The Composition of Comets

Cochran, A. L.; Levasseur-Regourd, A. C.; Cordiner, Martin; Hadamcik, Edith; Lasue, J.; Gicquel, A.; Schleicher, D. G.; Charnley, Steven B.; Mumma, M. J.; Paganini, L.; Bockelée‐Morvan, Dominique; Biver, Nicolás; Kuan, Yi‐Jehng

doi:10.1007/s11214-015-0183-6

Cited by 109 publications

(87 citation statements)

References 198 publications

(183 reference statements)

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“…This is supported by the detection of ethylene glycol and formamide on comets C/2012 F6 (Lemmon) and C/2013 R1 (Lovejoy), as well as ethanol and glycolaldehyde in the latter target (Biver et al 2014(Biver et al , 2015. The determined volatile composition does not show any major differences from that seen in other comets (as reviewed in Cochran et al 2015;Dello Russo et al 2016).…”

Section: Representability Of the Targetsmentioning

confidence: 65%

Ingredients for solar-like systems: protostar IRAS 16293-2422 B versus comet 67P/Churyumov–Gerasimenko

Drozdovskaya

Dishoeck

Rubin

et al. 2019

Monthly Notices of the Royal Astronomical Society

129

102

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Our modern day Solar System has 4.6 × 10 9 yrs of evolution behind it with just a few relics of its birth conditions remaining. Comets are thought to be some of the most pristine tracers of the initial ingredients that were combined to produce the Earth and the other planets. Other low-mass protostars may be analogous to our proto-Sun and hence, could be used to study the building blocks necessary to form Solar-like systems. This study tests this idea on the basis of new high sensitivity, high spatial resolution ALMA data on the protoplanetary discscales (∼ 70 au) of IRAS 16293-2422 and the bulk composition of comet 67P/Churyumov-Gerasimenko, as determined for the first time with the unique in situ monitoring carried out by Rosetta. The comparative analysis of the observations from the Protostellar Interferometric Line Survey (PILS) and the measurements made with Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA) shows that the relative abundances of CHO-, N-, and Sbearing molecules correlate, with some scatter, between protostellar and cometary data. A tentative correlation is seen for the first time for P-and Cl-bearing compounds. The results imply that the volatile composition of cometesimals and planetesimals is partially inherited from the pre-and protostellar phases of evolution.

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Section: Representability Of the Targetsmentioning

confidence: 65%

Ingredients for solar-like systems: protostar IRAS 16293-2422 B versus comet 67P/Churyumov–Gerasimenko

Drozdovskaya

Dishoeck

Rubin

et al. 2019

Monthly Notices of the Royal Astronomical Society

129

102

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“…Comets, as studied from previous flyby missions and remote spectroscopy, are composed of ices (mainly water ice) and refractory species, which consist of rock-forming elements (e.g., silicates) and of C, H, O, and N carbonaceous compounds (e.g., Cochran et al 2015). The MIRO and VIRTIS experiments at 67P confirm these assumptions (e.g., Gulkis et al 2015;Capaccioni et al 2015).…”

Section: Permittivity Valuesmentioning

confidence: 92%

CONSERT suggests a change in local properties of 67P/Churyumov-Gerasimenko’s nucleus at depth

Ciarletti

Levasseur-Regourd

Lasue

et al. 2015

A&A

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Context. After the successful landing of Philae on the nucleus of 67P/Churyumov-Gerasimenko, the Rosetta mission provided the first opportunity of performing measurements with the CONSERT tomographic radar in November 2014. CONSERT data were acquired during this first science sequence. They unambiguously showed that propagation through the smaller lobe of the nucleus was achieved. Aims. While the ultimate objective of the CONSERT radar is to perform the tomography of the nucleus, this paper focuses on the local characterization of the shallow subsurface in the area of Philae's final landing site, specifically determining the possible presence of a permittivity gradient below the nucleus surface. Methods. A number of electromagnetic simulations were made with a ray-tracing code to parametrically study how the gradient of the dielectric constant in the near-subsurface affects the ability of CONSERT to receive signals. Results. At the 90 MHz frequency of CONSERT, the dielectric constant is a function of porosity, composition, and temperature. The dielectric constant values considered for the study are based on observations made by the other instruments of the Rosetta mission, which indicate a possible near-surface gradient in physical properties and on laboratory measurements made on analog samples. Conclusions. The obtained simulated data clearly show that if the dielectric constant were increasing with depth, it would have prevented the reception of signal at the CONSERT location during the first science sequence. We conclude from our simulations that the dielectric constant most probably decreases with depth.

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“…Unlike the growing chemical database for comets (Cochran et al 2015), the more distant and less active Centaurs lack sufficient information, either from surface reflectance or from gas emission, to determine mixing ratios between volatile species. Thus, we make the distinction that depletion in these cases refers to the reduced activity level detected for a given species (such as CO) relative to other objects or a certain reference.…”

Section: Co Production Rates Adjusted For Nucleus Sizementioning

confidence: 99%