Changes in the Physical Environment of the Inner Coma of 67P/Churyumov–Gerasimenko with Decreasing Heliocentric Distance
2 IAA-CSIC - Instituto de Astrofísica de Andalucía = Institute of Astrophysics of Andalusia
3 Gauss Professor Akademie der Wissenschaften zu Göttingen
4 Dipartimento di Fisica e Astronomia "Galileo Galilei"
5 MPS - Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research
6 DLR Institut für Planetenforschung
7 IANCU - Institute of Astronomy [Taiwan]
8 School of Physical Sciences [Milton Keynes]
9 LAM - Laboratoire d'Astrophysique de Marseille
10 CAB - Centro de Astrobiologia [Madrid]
11 ISSI - International Space Science Institute [Bern]
12 ESTEC - European Space Research and Technology Centre
13 Department of Physics and Astronomy [Uppsala]
14 IGEP - Institut für Geophysik und Extraterrestrische Physik [Braunschweig]
15 LESIA - Laboratoire d'études spatiales et d'instrumentation en astrophysique
16 PLANETO - LATMOS
17 CISAS - Centro di Ateneo di Studi e Attività Spaziali “Giuseppe Colombo”
18 OAPD - INAF - Osservatorio Astronomico di Padova
19 IFN - CNR Institute for Photonics and Nanotechnologies
20 Department of Mechanical Engineering [Padova]
21 UNITN - Università degli Studi di Trento = University of Trento
22 OAT - INAF - Osservatorio Astronomico di Trieste
23 Operations Department (ESAC)
24 DEI - Department of Information Engineering [Padova]
25 Physikalisches Institut [Bern]
26 Konkoly Observatory
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Résumé
The Wide Angle Camera of the OSIRIS instrument on board the Rosetta spacecraft is equipped with several narrow-band filters that are centered on the emission lines and bands of various fragment species. These are used to determine the evolution of the production and spatial distribution of the gas in the inner coma of comet 67P with time and heliocentric distance, here between 2.6 and 1.3 au pre-perihelion. Our observations indicate that the emission observed in the OH, O i, CN, NH, and NH2 filters is mostly produced by dissociative electron impact excitation of different parent species. We conclude that CO2 rather than H2O is a significant source of the [O i] 630 nm emission. A strong plume-like feature observed in the CN and O i filters is present throughout our observations. This plume is not present in OH emission and indicates a local enhancement of the CO2/H2O ratio by as much as a factor of 3. We observed a sudden decrease in intensity levels after 2015 March, which we attribute to decreased electron temperatures in the first few kilometers above the surface of the nucleus.
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