Exploration and Protection of Europa's Biosphere: Implications of Permeable Ice

Greenberg, R.

doi:10.1089/ast.2011.0608

Cited by 6 publications

(3 citation statements)

References 23 publications

(20 reference statements)

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“…This is particularly exciting for exomoon-hunting, because Neptune-mass exoplanets are among the most common mass-category of exoplanets, if they can also form satellites, there must be a much larger population of exomoons than previously considered. Moreover, icy moons in our Solar System are the main targets to search for extraterrestrial life (Europa in case of Jupiter, Greenberg 2011;Sparks et al 2017, and Enceladus in case of Saturn, Parkinson et al 2008), hence a larger amount of icy satellites of the similar kind means potentially larger sample of habitable words.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

In Situ Formation of Icy Moons of Uranus and Neptune

Szulágyi

Cilibrasi

Mayer

2018

ApJL

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Satellites of giant planets thought to form in gaseous circumplanetary disks (CPDs) during the late planet-formation phase, but it was unknown so far whether smaller mass planets, such as the ice giants could form such disks, thus moons there. We combined radiative hydrodynamical simulations with satellite population synthesis to investigate the question in the case of Uranus and Neptune. For both ice giants we found that a gaseous CPD is created at the end of their formation. The population synthesis confirmed that Uranian-like, icy, prograde satellite-system could form in these CPDs within a couple of 10 5 years. This means that Neptune could have a Uranian-like moon-system originally that was wiped away by the capture of Triton. Furthermore, the current moons of Uranus can be reproduced by our model without the need for planet-planet impact to create a debris disk for the moons to grow. These results highlight that even ice giants -that among the most common masscategory of exoplanets -can also form satellites, opening a way to a potentially much larger population of exomoons than previously thought.

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Section: Conclusion and Discussionmentioning

confidence: 99%

In Situ Formation of Icy Moons of Uranus and Neptune

Szulágyi

Cilibrasi

Mayer

2018

ApJL

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“…This lends itself to the suggestion that they formed in discs of gas and dust orbiting around their parent planets (Korycansky et al 1991;Ward & Canup 2010). These circumplanetary discs (CPDs) are thus the birthplaces of icy moons such as Europa and Enceladus, considered promising candidates for extraterrestrial life (Greenberg 2011;Blanc et al 2020;Parkinson et al 2008;Neveu et al 2020). They also regulate the flow of material onto a protoplanet (Rivier et al 2012), from which it follows that they determine the final mass that the mature planet can attain.…”

Section: Introductionmentioning

confidence: 89%

Size-selective accretion of dust onto CPDs: Low CPD masses and filtration of larger grains

Karlin¹,

Panić²,

Loo³

2023

Preprint

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The major satellites of Jupiter and Saturn are believed to have formed in circumplanetary discs, which orbit forming giant protoplanets. Gas and dust in CPDs have different distributions and affect each other by drag, which varies with grain size. Yet simulations of multiple dust grain sizes with separate dynamics have not been done before. We seek to assess how much dust of each grain size there is in circumplanetary discs. We run multifluid 3D hydrodynamical simulations including gas and four discrete grain sizes of dust from 1 𝜇m to 1 mm, representing a continuous distribution. We consider a 1𝑀 Jup protoplanet embedded in a protoplanetary disc around a 1𝑀 star. Our results show a truncated MRN distribution at smaller grain sizes, which starts to tail off by 𝑎 = 100 𝜇m and is near zero at 1 mm. Large dust grains, which hold most of the dust mass, have very inefficient accretion to the CPD, due to dust filtration. Therefore CPDs' dust masses must be small, with mass ratio ∼ a few ×10 −6 to the protoplanet. These masses and the corresponding millimetre opacities are in line with CPD fluxes observed to date.

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Section: Introductionmentioning

confidence: 94%

Size-selective accretion of dust on to CPDs: low CPD masses and filtration of larger grains

Karlin

Panić

Loo

2023

Monthly Notices of the Royal Astronomical Society

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The major satellites of Jupiter and Saturn are believed to have formed in circumplanetary discs, which orbit forming giant protoplanets. Gas and dust in CPDs have different distributions and affect each other by drag, which varies with grain size. Yet simulations of multiple dust grain sizes with separate dynamics have not been done before. We seek to assess how much dust of each grain size there is in circumplanetary discs. We run multifluid 3D hydrodynamical simulations including gas and four discrete grain sizes of dust from 1μm to 1 mm, representing a continuous distribution. We consider a 1 Mjup protoplanet embedded in a protoplanetary disc around a 1 M⊙ star. Our results show a truncated MRN distribution at smaller grain sizes, which starts to tail off by a = 100μm and is near zero at 1 mm. Large dust grains, which hold most of the dust mass, have very inefficient accretion to the CPD, due to dust filtration. Therefore CPDs’ dust masses must be small, with mass ratio ∼ a few × 10−6 to the protoplanet. These masses and the corresponding millimetre opacities are in line with CPD fluxes observed to date.

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Exploration and Protection of Europa's Biosphere: Implications of Permeable Ice

Cited by 6 publications

References 23 publications

In Situ Formation of Icy Moons of Uranus and Neptune

In Situ Formation of Icy Moons of Uranus and Neptune

Size-selective accretion of dust onto CPDs: Low CPD masses and filtration of larger grains

Size-selective accretion of dust on to CPDs: low CPD masses and filtration of larger grains

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