Modelling the Interior Structure of Enceladus Based on the 2014’s Cassini Gravity Data

Taubner, Ruth-Sophie; Leitner, Johannes; Firneis, M. G.; Hitzenberger, R.

doi:10.1007/s11084-015-9475-9

Cited by 7 publications

(9 citation statements)

References 18 publications

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“…In the following section, we will focus on methanogens and their adaptation to extreme conditions. A more detailed review about that topic can be found in Taubner et al (2016b). Besides Earth, methane (CH 4 ) has been detected on every planet of the Solar System, on the dwarf planets Pluto, Makemake, and Eris (Formisano et al 2004, Mumma et al 2009, Webster et al 2015, and on the icy moons Titan (Niemann et al 2005) and Enceladus (Waite et al 2009(Waite et al , 2014(Waite et al , 2017.…”

Section: Methanogens As Model Organisms For Icy Moon Related Cultivatmentioning

confidence: 99%

“…Most of the CH 4 found on Earth is of biogenic origin . Methanogens are the overwhelmingly dominant producers of CH 4 as metabolic end products of their carbon-and energy-yielding reactions (Thauer et al 2008;Taubner et al 2016b;Rittmann et al 2015), however, some (aerobic) marine microorganisms were also shown to produce CH 4 from methylphosphonic acid (Karl et al 2008;Metcalf et al 2012;Carini et al 2014). Methanogens are a phylogenetically and metabolically diverse group of prokaryotic organisms from the domain Archaea.…”

Section: Methanogens As Model Organisms For Icy Moon Related Cultivatmentioning

confidence: 99%

“…Most of the >150 characterized methanogens grow at neutral pH values (Taubner et al 2016b). Methanogens such as M. okinawensis (Takai et al 2002; and M. marburgensis (Bernacchi et al 2014) tolerate a broader pH range down to values of 3.5 and 4.5, respectively.…”

Section: Adaptation To Phmentioning

confidence: 99%

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Microbial Diversity and Biosignatures: An Icy Moons Perspective

et al. 2020

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The icy moons of the outer Solar System harbor potentially habitable environments for life, however, compared to the terrestrial biosphere, these environments are characterized by extremes in temperature, pressure, pH, and other physico-chemical conditions. Therefore, the search for life on these icy worlds is anchored on the study of terrestrial extreme environments (termed "analogue sites"), which harbor microorganisms at the frontiers of polyextremophily. These so-called extremophiles have been found in areas previously considered sterile: hot springs, hydrothermal vents, acidic or alkaline lakes, hypersaline environments, deep sea sediments, glaciers, and arid areas, amongst others. Such model systems and communities in extreme terrestrial environments may provide important information relevant to the astrobiology of icy bodies, including the composition of potential biological communities and the identification of biosignatures that they may produce. Extremophiles can use either sunlight (phototrophs) or chemical energy (chemotrophs) as energy sources, and different chemical compounds as electron donors or acceptors. Aerobic microorganisms use oxygen (O 2) as a terminal electron acceptor, whereas anaerobic microorganisms may use nitrate (NO − 3), sulfate (SO 2− 4), carbon dioxide (CO 2

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Section: Methanogens As Model Organisms For Icy Moon Related Cultivatmentioning

confidence: 99%

Section: Methanogens As Model Organisms For Icy Moon Related Cultivatmentioning

confidence: 99%

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Microbial Diversity and Biosignatures: An Icy Moons Perspective

et al. 2020

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“…However, on the basis of results of Cassini, Rappaport et al (2007) suggested that Enceladus has a hydrated core of density 2500 kg m À3 . Recent results of the Cassini spacecraft have indicated the MoI of Enceladus to be 0.335, which suggests the differentiation of satellite into a hydrated rocky core (Iess et al 2014;Taubner et al 2016). Schubert et al (2007) have shown variation in the MoI as a function of the assumed density of the rocky core to explain the two-layer model for Enceladus.…”

Section: Thermal Evolution Of Ganymede and Titanmentioning

confidence: 99%

Thermal evolution of trans‐Neptunian objects, icy satellites, and minor icy planets in the early solar system

Bhatia

Sahijpal

2017

Meteorit & Planetary Scien

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Numerical simulations are performed to understand the early thermal evolution and planetary scale differentiation of icy bodies with the radii in the range of 100–2500 km. These icy bodies include trans‐Neptunian objects, minor icy planets (e.g., Ceres, Pluto); the icy satellites of Jupiter, Saturn, Uranus, and Neptune; and probably the icy‐rocky cores of these planets. The decay energy of the radionuclides, 26Al, 60Fe, 40K, 235U, 238U, and 232Th, along with the impact‐induced heating during the accretion of icy bodies were taken into account to thermally evolve these planetary bodies. The simulations were performed for a wide range of initial ice and rock (dust) mass fractions of the icy bodies. Three distinct accretion scenarios were used. The sinking of the rock mass fraction in primitive water oceans produced by the substantial melting of ice could lead to planetary scale differentiation with the formation of a rocky core that is surrounded by a water ocean and an icy crust within the initial tens of millions of years of the solar system in case the planetary bodies accreted prior to the substantial decay of 26Al. However, over the course of billions of years, the heat produced due to 40K, 235U, 238U, and 232Th could have raised the temperature of the interiors of the icy bodies to the melting point of iron and silicates, thereby leading to the formation of an iron core. Our simulations indicate the presence of an iron core even at the center of icy bodies with radii ≥500 km for different ice mass fractions.

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“…The icy shell likely contains ”misty ice caverns“ [ 192 ] and/or a (global) subsurface ocean in contact with the rocky core [ 163 , 193 , 194 ]. According to several models, the rocky core expands to a radius of about 160 to 190 km [ 193 , 195 , 196 ].…”

Section: Known and Potential Habitats For Methanogens In The Solarmentioning

confidence: 99%

Assessing the Ecophysiology of Methanogens in the Context of Recent Astrobiological and Planetological Studies

Taubner

Schleper

Firneis

et al. 2015

Life

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Among all known microbes capable of thriving under extreme and, therefore, potentially extraterrestrial environmental conditions, methanogens from the domain Archaea are intriguing organisms. This is due to their broad metabolic versatility, enormous diversity, and ability to grow under extreme environmental conditions. Several studies revealed that growth conditions of methanogens are compatible with environmental conditions on extraterrestrial bodies throughout the Solar System. Hence, life in the Solar System might not be limited to the classical habitable zone. In this contribution we assess the main ecophysiological characteristics of methanogens and compare these to the environmental conditions of putative habitats in the Solar System, in particular Mars and icy moons. Eventually, we give an outlook on the feasibility and the necessity of future astrobiological studies concerning methanogens.

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Modelling the Interior Structure of Enceladus Based on the 2014’s Cassini Gravity Data

Cited by 7 publications

References 18 publications

Microbial Diversity and Biosignatures: An Icy Moons Perspective

Microbial Diversity and Biosignatures: An Icy Moons Perspective

Thermal evolution of trans‐Neptunian objects, icy satellites, and minor icy planets in the early solar system

Assessing the Ecophysiology of Methanogens in the Context of Recent Astrobiological and Planetological Studies

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