Internal structure and cryovolcanism on Trans-Neptunian objects

Guilbert-Lepoutre, A.; Prialnik, Dina; Métayer, Robin

doi:10.1016/b978-0-12-816490-7.00008-4

Cited by 4 publications

(5 citation statements)

References 114 publications

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“…To address this, we determined the rates and mechanism of olivine dissolution in alkaline solutions at -20, 4, and 22 °C from dissolution experiments that lasted up to 442 days. The range of temperatures chosen corresponds to those that can be achieved in mid-to large-sized icy worlds from radiogenic sources alone, in the absence of extra heat due to tidal friction 4,5,7 . Most icy worlds with diametres exceeding 400-500 km cross this temperature threshold when their cores, comprised of ice and rock, undergo an initial heating period.…”

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confidence: 99%

“…This process likely controlled the early evolution of most icy worlds, including Ceres, ' and Uranus' mid-sized moons (Mimas, Enceladus, Dione, Ariel, Oberon, Titania) 1 , and TNOs with diameters >500 km 7 . Low core densities of Ceres (2400-2900 kg m -3 ) 20 , Enceladus (2400-2500 kg m -3 ) 21 , and Dione (2400-2500 kg m -3 ) 22 corroborate the hypothesis that the rocky cores of these worlds are largely composed of altered hydrated minerals.…”

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confidence: 99%

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Geologically rapid aqueous mineral alteration at subfreezing temperatures in icy worlds

et al. 2022

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confidence: 99%

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confidence: 99%

Geologically rapid aqueous mineral alteration at subfreezing temperatures in icy worlds

et al. 2022

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“…If objects are captured by planets, this mantle may be activated by the additional energy sources that become available, such as tidal heating. In this case a sub-surface ocean can form and allow for cryovolcanism (Rhoden et al 2015;Thomas et al 2016;Guilbert-Lepoutre et al 2020). A dense outer crust is found in differentiated objects.…”

Section: Discussionmentioning

confidence: 99%

On the structure and long-term evolution of ice-rich bodies

Loveless,

Prialnik,

Podolak

2022

Preprint

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The interest in the structure of ice-rich planetary bodies, in particular the differentiation between ice and rock, has grown due to the discovery of Kuiper belt objects and exoplanets. We thus carry out a parameter study for a range of planetary masses M , yielding radii 50 < ∼ R < ∼ 3000 km, and for rock/ice mass ratios between 0.25 and 4, evolving them for 4.5 Gyr in a cold environment, to obtain the present structure. We use a thermal evolution model that allows for liquid and vapor flow in a porous medium, solving mass and energy conservation equations under hydrostatic equilibrium for a spherical body in orbit around a central star. The model includes the effect of pressure on porosity and on the melting temperature, heating by long-lived radioactive isotopes, and temperature-dependent serpentinization and dehydration. We obtain the boundary in parameter space [size, rock-content] between bodies that differentiate, forming a rocky core, and those which remain undifferentiated: small bodies, bodies with a low rock content, and the largest bodies considered, which develop high internal pressures and barely attain the melting temperature. The final differentiated structure comprises a rocky core, an ice-rich mantle, and a thin dense crust below the surface. We obtain and discuss the bulk density-radius relationship. The effect of a very cold environment is investigated and we find that at an ambient temperature of ∼20 K, small bodies preserve the ice in amorphous form to the present.

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“…For the initial 26 Al/ 27 Al ratio we adopt a value of 5.25 • 10 −5 at calcium-aluminium-rich inclusion (CAI) formation (Kita et al, 2013), while for 60 Fe we use an initial ratio of 60 Fe/ 56 Fe = 1.9 • 10 −7 (Tachibana and Huss, 2003;Mostefaoui et al, 2004). However it should be pointed out that the 26 Al/ 27 Al and 60 Fe/ 56 Fe values for comets and KBOs are so far unconstrained (Prialnik et al 2008;Merk and Prialnik, 2006;Choi et al 2002;Guilbert-Lepoutre et al 2019).…”

Section: Heating By Short-lived Radionuclidesmentioning

confidence: 99%

Modification of icy planetesimals by early thermal evolution and collisions: Constraints for formation time and initial size of comets and small KBOs

Golabek,

Jutzi

2021

Preprint

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Comets and small Kuiper belt objects are considered to be among the most primitive objects in the solar system as comets like C/1995 O1 Hale-Bopp are rich in highly volatile ices like CO. It has been suggested that early in the solar system evolution the precursors of both groups, the so-called icy planetesimals, were modified by both short-lived radiogenic heating and collisional heating. Here we employ 2D finite-difference numerical models to study the internal thermal evolution of these objects, where we vary formation time, radius and rock-to-ice mass fraction. Additionally we perform 3D SPH collision models with different impact parameters, thus considering both cratering and catastrophic disruption events. Combining the results of both numerical models we estimate under which conditions highly volatile ices like CO, CO 2 and NH 3 can be retained inside present-day comets and Kuiper belt objects. Our results indicate that for present-day objects de-

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Internal structure and cryovolcanism on Trans-Neptunian objects

Cited by 4 publications

References 114 publications

Geologically rapid aqueous mineral alteration at subfreezing temperatures in icy worlds

Geologically rapid aqueous mineral alteration at subfreezing temperatures in icy worlds

On the structure and long-term evolution of ice-rich bodies

Modification of icy planetesimals by early thermal evolution and collisions: Constraints for formation time and initial size of comets and small KBOs

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