Formation of the Galilean Satellites: Conditions of Accretion
Open accessAbstract
We examine formation conditions for the Galilean satellites in the context of models of late-stage giant planet accretion and satellite-disk interactions. We first reevaluate the current standard, in which the satellites form from a "minimum mass subnebula" disk, obtained by augmenting the mass of the current satellites to solar abundance and resulting in a disk mass containing about 2% of Jupiter's mass. Conditions in such a massive and gas-rich disk are difficult to reconcile with both the icy compositions of Ganymede and Callisto and the protracted formation time needed to explain Callisto's apparent incomplete differentiation. In addition, we argue that disk torques in such a gas-rich disk would cause large satellites to be lost to inward decay onto the planet. These issues have prevented us from identifying a self-consistent scenario for the formation and survival of the Galilean satellites using the standard model. We then consider an alternative, in which the satellites form in a circumplanetary accretion disk produced during the very end stages of gas accretion onto Jupiter. In this case, an amount of gas and solids of at least ∼0.02 Jovian masses must still be processed through the disk during the satellite formation era, but this amount need not have been present all at once. We find that an accretion disk produced by a slow inflow of gas and solids, e.g., 2 × 10 -7 Jovian masses per year, is most consistent with conditions needed to form the Galilean satellites, including disk temperatures low enough for ices and protracted satellite accretion times of ≥10 5 yr. Such a "gas-starved" disk has an orders-of-magnitude lower gas surface density than the minimum mass subnebula (and for many cases is optically thin). Solids delivered to the disk build up over many disk viscous cycles, resulting in a greatly reduced gas-to-solids ratio during the final stages of satellite accretion. This allows for the survival of Galilean-sized satellites against disk torques over a wide range of plausible conditions.
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For Galilean satellites forming in the Jovian circumplanetary disk after dissipation, smaller values of ξ ~0.1-0.2 are found.
“For the Galilean satellites forming in the Jovian circumplanetary disk after dissipation, smaller values of ξ ∼ 0 . 1 -0 . 2 are found (Canup & Ward 2002; Magni & Coradini 2004; Ward & Canup 2010).”
From Mass and period limits on the ringed companion transiting the young star J1407 (2015) · cites this paper as Canup & Ward 2002
Section 1.4 uses 0.1 as a reference value for the disk scale-height ratio, and Section 3.3 discusses how that ratio varies across a circumjovian disk. Our copy does not identify it as ξ or report a range of 0.1–0.2 specifically for the satellite-forming disk after dissipation. (LLM, conf=0.70)
Experimental — accuracy not yet measuredSimulations indicate that ξ > 0.4 are unlikely.
“Simulations indicate that ξ > 0 . 4 are unlikely and that typical values are expected to be in the range of 0 . 1 < ξ < 0 . 3 (Quillen & Trilling 1998; Canup & Ward 2002; Magni & Coradini 2004; Ayliffe & Bate 2009; Ward & Canup 2010).”
From Mass and period limits on the ringed companion transiting the young star J1407 (2015) · cites this paper as Canup & Ward 2002
The Summary and Discussion gives a model requirement of specific angular momentum equivalent to 0.3–0.4 in units of Jupiter’s orbital frequency and Hill radius. It does not say simulations find values above 0.4 unlikely; instead, it says future hydrocode simulations may be able to test that requirement. (LLM, conf=0.83)
Experimental — accuracy not yet measuredThe lifetime of the second phase of Jupiter's circumstellar disk is estimated to be of order a million years.
“The lifetime of the second phase of Jupiter's circumstellar disk is estimated to be of order a million years (Canup & Ward 2002;Alibert et al. 2005;Ward & Canup 2010).”
From PLANETARY CONSTRUCTION ZONES IN OCCULTATION: DISCOVERY OF AN EXTRASOLAR RING SYSTEM TRANSITING A YOUNG SUN-LIKE STAR AND FUTURE PROSPECTS FOR DETECTING ECLIPSES BY CIRCUMSECONDARY AND CIRCUMPLANETARY DISKS (2012) · cites this paper as Canup & Ward 2002
Section 3.3 (page unavailable) uses 5 × 10^6 years as a characteristic timescale for gas inflow onto Jupiter, but says that slow inflow need persist for at least about 10^5 years to supply the satellites. It does not estimate a million-year lifetime for a “second phase” disk; the model concerns a circumjovian, or circumplanetary, disk rather than a circumstellar one. (LLM, conf=0.82)
Experimental — accuracy not yet measuredThe circumplanetary disk aspect ratio h/r is predicted to be in the range 0.1-0.3.
“The circumplanetary disk aspect ratio h/r is predicted to be in the range 0.1-0.3”
From PLANETARY CONSTRUCTION ZONES IN OCCULTATION: DISCOVERY OF AN EXTRASOLAR RING SYSTEM TRANSITING A YOUNG SUN-LIKE STAR AND FUTURE PROSPECTS FOR DETECTING ECLIPSES BY CIRCUMSECONDARY AND CIRCUMPLANETARY DISKS (2012) · cites this paper as Canup & Ward 2002
Section 3.3 describes a modeled circumplanetary disk whose aspect ratio increases with radius, and Section 3.4 uses approximately 0.1 as a disk value. The passages do not establish 0.3 as an upper bound or explicitly predict a 0.1–0.3 range (pages unavailable in our copy). (LLM, conf=0.82)
Experimental — accuracy not yet measuredAfter gas is cleared out of the planetary system, dust in the circumplanetary disk accretes into moons or remains as a ring system within the Roche limit of the planet.
