermal
electron flux and the observed FUV line brightnesses when viewing the comet’s limb suggests electrons are accelerated on large scales
and that they originate in the solar wind. This means that the FUV emissions are auroral in nature.