Amino acids derived from Titan Tholins

Khare, B. N.; Sagan, Carl; Ogino, Hiroshi; Nagy, Bartholomew; Er, Cevat; Schram, Karl H.; Arakawa, E. T.

doi:10.1016/0019-1035(86)90080-1

Cited by 149 publications

(91 citation statements)

References 22 publications

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“…It is well known that harsh hydrolysis of similar samples reveals a product mixture containing both natural and meteoritic amino°acids,°presumably°from°nitrile°hydrolysis° [26,27]. The hydrolysis of the C x H y N z containing tholin samples is currently further explored in a more systematic way and the results of this study will be summarized in a separate paper.…”

Section: Exposure To Air and Watermentioning

confidence: 96%

Organic environments on Saturn’s moon, Titan: Simulating chemical reactions and analyzing products by FT-ICR and ion-trap mass spectrometry

Somogyi

Smith

et al. 2005

J. Am. Soc. Mass Spectrom.

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Laboratory simulations have been carried out to model chemical reactions that possibly take place in the stratosphere of Saturn's moon, Titan. The aerosol products of these reactions (tholin samples) have been systematically analyzed by mass spectrometry using electrospray ionization (ESI) and laser desorption (LD). A wide variety of ions with a general formula C x H y N z detected by ultrahigh resolution and accurate mass measurements in a Fourier transform/ion cyclotron resonance (FT-ICR) cell reflect the complexity of these polymeric products, both in chemical compositions and isomeric distributions. As a common feature, however, tandem mass spectral (MS/MS) data and H/D exchange products in the solution phase support the presence of amino and nitrile functionalities in these (highly unsaturated) "tholin" compounds. The present work demonstrates that ESI-MS coupled with FT-ICR is a suitable and "intact" method to analyze tholin components formed under anaerobic conditions; only species with C x H y N z are detected for freshly prepared and harvested samples. However, when intentionally exposed to water, oxygen-containing compounds are unambiguously detected. (J Am Soc Mass Spectrom 2005, 16, 850 -859)

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Section: Exposure To Air and Watermentioning

confidence: 96%

Organic environments on Saturn’s moon, Titan: Simulating chemical reactions and analyzing products by FT-ICR and ion-trap mass spectrometry

Somogyi

Smith

et al. 2005

J. Am. Soc. Mass Spectrom.

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“…: the ices in our case). We ran models considering amorphous and crystalline water ice (Grundy & Schmitt 1998), olivine and pyroxene (see Barucci et al 2012), triton, titan and ice tholins (Khare et al 1986(Khare et al , 1993, methanol , methane (Quirico & Schmitt 1997), amorphous carbon (Zubko et al 1996), and kaolinite (Merlin et al 2010b). Results of the best-fit models for the different spectra are reported in Table 2 and Fig.…”

Section: Spectral Modelsmentioning

confidence: 99%

Methanol ice on the surface of minor bodies in the solar system

Merlin¹,

Quirico²,

Barucci³

et al. 2012

A&A

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Aims. Spectral analyses of trans-Neptunan objects (TNOs) and of the linked Centaurs, which are supposed to be among the most primitive minor bodies in the solar system, reveal some chemical and physical properties of their surface. To determine the surface composition of these objects and their surface evolution is essential for gaining clues on the conditions under which the solar system has been formed. Methods. Chemical composition and physical properties of the surface of three objects have been constrained by computing the depth of the absorption features of the spectra in the near-infrared, running spectral models based on radiative transfer theory in the [0.4−2.3] μm range, and analyzing new laboratory measurements of the spectral behavior of thin samples of H 2 O-CH 3 OH mixtures. Results. Our investigations allow us to confirm the presence of CH 3 OH ice on the surface of the Centaur (5145) Pholus and the resonant (55638) TNO 2002 VE 95 . It may also possibly be found on the classical TNO (120348) 2004 TY 364 . Our laboratory experiments indicate that the behavior of the methanol and water ice absorption bands is dependent on the ambient temperature and the dilution level of the mixture. These results also suggest that methanol may be diluted in water ice on the surface of the Centaur Pholus. Conclusions. Formation and destruction processes of methanol suggest that a part (at least) of the surface of these objects is younger than the solar system age. If confirmed, this shows that primordial ices could still be detected on the surface of objects that are submitted to irradiation and rejuvenation processes.

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“…Once deposited on Titan's surface, the aerosols and their complex organic content may follow a chemical evolution of astrobiological interest. Laboratory experiments show that, once in contact with liquid water, Titan tholins can release many compounds of biological interest, such as amino acids [19]. Such processes could be particularly favourable in regions on Titan's surface where cryovolcanism is occurring.…”

Section: A Complex Prebiotic-like Chemistrymentioning

confidence: 99%

TandEM: Titan and Enceladus mission

et al. 2008

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International audienceTandEM was proposed as an L-class (large) mission in response to ESA's Cosmic Vision 2015-2025 Call, and accepted for further studies, with the goal of exploring Titan and Enceladus. The mission concept is to perform in situ investigations of two worlds tied together by location and properties, whose remarkable natures have been partly revealed by the ongoing Cassini-Huygens mission. These bodies still hold mysteries requiring a complete exploration using a variety of vehicles and instruments. TandEM is an ambitious mission because its targets are two of the most exciting and challenging bodies in the Solar System. It is designed to build on but exceed the scientific and technological accomplishments of the Cassini-Huygens mission, exploring Titan and Enceladus in ways that are not currently possible (full close-up and in situ coverage over long periods of time). In the current mission architecture, TandEM proposes to deliver two medium-sized spacecraft to the Saturnian system. One spacecraft would be an orbiter with a large host of instruments which would perform several Enceladus flybys and deliver penetrators to its surface before going into a dedicated orbit around Titan alone, while the other spacecraft would carry the Titan in situ investigation components, i.e. a hot-air balloon (Montgolfière) and possibly several landing probes to be delivered through the atmospher

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Amino acids derived from Titan Tholins

Cited by 149 publications

References 22 publications

Organic environments on Saturn’s moon, Titan: Simulating chemical reactions and analyzing products by FT-ICR and ion-trap mass spectrometry

Organic environments on Saturn’s moon, Titan: Simulating chemical reactions and analyzing products by FT-ICR and ion-trap mass spectrometry

Methanol ice on the surface of minor bodies in the solar system

TandEM: Titan and Enceladus mission

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