“After the gas is cleared out of the planetary system, dust in the circumplanetary disk then accretes into moons or remains as a ring system within the Roche limit of the planet (Canup & Ward 2002;Magni & Coradini 2004;Ward & Canup 2010).”
From MODELING GIANT EXTRASOLAR RING SYSTEMS IN ECLIPSE AND THE CASE OF J1407B: SCULPTING BY EXOMOONS? (2015) · cites this paper as Canup & Ward 2002
Section 3.4 describes solids in a circumplanetary disk accumulating to form satellites. But Section 3 says satellite growth occurred while the final gas inflow was still present, not after gas was cleared. The passages do not support the alternative that solids remain as a ring within the planet’s Roche limit; page numbers were not available in our copy. (LLM, conf=0.87)
Experimental — accuracy not yet measured
If moons are present around gas giants, typical timescales for in-situ formation in a gaseous circumplanetary disk range from 10^5-10^6 years for gas-starved disk models down to 10^2-10^4 years for dense circumplanetary disks.
“If moons are present around gas giants, typical timescales for in-situ formation in a gaseous circumplanetary disk ranges from 10 5 -10 6 years for gas starved-disk models (Canup and Ward 2002;Szulágyi et al., 2018) down to 10 2 -10 4 years for dense circumplanetary disks (Lunine and Stevenson 1982).”
From A Self-Gravitating Exoring Around J1407b and Implications for In-Situ Exomoon Formation (2022) · cites this paper as Canup and Ward 2002
The Abstract and §4 (Summary and Discussion; page unavailable) describe gas-starved circumjovian disks with satellite accretion times of about 10^5 years. They do not establish the claimed range up to 10^6 years as a typical formation timescale for moons around gas giants generally. The dense-disk timescale is attached to a different citation, not Canup and Ward (2002). (LLM, conf=0.84)
Experimental — accuracy not yet measuredThe lack of differentiation of Callisto suggests that the accretion or formation timescale for all the Galilean satellites was prolonged and would have happened during the second phase of evolution after the circumstellar disk dissipated.
“The lack of differentiation of Callisto (Anderson et al. 1996) suggests that the accretion or formation timescale for all the Galilean satellites was prolonged (Canup & Ward 2002) and would have happened during the second phase of evolution after the circumstellar disk dissipated”
From PLANETARY CONSTRUCTION ZONES IN OCCULTATION: DISCOVERY OF AN EXTRASOLAR RING SYSTEM TRANSITING A YOUNG SUN-LIKE STAR AND FUTURE PROSPECTS FOR DETECTING ECLIPSES BY CIRCUMSECONDARY AND CIRCUMPLANETARY DISKS (2012) · cites this paper as Canup & Ward 2002
The existence of circumplanetary disks after the dissipation of the protosolar nebular disk has been postulated from formation scenarios for the Galilean satellites.
“The existence of circumplanetary disks after the dissipation of the protosolar (circumstellar) nebular disk has been postulated from formation scenarios for the Galilean satellites (Canup & Ward 2002;Magni & Coradini 2004;Ward & Canup 2010).”
From PLANETARY CONSTRUCTION ZONES IN OCCULTATION: DISCOVERY OF AN EXTRASOLAR RING SYSTEM TRANSITING A YOUNG SUN-LIKE STAR AND FUTURE PROSPECTS FOR DETECTING ECLIPSES BY CIRCUMSECONDARY AND CIRCUMPLANETARY DISKS (2012) · cites this paper as Canup & Ward 2002
Typical values of ξ are expected to be in the range 0.1 < ξ < 0.3.
“Simulations indicate that ξ > 0 . 4 are unlikely and that typical values are expected to be in the range of 0 . 1 < ξ < 0 . 3 (Quillen & Trilling 1998; Canup & Ward 2002; Magni & Coradini 2004; Ayliffe & Bate 2009; Ward & Canup 2010).”
From Mass and period limits on the ringed companion transiting the young star J1407 (2015) · cites this paper as Canup & Ward 2002
Sections 3.1–3.2 discuss circumjovian disk dimensions, and the Summary and Discussion gives a range for inflowing material’s specific angular momentum, but none identifies ξ or states that its typical values lie between 0.1 and 0.3. Searches for ξ, the stated range, and disk dimensions relative to the Hill radius did not find the claimed estimate in our copy; page numbers were unavailable. (LLM, conf=0.72)
Experimental — accuracy not yet measured
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Liquid water on Enceladus from observations of ammonia and 40Ar in the plume
Waite Jr, J. H., Lewis, W. S., Magee, B. A., Lunine, J. I., McKinnon, W. B., Glein, C. R., Mousis, O., Young, D. T., Brockwell, T., Westlake, J., et al. (2009) · Nature · doi:10.1038/nature08153 · Cited by 588 · see citing works
Morbidelli, A., Lunine, J., O'Brien, D., Raymond, S., & Walsh, K. (2012) · Annual Review of Earth and Planetary Sciences · doi:10.1146/annurev-earth-042711-105319 · Cited by 437 · see citing works
“In this case, the low content of short-lived radioactive elements might have allowed them to avoid differentiation, as in the cases of Callisto (Canup & Ward 2002) or Titan (Sotin et al. 2010).”
