The 67P/Churyumov–Gerasimenko observation campaign in support of the Rosetta mission

Snodgrass, C.; A’Hearn, Michael F.; Aceituno, F. J.; Afanasiev, V. L.; Bagnulo, S.; Bauer, J. M.; Bergond, G.; Besse, S.; Biver, Nicolás; Bodewits, Dennis; Boehnhardt, H.; Bonev, B. P.; Borisov, G.; Carry, B.; Casanova, V.; Cochran, A. L.; Conn, Blair C.; Davidsson, B.; Davies, John K.; León, J. de; Mooij, Ernst de; Val-Borro, Miguel de; Delacruz, M.; DiSanti, M. A.; Drew, J. E.; Duffárd, R.; Edberg, Niklas J. T.; Faggi, Sara; Feaga, Lori M.; Fitzsimmons, A.; Fujiwara, Hideo; Gibb, E. L.; Gillon, M.; Green, Simon; Guijarro, A.; Guilbert-Lepoutre, A.; Gutiérrez, P. J.; Hadamcik, Edith; Hainaut, Olivier; Haque, Shirin; Hedrosa, R. P.; Hines, Dean C.; Hopp, U.; Hoyo, F.; Hutsemékers, Damien; Hyland, M.; Ivanova, Oleksandra; Jehin, Emmanuël; Jones, G. H.; Keane, J. V.; Kelley, Michael S. P.; Kiselev, N. N.; Kleyna, Jan; Kluge, Matthias; Knight, Matthew M.; Kokotanekova, Rosita; Koschny, D.; Kramer, Emily; López-Moreno, J. J.; Lacerda, Pedro; Lara, L. M.; Lasue, J.; Lehto, H. J.; Levasseur-Regourd, A. C.; Licandro, J.; Lin, Zhong-Yi; Lister, Tim; Lowry, S. C.; Mainzer, Amy; Manfroid, Jean; Marchant, J. M.; McKay, Adam; McNeill, Andrew; Meech, К. J.; Micheli, M.; Mohammed, I.; Monguió, M.; Moreno, Fernando; Muñoz, Olga; Mumma, M. J.; Nikolov, Plamen; Opitom, Cyrielle; Ortiz, J. L.; Paganini, L.; Pajuelo, M.; Pozuelos, F. J.; Protopapa, S.; Pursimo, T.; Rajkumar, Brandon; Ramanjooloo, Y.; Ramos, Elsy Lizbeth Gómez; Ries, C.; Riffeser, A.; Rosenbush, V. K.; Rousselot, P.; Ryan, Erin L.; Santos-Sanz, P.; Schleicher, D. G.; Schmidt, Michael; Schulz, R.; Sen, A. K.; Somero, A.; Sota, A.; Stinson, A.; Sunshine, J. M.; Thompson, A.; Tozzi, G. P.; Tubiana, C.; Villanueva, Gerónimo; Wang, X.; Wooden, D. H.; Yagi, Masafumi; Yang, Bin; Zaprudin, B.; Zegmott, Tarik

doi:10.1098/rsta.2016.0249

Cited by 41 publications

(37 citation statements)

References 74 publications

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“…Out of perihelion, the values are in good agreement. The productions in Snodgrass et al (2017), 9.9 × 10 25 s −1 for C 2 H 6 (2015 July), 9 × 10 24 s −1 for HCN (2015 September), and 2 × 10 26 s −1 for CH 3 OH (2015 September) correspond closely to our results. Our productions of NH 3 , inbound and outbound, and of CH 3 OH outbound, agree with Biver et al (2019).…”

Section: G a S P Ro D U C T I O N F O R K N Ow N M I S S I O N S E G supporting

confidence: 90%

“…Fig. 3 also includes the water production given by Snodgrass et al (2017) for the end of 2015 July (5.1 × 10 27 s −1 ), which is within our error bounds whereas for the week after perihelion their value 3.2 × 10 27 s −1 is lower by a factor of 4 compared to our estimation. At later times (2015 September, October, and November), their values are again within our error bounds.…”

Section: G a S P Ro D U C T I O N F O R K N Ow N M I S S I O N S E G supporting

confidence: 72%

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The gas production of 14 species from comet 67P/Churyumov–Gerasimenko based on DFMS/COPS data from 2014 to 2016

Läuter

Kramer

Rubin

et al. 2020

Monthly Notices of the Royal Astronomical Society

110

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The coma of comet 67P/Churyumov-Gerasimenko has been probed by the Rosetta spacecraft and shows a variety of different molecules. The ROSINA COmet Pressure Sensor and the Double Focusing Mass Spectrometer provide in-situ densities for many volatile compounds including the 14 gas species H2O, CO2, CO, H2S, O2, C2H6, CH3OH, H2CO, CH4, NH3, HCN, C2H5OH, OCS, and CS2. We fit the observed densities during the entire comet mission between August 2014 and September 2016 to an inverse coma model. We retrieve surface emissions on a cometary shape with 3996 triangular elements for 50 separated time intervals. For each gas we derive systematic error bounds and report the temporal evolution of the production, peak production, and the time-integrated total production. We discuss the production for the two lobes of the nucleus and for the northern and southern hemispheres. Moreover we provide a comparison of the gas production with the seasonal illumination.

