Accretion disks around Jupiter and Saturn at the stage of regular satellite formation

Makalkin, A. B.; Дорофеева, В. А.

doi:10.1134/s0038094614010067

Cited by 37 publications

(22 citation statements)

References 42 publications

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“…Moreover, we find that the H 2 O ice lines in both cases need about 10 5 yr to move radially from the outer disk edges to their final positions (see labels). Our values for Σ g are similar to those presented by Makalkin & Dorofeeva (2014) in their Fig. 4.…”

Section: /3supporting

confidence: 90%

“…They found that values between 10 −9 M Jup yr −1 and 10 −6 M Jup yr −1 (about 10 M Gan Myr −1 to 10 4 M Gan Myr −1 ) satisfy these constraints. Obviously, our results are at the lower end of this range, while accretion rates up to three orders of magnitude higher should be reasonable according to Makalkin & Dorofeeva (2014). Yet, these authors also claimed that planetary illumination be negligible in the final states of accretion, which is not supported by our findings (see Fig.…”

Section: Shutdown Accretion Rates and Loss Of Moonscontrasting

confidence: 78%

“…The equations of energy transport (Makalkin & Dorofeeva 2014) then allow us to derive the temperature profile both at the disk surface, where the optical depth τ = 2/3, and in the disk midplane. This model invokes absorption of planetary illumination in the disk photosphere at a height z s (r) above the midplane, modeled by an absorption coefficient (k s ), as well as the transport of energy through an optically thick disk to the surface, modeled by κ P .…”

Section: /3mentioning

confidence: 99%

“…Again, the additional energy terms in our model are one reason for the lower final accretion rates that we require in order to have the H 2 O ice line interior to the orbit of Ganymede. Makalkin & Dorofeeva (2014) also studied Jupiter's accretion rates and their compatibility with the Galilean moon system. They found that values between 10 −9 M Jup yr −1 and 10 −6 M Jup yr −1 (about 10 M Gan Myr −1 to 10 4 M Gan Myr −1 ) satisfy these constraints.…”

Section: Shutdown Accretion Rates and Loss Of Moonsmentioning

confidence: 99%

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Conditions for water ice lines and Mars-mass exomoons around accreting super-Jovian planets at 1−20 AU from Sun-like stars

Heller

2015

A&A

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Context. The first detection of a moon around an extrasolar planet (an "exomoon") might be feasible with NASA's Kepler or ESA's upcoming PLATO space telescopes or with the future ground-based European Extremely Large Telescope. To guide observers and to use observational resources most efficiently, we need to know where the largest, most easily detected moons can form. Aims. We explore the possibility of large exomoons by following the movement of water (H 2 O) ice lines in the accretion disks around young super-Jovian planets. We want to know how the different heating sources in those disks affect the location of the H 2 O ice lines as a function of stellar and planetary distance. Methods. We simulate 2D rotationally symmetric accretion disks in hydrostatic equilibrium around super-Jovian exoplanets. The energy terms in our semi-analytical framework -(1) viscous heating; (2) planetary illumination; (3) accretional heating of the disk; and (4) stellar illumination -are fed by precomputed planet evolution models. We consider accreting planets with final masses between 1 and 12 Jupiter masses at distances between 1 and 20 AU to a solar type star. Results. Accretion disks around Jupiter-mass planets closer than about 4.5 AU to Sun-like stars do not feature H 2 O ice lines, whereas the most massive super-Jovians can form icy satellites as close as 3 AU to Sun-like stars. We derive an empirical formula for the total moon mass as a function of planetary mass and stellar distance and predict that super-Jovian planets forming beyond about 5 AU can host Mars-mass moons. Planetary illumination is the major heat source in the final stages of accretion around Jupiter-mass planets, whereas disks around the most massive super-Jovians are similarly heated by planetary illumination and viscous heating. This indicates a transition towards circumstellar accretion disks, where viscous heating dominates in the stellar vicinity. We also study a broad range of circumplanetary disk parameters for planets at 5.2 AU and find that the H 2 O ice lines are universally between about 15 and 30 Jupiter radii in the final stages of accretion when the last generation of moons is supposed to form. Conclusions. If the abundant population of super-Jovian planets around 1 AU formed in situ, then these planets should lack the previously predicted population of giant icy moons, because those planets' disks did not host H 2 O ice in the final stages of accretion. But in the more likely case that these planets migrated to their current locations from beyond about 3 to 4.5 AU they might be orbited by large, water-rich moons. In this case, Mars-mass ocean moons might be common in the stellar habitable zones. Future exomoon detections and non-detections can provide powerful constraints on the formation and migration history of giant exoplanets.