BackgroundA common mass scaling for satellite systems of gaseous planets
Canup, R., & Ward, W. (2006) · Nature · doi:10.1038/nature04860 · Cited by 314 · see citing works
“Continued satellite growth then occurs with an overall rate controlled by the rate of solid inflow 9 .”
BackgroundMethodInfluentialSelf-citationCapture of Irregular Satellites during Planetary Encounters
David Nesvorný, A., Vokrouhlický, D., & Morbidelli, A. (2007) · The Astronomical Journal · doi:10.1086/512850 · Cited by 233 · see citing works
DISTRIBUTION OF ACCRETING GAS AND ANGULAR MOMENTUM ONTO CIRCUMPLANETARY DISKS
Tanigawa, T., Ohtsuki, K., & Machida, M. N. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/747/1/47 · Cited by 230 · see citing works
“However, it was suggested that the MMSN model has difficulty in reproducing current satellite systems around Jupiter and Saturn (Canup & Ward 2002).”
BackgroundMethodOrbital and Collisional Evolution of the Irregular Satellites
Nesvorn, D., Alvarellos, J. L., Luke Dones, B., & Levison, H. F. (2003) · The Astronomical Journal · doi:10.1086/375461 · Cited by 226 · see citing works
FOMALHAUT'S DEBRIS DISK AND PLANET: CONSTRAINING THE MASS OF FOMALHAUT B FROM DISK MORPHOLOGY
Chiang, E., Kite, E., Kalas, P., Graham, J. R., & Clampin, M. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/693/1/734 · Cited by 223 · see citing works
“It is not clear, however, how such a disk would survive for the system age of ∼100 Myr; protosatellite disks are thought to evolve on timescales shorter than a few Myr (e.g., Canup & Ward 2002; Mosqueira & Estrada 2003).”
BackgroundKlein, B., Jura, M., Koester, D., Zuckerman, B., & Melis, C. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/709/2/950 · Cited by 126 · see citing works
“By mass, the Earth’s mantle4, Ceres and Callisto are 0.03 – 0.1%, 25%, and 50% water, respectively (van Thienen et al. 2007, McCord & Sotin 2005, Canup & Ward 2002, respectively).”
BackgroundInfluentialACCRETING CIRCUMPLANETARY DISKS: OBSERVATIONAL SIGNATURES
Zhu, Z. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/799/1/16 · Cited by 180 · see citing works
“…to circumplanetary disks can occur at high altitudes (Tanigawa et al. 2012, Szulagyi et al. 2014), the infall can carry little angular momentum (Canup & Ward 2002), the infall can be episodic (Gressel et al. 2013), the surface of the disk can be subject to magnetorotational instability (MRI)…”
BackgroundInterior composition, structure and dynamics of the Galilean satellites
Schubert, G., Anderson, J. D., Spohn, T., & McKinnon, W. B. (2004) · elib (German Aerospace Center) · Cited by 171 · see citing works
Ayliffe, B. A., & Bate, M. R. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15002.x · Cited by 167 · see citing works
“Canup & Ward (2002) discuss the uncertainty in the nature of such a disc, whether it is an accretion circumplanetary disc or a spin-out disc.”
BackgroundResultInfluentialTIDALLY HEATED TERRESTRIAL EXOPLANETS: VISCOELASTIC RESPONSE MODELS
Henning, W. G., O'Connell, R. J., & Sasselov, D. D. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/707/2/1000 · Cited by 206 · see citing works
“Differential inwards migration is common in early solar systems (Thommes & Lissauer 2005) and planetary moon systems (Kley 1999; Canup & Ward 2002), and is a possible origin of the 1:2:4 resonant Laplace relation among the Jovian satellites (Peale & Lee 2002).”
BackgroundFormation of Regular Satellites from Ancient Massive Rings in the Solar System
Crida, A., & Charnoz, S. (2012) · Science · doi:10.1126/science.1226477 · Cited by 176 · see citing works
Origin of Saturn's Rings and Inner Moons by Mass Removal from a Lost Titan-Sized Satellite
Canup, R. M. (2010) · Nature · doi:10.1038/nature09661 · Cited by 166 · see citing works
“The Jovian and Saturnian regular satellites are believed to have formed within circumplanetary disks of gas and solids produced during the end stages of nebular gas inflow to the planets 6,8,9 .”
BackgroundORIGIN OF THE DIFFERENT ARCHITECTURES OF THE JOVIAN AND SATURNIAN SATELLITE SYSTEMS
Sasaki, T., Stewart, G. R., & Ida, S. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/714/2/1052 · Cited by 112 · see citing works
“This setting is the same as that adopted by Canup & Ward (2002, 2006).”
BackgroundMethodInfluentialIrregular Satellites of the Planets: Products of Capture in the Early Solar System
Jewitt, D. C., & Haghighipour, N. (2007) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.44.051905.092459 · Cited by 154 · see citing works
“Perhaps the mass flowed through the disk toward the planet, and was not all present at one time (Canup & Ward 2002, 2006).”
BackgroundThe recent formation of Saturn's moonlets from viscous spreading of the main rings
Charnoz, S., Salmon, J., & Crida, A. (2010) · Nature · doi:10.1038/nature09096 · Cited by 135 · see citing works
Circumplanetary disc or circumplanetary envelope?