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Section: G a S P Ro D U C T I O N F O R K N Ow N M I S S I O N S E G supporting

confidence: 90%

Section: G a S P Ro D U C T I O N F O R K N Ow N M I S S I O N S E G supporting

confidence: 72%

The gas production of 14 species from comet 67P/Churyumov–Gerasimenko based on DFMS/COPS data from 2014 to 2016

Läuter

Kramer

Rubin

et al. 2020

Monthly Notices of the Royal Astronomical Society

110

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“…2004 ), but in situ measurements were required to get a more detailed picture: despite a large campaign of observations supporting the Rosetta mission (Snodgrass et al. 2017 ), only the brightest emission features were detectable in remote data, and then only around the perihelion period while the Southern hemisphere was illuminated (Opitom et al. 2017 ; Snodgrass et al.…”

Section: Observation Of Cometsmentioning

confidence: 99%

On the Origin and Evolution of the Material in 67P/Churyumov-Gerasimenko

et al. 2020

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Primitive objects like comets hold important information on the material that formed our solar system. Several comets have been visited by spacecraft and many more have been observed through Earth-and space-based telescopes. Still our understanding remains limited. Molecular abundances in comets have been shown to be similar to interstellar ices and thus indicate that common processes and conditions were involved in their formation. The samples returned by the Stardust mission to comet Wild 2 showed that the bulk refractory material was processed by high temperatures in the vicinity of the early sun. The recent Rosetta mission acquired a wealth of new data on the composition of comet 67P/Churyumov-Gerasimenko (hereafter 67P/C-G) and complemented earlier observations of other comets. The isotopic, elemental, and molecular abundances of the volatile, semivolatile, and refractory phases brought many new insights into the origin and processing of the incorporated material. The emerging picture after Rosetta is that at least part of the volatile material was formed before the solar system and that cometary nuclei agglomerated over a wide range of heliocentric distances, different from where they are found today. Deviations from bulk solar system abundances indicate that the material was not fully homogenized at the location of comet formation, despite the radial mixing implied by the Stardust results. Post-formation evolution of the material might play an important role, which further

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“…The Royal Society discussion meeting on ‘Cometary science after Rosetta’ provided an excellent forum for its subject matter. This paper is derived from a presentation designed to give a snapshot of the Rosetta mission science so far, particularly focusing on the orbiter, with the lander discussed more broadly elsewhere in this issue [ 39 ] as well as the significant ground and near-Earth campaign [ 154 ]. When considering what Rosetta set out to achieve, referring to table 1 , it is the authors' belief that we have made great inroads to all aspects of the topics that the mission was designed to address, but we are by no means finished, and there is plenty of science to come as correlative analyses among instruments become more prevalent and more sophisticated modelling is accomplished.…”

Section: Discussionmentioning

confidence: 99%

The Rosetta mission orbiter science overview: the comet phase

Taylor

Altobelli

Buratti

et al. 2017

Phil. Trans. R. Soc. A.

101

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The international Rosetta mission was launched in 2004 and consists of the orbiter spacecraft Rosetta and the lander Philae. The aim of the mission is to map the comet 67P/Churyumov–Gerasimenko by remote sensing, and to examine its environment in situ and its evolution in the inner Solar System. Rosetta was the first spacecraft to rendezvous with and orbit a comet, accompanying it as it passes through the inner Solar System, and to deploy a lander, Philae, and perform in situ science on the comet's surface. The primary goals of the mission were to: characterize the comet's nucleus; examine the chemical, mineralogical and isotopic composition of volatiles and refractories; examine the physical properties and interrelation of volatiles and refractories in a cometary nucleus; study the development of cometary activity and the processes in the surface layer of the nucleus and in the coma; detail the origin of comets, the relationship between cometary and interstellar material and the implications for the origin of the Solar System; and characterize asteroids 2867 Steins and 21 Lutetia. This paper presents a summary of mission operations and science, focusing on the Rosetta orbiter component of the mission during its comet phase, from early 2014 up to September 2016.This article is part of the themed issue ‘Cometary science after Rosetta’.

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The 67P/Churyumov–Gerasimenko observation campaign in support of the Rosetta mission

Cited by 41 publications

References 74 publications

The gas production of 14 species from comet 67P/Churyumov–Gerasimenko based on DFMS/COPS data from 2014 to 2016

The gas production of 14 species from comet 67P/Churyumov–Gerasimenko based on DFMS/COPS data from 2014 to 2016

On the Origin and Evolution of the Material in 67P/Churyumov-Gerasimenko

The Rosetta mission orbiter science overview: the comet phase

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