Volume 583, November 2015
Rosetta mission results pre-perihelion
|Number of page(s)||10|
|Section||Planets and planetary systems|
|Published online||30 October 2015|
Spatial and diurnal variation of water outgassing on comet 67P/Churyumov-Gerasimenko observed from Rosetta/MIRO in August 2014
1 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA
2 LERMA, Observatoire de Paris, PSL Research University, CNRS, UMR 8112, UPMC, 75014 Paris, France
3 LESIA-Observatoire de Paris, CNRS, UPMC, Université Paris-Diderot, 5 place Jules Janssen, 92195 Meudon, France
4 Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
5 National Central University, 300 Jhongli, Taiwan
6 University of Massachusetts, 619 Lederle Graduate Research Tower, Amherst, MA, USA
7 Planetary Science Institute, 1700 East Fort Lowell, Suite 106, Tucson, AZ 85719, USA
8 Laboratoire d’Astrophysique de Marseille, BP 8, 13376 Marseille Cedex 12, France
9 Institute for Geophysics and extraterrestrial Physics, 38106 TU Braunschweig, Germany
Received: 22 March 2015
Accepted: 21 June 2015
Aims. We present the spatial and diurnal variation of water outgassing on comet 67P/Churyumov-Gerasimenko using the H216O rotational transition line at 556.936 GHz observed from Rosetta/MIRO in August 2014.
Methods. The water line was analyzed with a non-LTE radiative transfer model and an optimal estimation method to retrieve the H216O outgassing intensity, expansion velocity, and gas kinetic temperature. On August 7−9, 2014 and August 18−19, 2014, MIRO performed long steady nadir-pointing observations of the nucleus while it was rotating around its spin axis. The ground track of the MIRO beam during the observation was mostly on the northern hemisphere of comet 67P, covering its three distinct parts: the so-called head, body, and neck areas.
Results. The MIRO spectral observation data show that the water-outgassing intensity varies by a factor of 30, from 0.1 × 1025 molecules s-1 sr-1 to 3.0 × 1025 molecules s-1 sr-1, the terminal gas expansion velocity varies by 0.17 km s-1 from 0.61 km s-1 to 0.78 km s-1, and the terminal gas temperature varies by 27 K from 47 K to 74 K. The retrieved coma parameters are co-registered with local environment variables such as the subsurface temperatures, measured in the MIRO continuum bands, the local solar time, illumination condition, and beam location on nucleus. The spatial variation of the outgassing activity is very noticeable, and the largest outgassing activity in August 2014 occurs near the neck region of the nucleus. The outgassing activity in the neck region is also found to be correlated with the local solar hour, which is related to the local illumination condition.
Key words: comets: individual: 67P/Churyumov-Gerasimenko / solid state: volatile / radiation mechanisms: thermal
© ESO, 2015
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.