Szulágyi, J., Masset, F. S., Lega, E., Crida, A., Morbidelli, A., & Guillot, T. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw1160 · Cited by 146 · see citing works
“…(CPD) formed around massive giant planets is twofold: this subdisk regulates the growth of the planet in the last stages (e.g. Lissauer et al. 2009; Rivier et al. 2012; Szulágyi et al. 2014), and it is the birth-nest for satellites to form (Canup & Ward 2002, 2006; Mosqueira & Estrada 2003a,b).”
BackgroundMamajek, E. E., Quillen, A. C., Pecaut, M. J., Moolekamp, F., Scott, E. L., Kenworthy, M. A., Cameron, A. C., & Parley, N. R. (2012) · The Astronomical Journal · doi:10.1088/0004-6256/143/3/72 · Cited by 140 · see citing works
“Studies of primordial circumplanetary disks have calculated their thermal structure (Canup & Ward 2002; Alibert et al. 2005).”
BackgroundMethodInfluentialInternal structure of Europa and Callisto
Kuskov, O. L., & Kronrod, V. A. (2005) · Icarus · doi:10.1016/j.icarus.2005.04.014 · Cited by 137 · see citing works
Gressel, O., Nelson, R. P., Turner, N. J., & Ziegler, U. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/779/1/59 · Cited by 130 · see citing works
“The inclusion of magnetic field leads to a further reduced disk mass. Generally, the observed surface densities are in the range of the “gas-starved” scenario of Canup & Ward (2002, 2006), which is significantly lower than in the “minimum mass” models of Mosqueira & Estrada (2003).”
ResultRing Particle Composition and Size Distribution
Cuzzi, J., Clark, R., Filacchione, G., French, R., Johnson, R. E., Marouf, E., & Spilker, L. (2009) · Springer eBooks · doi:10.1007/978-1-4020-9217-6_15 · Cited by 124 · see citing works
Formation, Habitability, and Detection of Extrasolar Moons
Heller, R., Williams, D. M., Kipping, D., Limbach, M., Turner, E., Greenberg, R., Sasaki, T., Bolmont, É., Grasset, O., Lewis, K., et al. (2014) · Astrobiology · doi:10.1089/ast.2014.1147 · Cited by 109 · see citing works
“…minimum mass model (Mosqueira and Estrada, 2003a, 2003b; Estrada et al., 2009), another one is an actively supplied gaseous accretion disk model (Canup and Ward, 2002, 2006, 2009), and a third one relies on the viscous spreading of a massive disk inside the planet’s Roche limit (Crida and…”
InfluentialDid Saturn's rings form during the Late Heavy Bombardment?
Charnoz, S., Morbidelli, A., Dones, L., & Salmon, J. (2008) · Icarus · doi:10.1016/j.icarus.2008.10.019 · Cited by 107 · see citing works
“In recent years, it has been proposed that regular satellites of the giant planets form in “gas-starved” circumplanetary disks (Canup and Ward, 2002, 2006).”
BackgroundMODELING GIANT EXTRASOLAR RING SYSTEMS IN ECLIPSE AND THE CASE OF J1407B: SCULPTING BY EXOMOONS?
Kenworthy, M. A., & Mamajek, E. E. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/800/2/126 · Cited by 123 · see citing works
“After the gas is cleared out of the planetary system, dust in the circumplanetary disk then accretes into moons or remains as a ring system within the Roche limit of the planet (Canup & Ward 2002; Magni & Coradini 2004; Ward & Canup 2010).”
BackgroundChen, W., Hua, S., & Ge, S. S. (2014) · Automatica · doi:10.1016/j.automatica.2014.07.020 · Cited by 123 · see citing works
“Other representative works on the adaptive NN control for discrete-time systems are found in Chen and Khalil (1995), Jagannathan and Lewis (1996), He and Jagannathan (2007), Yang, Ge, Xiang, Chai, and Lee (2008), Zhang, Lou, and Liu (2009), Zhang, Song, Wei, and Zhang (2011).”
BackgroundInfluentialLarge Ocean Worlds with High-Pressure Ices
Journaux, B., Kalousová, K., Sotin, C., Tobie, G., Vance, S. D., Saur, J., Bollengier, O., Noack, L., Rückriemen‐Bez, T., Hoolst, T. V., et al. (2020) · Space Science Reviews · doi:10.1007/s11214-019-0633-7 · Cited by 123 · see citing works
Thermohydrodynamics of Circumstellar Disks with High‐Mass Planets
D’Angelo, G., Henning, T. K., & Kley, W. (2003) · The Astrophysical Journal · doi:10.1086/379224 · Cited by 123 · see citing works
“All of these properties appear to be consistent with the “fast-inflow” analytical models of protojovian disks recently developed by Canup & Ward (2002).”
ResultEvolution of Titan's rocky core constrained by Cassini observations
Castillo-Rogez, J. C., & Lunine, J. I. (2010) · Geophysical Research Letters · doi:10.1029/2010gl044398 · Cited by 122 · see citing works
Bowler, B. P., Liu, M. C., Kraus, A. L., Mann, A. W., & Ireland, M. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/743/2/148 · Cited by 116 · see citing works
“In our Solar System the regular satellites of the giant planets are fossil records of these structures (Canup & Ward 2002) and the excess optical emission from Fomalhaut b has been attributed to scattering from an enormous disk around that extrasolar planet (Kalas et al. 2008).”
