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

Läuter, M.; Kramer, Tobias; Rubin, Martin; Altwegg, Kathrin

doi:10.1093/mnras/staa2643

Cited by 53 publications

(127 citation statements)

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“…The short-term variation of the methanol line shifts and intensity, likely related to nucleus rotation, are observed in ALMA data (Roth et al 2020(Roth et al , 2021. Läuter et al (2020). (b) Assuming a daughter distribution with Lp = 1000 km (Cordiner et al 2014(Cordiner et al , 2017.…”

Section: Comparison With Other Observationsmentioning

confidence: 99%

Molecular composition of comet 46P/Wirtanen from millimetre-wave spectroscopy

Biver

Bockelée‐Morvan

Boissier

et al. 2021

A&A

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We present the results of a molecular survey of comet 46P/Wirtanen undertaken with the IRAM 30-m and NOEMA radio telescopes in December 2018. Observations at IRAM 30-m during the 12–18 December period comprise a 2 mm spectral survey covering 25 GHz and a 1 mm survey covering 62 GHz. The gas outflow velocity and kinetic temperature have been accurately constrained by the observations. We derive abundances of 11 molecules, some being identified remotely for the first time in a Jupiter-family comet, including complex organic molecules such as formamide, ethylene glycol, acetaldehyde, or ethanol. Sensitive upper limits on the abundances of 24 other molecules are obtained. The comet is found to be relatively rich in methanol (3.4% relative to water), but relatively depleted in CO, CS, HNC, HNCO, and HCOOH.

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Section: Comparison With Other Observationsmentioning

confidence: 99%

Molecular composition of comet 46P/Wirtanen from millimetre-wave spectroscopy

Biver

Bockelée‐Morvan

Boissier

et al. 2021

A&A

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“…The mass spectra presented in this work are consistent within errors with these methanol oxygen and carbon isotopic ratios (Appendix A). The measured methanol abundances relative to water and total production rates from ROSINA during the entire duration of the Rosetta mission between August 2014 and September 2016 are presented by Läuter et al (2020). Based on a comparison of production rates, CH 3 OH may be grouped with H 2 O, O 2 , H 2 CO, and NH 3 .…”

Section: P/c-g: Rosina Mass Spectramentioning

confidence: 99%

“…However, it remains difficult to piece together the spatial distribution of desorbing gas as the measurements are being carried out at one specific location above a certain part of the comet (e.g. Läuter et al 2020). Mass spectrometry eliminates the uncertainties stemming from excitation and spectroscopy.…”

Section: Caveats Of Cometary Measurementsmentioning

confidence: 99%

“…Comet 67P/C-G likely carries both variants of mono-deuterated methanol (CH 3 OD, CH 2 DOH), and both variants of di-deuterated methanol (CH 2 DOD, CHD 2 OH) at combined abundances of 5.5 ± 0.46 and 0.069 ± 0.014 per cent relative to CH 3 OH, respectively (Section 3.1). Methanol is available in the coma of 67P/C-G at an average level of 0.5 per cent relative to water (Läuter et al 2020; Section 3.1). The methanol formation and deuteration schemes are supported by a wealth of laboratory experiments (Section 4.1, Appendix C).…”

Section: Formation and Deuteration Of Volatiles In 67p/c-gmentioning

confidence: 99%

“…Modelling of thermophysics, hydrostatics, orbit evolution, and collision physics suggests that 67P/C-G is a primordial rubble pile (Davidsson et al 2016). Its persistent exposure to temperatures below 20 K is supported by the detection of not only CO but also other hypervolatiles such as O 2 (Bieler et al 2015;Fougere et al 2016;Gasc et al 2017;Keeney et al 2017Keeney et al , 2019Noonan et al 2018;Hoang et al 2019;Combi et al 2020;Läuter et al 2020), N 2 (Rubin et al 2015a), CH 4 (Le Roy et al 2015;Schuhmann et al 2019), and Ar (Balsiger et al 2015) with low binding energies (Ayotte et al 2001;Collings et al 2004;Bar-Nun, Notesco & Owen 2007). Some works argue that the only way that O 2 can be produced at the abundance level ∼4 per cent relative to water in 67P/C-G and show such a strong correlation with water is for it to be formed in a prestellar core that has a slightly elevated temperature of ∼15-25 K (in contrast to the typical core temperature of 10 K) through a combination of gas-phase and grain-surface processes (Taquet et al 2016(Taquet et al , 2018Eistrup & Walsh 2019).…”