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Section: /3supporting

confidence: 90%

Section: Shutdown Accretion Rates and Loss Of Moonscontrasting

confidence: 78%

Section: /3mentioning

confidence: 99%

Section: Shutdown Accretion Rates and Loss Of Moonsmentioning

confidence: 99%

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Conditions for water ice lines and Mars-mass exomoons around accreting super-Jovian planets at 1−20 AU from Sun-like stars

Heller

2015

A&A

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“…In particular, the H 2 O ice line, which is the radial distance at which the disk is cool enough for the transition of H 2 O vapor into solid ice, should have been between the orbits of rocky Europa at about 9.7 Jupiter radii (R Jup ) and icy Ganymede at about 15.5 R Jup from Jupiter. We simulate a 2D axisymmetric CPD in hydrostatic equilibrium around Jupiter using a "gas-starved" standard disk model (Canup & Ward 2002) that has been modified to include various heat sources (Makalkin & Dorofeeva 2014), namely, (i) viscous heating; (ii) planetary illumination in the "cold-start scenario"; (iii) direct accretion onto the CPD; and (iv) stellar illumination. The model is coupled to pre-computed planet evolution tracks (Mordasini 2013), and we here assume a solar luminosity 0.7 times its current value to take into account the faint young Sun (Sagan & Mullen 1972).…”

Section: Formation In the Circumjovian Accretion Diskmentioning

confidence: 99%

The formation of the Galilean moons and Titan in the Grand Tack scenario

Heller

Marleau

Pudritz

2015

A&A

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Context. In the Grand Tack (GT) scenario for the young solar system, Jupiter formed beyond 3.5 AU from the Sun and migrated as close as 1.5 AU until it encountered an orbital resonance with Saturn. Both planets then supposedly migrated outward for several 10 5 yr, with Jupiter ending up at ≈5 AU. The initial conditions of the GT and the timing between Jupiter's migration and the formation of the Galilean satellites remain unexplored. Aims. We study the formation of Ganymede and Callisto, both of which consist of ≈50% H 2 O and rock, in the GT scenario. We examine why they lack dense atmospheres, while Titan is surrounded by a thick N 2 envelope. Methods. We model an axially symmetric circumplanetary disk (CPD) in hydrostatic equilibrium around Jupiter. The CPD is warmed by viscous heating, Jupiter's luminosity, accretional heating, and the Sun. The position of the H 2 O ice line in the CPD, which is crucial for the formation of massive moons, is computed at various solar distances. We assess the loss of Galilean atmospheres due to high-energy radiation from the young Sun. Results. Ganymede and Callisto cannot have accreted their H 2 O during Jupiter's supposed GT, because its CPD (if still active) was too warm to host ices and much smaller than Ganymede's contemporary orbit. From a thermal perspective, the Galilean moons might have had significant atmospheres, but these would probably have been eroded during the GT in <10 5 yr by solar XUV radiation. Conclusions. Jupiter and the Galilean moons formed beyond 4.5 ± 0.5 AU and prior to the proposed GT. Thereafter, Jupiter's CPD would have been dry, and delayed accretion of planetesimals should have created water-rich Io and Europa. While Galilean atmospheres would have been lost during the GT, Titan would have formed after Saturn's own tack, because Saturn still accreted substantially for ≈10 6 yr after its closest solar approach, ending up at about 7 AU.

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Studies of the Problems of Planetary Cosmogony, Geochemistry and Cosmochemistry by Methods of Mathematical Modeling

Дорофеева

Dunaeva

Ипатов

et al. 2023

Advances in Geochemistry, Analytical Chemistry, and Planetary Sciences

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Accretion disks around Jupiter and Saturn at the stage of regular satellite formation

Cited by 37 publications

References 42 publications

Conditions for water ice lines and Mars-mass exomoons around accreting super-Jovian planets at 1−20 AU from Sun-like stars

Conditions for water ice lines and Mars-mass exomoons around accreting super-Jovian planets at 1−20 AU from Sun-like stars

The formation of the Galilean moons and Titan in the Grand Tack scenario

Studies of the Problems of Planetary Cosmogony, Geochemistry and Cosmochemistry by Methods of Mathematical Modeling

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