BackgroundMcKinnon, W. B., & ZOLENSKY, M. E. (2003) · Astrobiology · doi:10.1089/153110703322736150 · Cited by 119 · see citing works
“This is especially true for a slowly accreted Europa, appropriate to formation in a gas-starved disk (Canup and Ward, 2002), in which most of Europa’s water would have initially been trapped at depth, predominantly as hydrated silicates.”
BackgroundInfluentialLate origin of the Saturn system
Asphaug, E. I., & Reufer, A. (2012) · Icarus · doi:10.1016/j.icarus.2012.12.009 · Cited by 118 · see citing works
“Although the framework is certainly debated, it is believed that major satellites accrete from ices and silicates in the sub-nebulae of giant planets, analogous to miniature solar systems (Canup & Ward, 2002; Mosqueira & Estrada, 2003).”
BackgroundHEK. VI. On the Dearth of Galilean Analogs in Kepler, and the Exomoon Candidate Kepler-1625b I
Teachey, A., Kipping, D., & Schmitt, A. R. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/aa93f2 · Cited by 117 · see citing works
“For the regular satellites of Jupiter, the Galilean moons are thought to have condensed out of a circumplanetary disk, akin to planet formation within a protoplanetary disk (Canup & Ward 2002).”
BackgroundCIRCUMPLANETARY DISK FORMATION
Ward, W. R., & Canup, R. M. (2010) · The Astronomical Journal · doi:10.1088/0004-6256/140/5/1168 · Cited by 116 · see citing works
“A viscous protosatellite disk has been invoked by Coradini et al. (1989), Canup & Ward (2002, 2006), Alibert et al. (2005), and Sasaki et al. (2010), and perhaps the most compelling argument for this is that viscous diffusion allows most of the disk’s mass to evolve inward and be accreted by the…”
BackgroundMethodResultInfluentialSelf-citationEnvironments, needs and opportunities for future space photovoltaic power generation: A review
Bermudez-Garcia, A., Voarino, P., & Raccurt, O. (2021) · Applied Energy · doi:10.1016/j.apenergy.2021.116757 · Cited by 115 · see citing works
Morbidelli, A., Tsiganis, K., Batygin, K., Crida, A., & Gomes, R. (2012) · Icarus · doi:10.1016/j.icarus.2012.03.025 · Cited by 112 · see citing works
“It is likely that the giant collision that tilted Uranus occurred during the accretion phase of the planet, when satellites were not yet formed and the planet was surrounded by a tenuous disk of gas, very rich in solids, similar to that usually invoked for the formation of satellites around giant planets (Canup and Wa…”
BackgroundLikely detection of water-rich asteroid debris in a metal-polluted white dwarf
Raddi, R., Gänsicke, B. T., Koester, D., Farihi, J., Hermes, J. J., Scaringi, S., Breedt, E., & Girven, J. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv701 · Cited by 113 · see citing works
Spin-Orbit Secondary Resonance Dynamics of Enceladus
Wisdom, J. (2004) · The Astronomical Journal · doi:10.1086/421360 · Cited by 107 · see citing works
“The starting point for their deliberations is the Canup & Ward (2002) model for the formation of the Galilean satellites.”
BackgroundScience Goals and Mission Architecture of the Europa Lander Mission Concept
Hand, K. P., Phillips, C. B., Murray, A. E., Garvin, J. B., Maize, E. H., Gibbs, R., Reeves, G., Martin, A. M. S., Tan-Wang, G., Krajewski, J., et al. (2022) · The Planetary Science Journal · doi:10.3847/psj/ac4493 · Cited by 104 · see citing works
“…ocean has likely persisted for much of the history of the solar system, potentially providing a long-term, stable environment in which a second, independent origin of life might have arisen (Canup & Ward 2002; Hussmann & Spohn 2004; Moore et al. 2009; Hand et al. 2009; Russell et al. 2017).”
BackgroundTidal truncation of circumplanetary discs
Martin, R. G., & Lubow, S. H. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.18228.x · Cited by 134 · see citing works
“This fact has motivated a dynamical explanation in terms of circumplanetary disc sizes (e.g. Canup & Ward 2002; Mosqueira & Estrada 2003).”
BackgroundMethodResultInfluentialRenaud, J. P., & Henning, W. G. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aab784 · Cited by 99 · see citing works
“Alternatively, migration may occur inwards (Canup & Ward 2002, 2009; Peale & Lee 2002), as may analogously occur in exoplanet systems as Type I migration (e.g., Udry et al. 2003; Ida & Lin 2008), due to magnetohydrodynamic torques induced by each moon within a primordial gas/dust disk out of which…”
BackgroundBae, J., Zhu, Z., Baruteau, C., Benisty, M., Dullemond, C. P., Facchini, S., Isella, A., Keppler, M., Pérez, L. M., & Teague, R. D. (2019) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ab46b0 · Cited by 101 · see citing works
“Also, this picture is similar to some Galilean satellite formation models in the protoJovian disk (e.g., Canup & Ward 2002).”