Section: Volatiles Of 67p/c-g As Tracers Of Our Solar System's Pastmentioning

confidence: 99%

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Prestellar grain-surface origins of deuterated methanol in comet 67P/Churyumov–Gerasimenko

Drozdovskaya

Schroeder

Rubin

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Deuterated methanol is one of the most robust windows astrochemists have on the individual chemical reactions forming deuterium-bearing molecules and the physicochemical history of the regions where they reside. The first-time detection of mono- and di-deuterated methanol in a cometary coma is presented for comet 67P/Churyumov–Gerasimenko using Rosetta–ROSINA data. D-methanol (CH3OD and CH2DOH combined) and D2-methanol (CH2DOD and CHD2OH combined) have an abundance of 5.5 ± 0.46 and 0.00069 ± 0.00014 per cent relative to normal methanol. The data span a methanol deuteration fraction (D/H ratio) in the 0.71 − 6.6 per cent range, accounting for statistical corrections for the location of D in the molecule and including statistical error propagation in the ROSINA measurements. It is argued that cometary CH2DOH forms from CO hydrogenation to CH3OH and subsequent H-D substitution reactions in CH3-R. CHD2OH is likely produced from deuterated formaldehyde. Meanwhile, CH3OD and CH2DOD, could form via H-D exchange reactions in OH-R in the presence of deuterated water ice. Methanol formation and deuteration is argued to occur at the same epoch as D2O formation from HDO, with formation of mono-deuterated water, hydrogen sulfide, and ammonia occurring prior to that. The cometary D-methanol/methanol ratio is demonstrated to agree most closely with that in prestellar cores and low-mass protostellar regions. The results suggest that cometary methanol stems from the innate cold (10 − 20 K) prestellar core that birthed our Solar System. Cometary volatiles individually reflect the evolutionary phases of star formation from cloud to core to protostar.

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Protocells: Milestones and Recent Advances

Gözen

Köksal

Põldsalu

et al. 2022

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to assemble astonishing pieces of a complicated puzzle, and realized that further advancement requires input from multiple branches of science, not just biology as the primary life science. Detailed hypotheses have been established about the different scenarios of the emergence of life, including the "RNA world," [1] the "lipid world," [2] "replicator first," [3] "metabolism first," [4][5][6] and others. Although the origin of life is still surrounded by many open questions, our understanding of chemical, physicochemical, and biochemical processes possibly involved in the ancient events preceding Darwinian evolution has seen much progress. We have come a long way from Leduc's physicochemical, inorganic matter-centered view on the beginning of the evolution, yet the matter of the transition from nonliving to living matter still remains largely unsolved, and one of the great scientific problems of our time.The phylogenetic tree of different living domains reflects that life has evolved from simple to more complex structures, i.e., from single-to multicellular organisms. The oldest fossil evidence dating back 3.5 Gy (billion years) comes from stromatolites, [7][8][9][10] microorganismal residues in sedimentary rocks. [11] There appears to be a gap of knowledge regarding the period of evolution between the first primitive hypothetical cells and the fossilized ancient bacteria, which can be considered as an already advanced form of life. [12] It is highly likely that intermediate primitive cell precursors preceded the single-cell organisms. The hypothetical prebiotic structures that were the stepping stone to first self-sustaining living cells are commonly termed "protocells." The possibility of a strong link between the formation of protocells and the origin of life can today be reasonably assumed.One cannot easily proceed in the context of the evolution of cell-based organisms without briefly illuminating the concept of life as we know it on our planet. Over time, different requirements have been proposed for an entity to be considered alive. According to Tibor Ganti's chemoton model, [13] a protocell contains three autocatalytic subsystems: a membrane subsystem that keeps the components together and intact, a metabolic subsystem that captures energy and material resources, and an information subsystem that processes and transfers heritable information to progeny. To be considered alive, these subsystems must be unified and function co-operatively for the survival and evolution of the supersystem. Pohorille and Deamer suggested a modified set of 7 criteria related to the chemoton. [14] At about the same time, Oro defined the requirements by 10 characteristic features. [15] Despite their differences, these descriptions align well with NASA's broader definition of life: "a self-sustaining chemical system capable of Darwinian evolution."The origin of life is still one of humankind's great mysteries. At the transition between nonliving and living matter, protocells, initially featureless aggregates of abiotic matter, ga...

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

Cited by 53 publications

References 63 publications

Molecular composition of comet 46P/Wirtanen from millimetre-wave spectroscopy

Molecular composition of comet 46P/Wirtanen from millimetre-wave spectroscopy

Prestellar grain-surface origins of deuterated methanol in comet 67P/Churyumov–Gerasimenko

Protocells: Milestones and Recent Advances

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