MethodCapture of planets into mean-motion resonances and the origins of extrasolar orbital architectures
Batygin, K. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1063 · Cited by 99 · see citing works
“…as orbital changes induced by tides raised on the host planet are considered to be the dominant driving mechanism16 responsible 16 See however, Peale & Lee (2002) and Canup & Ward (2002) for for resonant pairs of satellites in the Solar System (Goldreich 1965; Peale 1976, 1986; Henrard 1983).”
BackgroundSubsurface Water Oceans on Icy Satellites: Chemical Composition and Exchange Processes
Sohl, F., Choukroun, M. N., Kargel, J. S., Kimura, J., Pappalardo, R. T., Vance, S. D., & Zolotov, M. Y. (2010) · Space Science Reviews · doi:10.1007/s11214-010-9646-y · Cited by 98 · see citing works
“…of Aqueous Fluids The satellites of the giant planets are thought to have originated from a compositionally diverse mixture of grains that slowly accumulated from the surrounding solar accretion disk (Canup and Ward 2002, 2009; Mosqueira et al. 2010, this issue; Coradini et al. 2010, this issue).”
BackgroundA Metamorphic Origin for Europa's Ocean
Daswani, M. M., Vance, S. D., Mayne, M. J., & Glein, C. R. (2021) · Geophysical Research Letters · doi:10.1029/2021gl094143 · Cited by 98 · see citing works
“…amounts of water ice as a function of the (possibly migrating) position of the circumjovian snow line toward the late stages of accretion (e.g., Canup & Ward, 2002, 2009; Lunine & Stevenson, 1982; Makalkin et al., 1999; Ronnet et al., 2017), and/or capture and impact processing (e.g., Estrada…”
BackgroundA model for low‐temperature biogeochemistry of sulfur, carbon, and iron on Europa
Zolotov, M. Y., & Shock, E. L. (2004) · Journal of Geophysical Research Atmospheres · doi:10.1029/2003je002194 · Cited by 97 · see citing works
“[8] According to the gas-starved disc model of Canup and Ward [2002], the Galilean satellites formed from a mixture of water ice and a rocky component that accumulated from the surrounding solar nebula rather than condensing in a high-pressure Jovian subnebula.”
MethodSEARCHING FOR CIRCUMPLANETARY DISKS AROUND LkCa 15
Isella, A., Chandler, C. J., Carpenter, J. M., Pérez, L. M., & Ricci, L. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/788/2/129 · Cited by 94 · see citing works
“…suggest that the truncation of a circumplanetary disk by the stellar gravitational field might occur between 0.1 rH and 0.7 rH (see, e.g., Canup & Ward 2002; D’Angelo et al. 2002; Szulagyi et al. 2013; Ward & Canup 2010), where rH = Rp 3 √ Mp/3M? is the planet Hill radius, Rp is the…”
BackgroundMethodInfluentialOn the radio detectability of circumplanetary discs
Zhu, Z., Andrews, S. M., & Isella, A. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1503 · Cited by 93 · see citing works
“On the other hand, the other satellite formation model, so-called “gas-starved”disc model (Canup & Ward 2002), has a much lower surface density.”
BackgroundMethodFormation of Giant Planet Satellites
Batygin, K., & Morbidelli, A. (2020) · Astrophysical Journal · doi:10.3847/1538-4357/ab8937 · Cited by 75 · see citing works
“In this manner, the circum-Jovian disk considered by Canup & Ward (2002) is not required to retain the full mass budget of the Galilean satellites at any one time, and can instead remain in quasi-steady state with relatively low density.”
BackgroundMethodResultInfluentialAngular Momentum Accretion onto a Gas Giant Planet
Machida, M. N., Kokubo, E., Inutsuka, S., & Matsumoto, T. (2008) · The Astrophysical Journal · doi:10.1086/590421 · Cited by 93 · see citing works
X-RAY AND INFRARED OBSERVATIONS OF TWO EXTERNALLY POLLUTED WHITE DWARFS
Jura, M. A., Muno, M. P., Farihi, J., & Zuckerman, B. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/699/2/1473 · Cited by 92 · see citing works
“An alternative model to explain simultaneously all of this star’s distinctive properties is that we are witnessing the consequences of the tidal-destruction of a single parent body at least as massive as Callisto and probably as massive as Mars.”
BackgroundMethodInfluentialOrigin of the Ganymede–Callisto dichotomy by impacts during the late heavy bombardment
Barr, A. C., & Canup, R. M. (2010) · Nature Geoscience · doi:10.1038/ngeo746 · Cited by 90 · see citing works
“Such a state is probable if the satellites formed in a cold, ‘gas-starved’ disk around Jupiter produced during the final stages of slow gas accretion by the planet 10,11,27 .”
BackgroundSelf-citationCLATHRATION OF VOLATILES IN THE SOLAR NEBULA AND IMPLICATIONS FOR THE ORIGIN OF TITAN'S ATMOSPHERE
Mousis, O. J., Lunine, J. I., Thomas, C., Pasek, M. A., Marboeuf, U., Alibert, Y., Ballenegger, V., Cordier, D., Ellinger, Y., Pauzat, F., et al. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/691/2/1780 · Cited by 87 · see citing works
“…we assume that solid material has been supplied essentially by the direct transport of gas-coupled solids into the disk with the gas inflow during the first phase of the subnebula’s evolution or by capture of heliocentrically orbiting solids as they pass through the disk (Canup & Ward 2002, 2006).”
BackgroundOn the Habitability and Future Exploration of Ocean Worlds
Hand, K. P., Sotin, C., Hayes, A. G., & Coustenis, A. (2020) · Space Science Reviews · doi:10.1007/s11214-020-00713-7 · Cited by 86 · see citing works
Barr, A. C., & Canup, R. M. (2008) · Icarus · doi:10.1016/j.icarus.2008.07.004 · Cited by 86 · see citing works
Self-citationConstraints on Mimas’ interior from Cassini ISS libration measurements
Tajeddine, R., Rambaux, N., Lainey, V., Charnoz, S., Richard, A., Rivoldini, A., & Noyelles, B. (2014) · Science · doi:10.1126/science.1255299 · Cited by 86 · see citing works
Evidence for a Circumplanetary Disk around Protoplanet PDS 70 b
Christiaens, V., Cantalloube, F., Casassus, S., Price, D. J., Absil, O., Pinte, C., Girard, J. H., & Montesinos, M. (2019) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ab212b · Cited by 85 · see citing works
WATER ICE LINES AND THE FORMATION OF GIANT MOONS AROUND SUPER-JOVIAN PLANETS
Heller, R., & Pudritz, R. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/806/2/181 · Cited by 42 · see citing works
“In the Canup & Ward (2002) and the Mosqueira & Estrada (2003) models, the accretion rate onto Jupiter was assumed to be time-independent.”
BackgroundCAPTURE AND EVOLUTION OF PLANETESIMALS IN CIRCUMJOVIAN DISKS
D’Angelo, G., & Podolak, M. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/806/2/203 · Cited by 84 · see citing works
“If we apply a gasdominated opacity, κR = 10 −4 cm2 g−1, as contemplated in some of the models of Canup & Ward (2002), then Tg becomes about equal to the effective temperature Te, as can be seen by comparing the red and blue curves in the two panels of Figure 6.”
MethodThe orbital–thermal evolution and global expansion of Ganymede
Bland, M. T., Showman, A. P., & Tobie, G. (2008) · Icarus · doi:10.1016/j.icarus.2008.11.016 · Cited by 83 · see citing works
“A potential scenario for such expansion stems from the possibility that both Ganymede and Callisto formed undifferentiated (Canup and Ward, 2002), though see Mosqueira and Estrada (2003).”
BackgroundResultInfluentialApplication of the MEGNO technique to the dynamics of Jovian irregular satellites
Hinse, T. C., Christou, A. A., Alvarellos, J. L., & Goździewski, K. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16307.x · Cited by 82 · see citing works
“The regular Galilean satellites are thought to have formed by accretion processes within a circum-Jovian planetary disc (Canup & Ward 2002; Mosqueira & Estrada 2003; Estrada & Mosqueira 2006).”
BackgroundPineda, J. E., Szulágyi, J., Quanz, S. P., van Dishoeck, E. F., Garufi, A., Meru, F., Mulders, G. D., Testi, L., Meyer, M. R., & Reggiani, M. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/aaf389 · Cited by 81 · see citing works
“On the other hand, the current CPD mass limits are consistent with the “gas-starved” disk scenario proposed by Canup & Ward (2002, 2006), as well as the numerical simulations by Szulágyi (2017) that show a correlation between CPD mass and CSD mass.”
Amalthea's Density Is Less Than That of Water
Anderson, J. D., Johnson, T. V., Schubert, G., Asmar, S. W., Jacobson, R. A., Johnston, D., Lau, E. L., Lewis, G. D., Moore, W. B., Taylor, A. H., et al. (2005) · Science · doi:10.1126/science.1110422 · Cited by 81 · see citing works
NEBULAR WATER DEPLETION AS THE CAUSE OF JUPITER'S LOW OXYGEN ABUNDANCE
Mousis, O. J., Lunine, J. I., Madhusudhan, N., & Johnson, T. V. (2012) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/751/1/l7 · Cited by 80 · see citing works
“In this case, the Jovian subnebula would be cold enough to allow formation of regular icy satellites from building blocks produced in the solar nebula (Canup & Ward 2002; Mousis & Gautier 2004; Alibert et al. 2005d).”
BackgroundA Systematic Study of the Final Masses of Gas Giant Planets
Tanigawa, T., & Ikoma, M. (2007) · The Astrophysical Journal · doi:10.1086/520499 · Cited by 79 · see citing works
“Satellites are likely to form in subdisks around accreting gas giant planets (e.g., Canup & Ward 2002, 2006).”
BackgroundTHE SURVIVAL OF WATER WITHIN EXTRASOLAR MINOR PLANETS
Jura, M., & Xu, S.-Y. (2010) · The Astronomical Journal · doi:10.1088/0004-6256/140/5/1129 · Cited by 57 · see citing works
“Jura et al. (2009) proposed that the hydrogen in the outer mixing zone of GD 362, a helium white dwarf, may have resulted from the accretion of a a parent body at least as massive as Callisto which has a radius of 2400 km3.”
BackgroundEffects of the Planetary Temperature on the Circumplanetary Disk and on the Gap
Szulágyi, J. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa7515 · Cited by 78 · see citing works
“The timescale of this is still unknown (Canup & Ward 2002, 2006; Estrada et al. 2009; Mosqueira & Estrada 2003a,b) and certainly depends on number of factors, such as semi-major axis, opacity of the gas and dust, the temperature and cooling rate of the planet.”
BackgroundTIDAL HEATING IN MULTILAYERED TERRESTRIAL EXOPLANETS
Henning, W. G., & Hurford, T. A. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/789/1/30 · Cited by 75 · see citing works
“…appear common and stable among exoplanet systems (Marcy et al. 2001; Lee & Peale 2002; Lee 2004; Haghighipour et al. 2003; Lecoanet et al. 2009), likely due to systematic assembly during convergent migration (Yu & Tremaine 2001), perhaps analogously to the Galilean moon system (Canup & Ward 2002).”
BackgroundGas-drag-assisted capture of Himalia's family
Ćuk, M., & Burns, J. A. (2003) · Icarus · doi:10.1016/j.icarus.2003.09.026 · Cited by 76 · see citing works
“(1999), Canup and Ward (2002), and Mosquera and Estrada (2003).”
BackgroundMethodInfluentialThe Potential for Tidally Heated Icy and Temperate Moons around Exoplanets
Scharf, C. A. (2006) · The Astrophysical Journal · doi:10.1086/505256 · Cited by 75 · see citing works
“We also plot a hypothetical upper mass limit based on the minimum mass subnebula postulated for the Jovian system (Canup & Ward 2002).”
BackgroundMethodThe Origin and Evolution of Saturn, with Exoplanet Perspective
Atreya, S., Crida, A., Guillot, T., Lunine, J., Madhusudhan, N., & Mousis, O. (2016) · Saturn in the 21st Century · doi:10.1017/9781316227220.002 · Cited by 69 · see citing works
“In the first model, the satellite formation takes place in a dense and hot disk at the early stages of the gas giant planet formation (Prinn and Fegley, 1981, 1989; Lunine et al., 1989), while the other model uses a thin and cold disk to depict satellite formation (Canup and Ward, 2002).”
BackgroundMethodInterior structures and tidal heating in the TRAPPIST-1 planets
Barr, A. C., Dobos, V., & Kiss, L. L. (2017) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201731992 · Cited by 74 · see citing works
“In the context of our assumptions, a planet with ρ̄ = ρhpp would correspond to a planet composed of pure H2O, which we consider unlikely based on planet and satellite formation models (e.g., Canup and Ward 2002; Morbidelli et al. 2012; Johansen et al. 2015).”
A model for the interior structure, evolution, and differentiation of Callisto
Nagel, K., Breuer, D., & Spohn, T. (2004) · Icarus · doi:10.1016/j.icarus.2003.12.019 · Cited by 74 · see citing works
“The satellitesimals, already consisting of rock/ice mixtures, can decouple from the gas and grow to satellites for sizes > 100 m (Canup and Ward, 2002; Mosqueira and Estrada, 2003a).”
BackgroundA gas-poor planetesimal capture model for the formation of giant planet satellite systems
Estrada, P. R., & Mosqueira, I. (2006) · Icarus · doi:10.1016/j.icarus.2005.11.006 · Cited by 73 · see citing works
“Along the lines of the prior section, except that satellitesimals are confined to a circumplanetary disk with scale-height H2, we first estimate the mass rate per unit area undergoing collisions between planetesimals and satellitesimals of comparable size.”
BackgroundInvestigating Europa’s Habitability with the Europa Clipper
Vance, S. D., Craft, K. L., Shock, E. L., Schmidt, B. E., Lunine, J. I., Hand, K. P., McKinnon, W. B., Spiers, E. M., Chivers, C. J., Lawrence, J., et al. (2023) · Space Science Reviews · doi:10.1007/s11214-023-01025-2 · Cited by 79 · see citing works
“The temperature gradient of the circumplanetary disk may have induced partial devolatilization of the satellite’s building blocks (Canup and Ward 2002), whereas accretional heating may have led to hydrodynamic escape of a primary ocean (Bierson and Nimmo 2020), or both may have occurred.”
Background“TAIL-END” BONDI-HOYLE ACCRETION IN YOUNG STAR CLUSTERS: IMPLICATIONS FOR DISKS, PLANETS, AND STARS
Throop, H. B., & Bally, J. (2008) · The Astronomical Journal · doi:10.1088/0004-6256/135/6/2380 · Cited by 73 · see citing works
“In some ways the accretion flow onto the disk can be compared to the proto-Jovian nebula “starved disk” model of Canup & Ward (2002), where gas accretes from the solar nebula disk onto the circum-Jovian disk orbiting within it.”
Origin of Water Ice in the Solar System
Lunine, J. I. (2006) · University of Arizona Press eBooks · doi:10.2307/j.ctv1v7zdmm.21 · Cited by 71 · see citing works
ON THE VIABILITY OF THE MAGNETOROTATIONAL INSTABILITY IN CIRCUMPLANETARY DISKS
Fujii, Y., Okuzumi, S., Tanigawa, T., & Inutsuka, S. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/785/2/101 · Cited by 44 · see citing works
“There have been several theoretical studies of satellite formation in disks (e.g., Lunine & Stevenson 1982; Canup & Ward 2002, 2006; Mosqueira & Estrada 2003a,b; Canup & Ward 2009; Estrada et al. 2009; Sasaki et al. 2010; Ogihara & Ida 2012).”
BackgroundMethodInfluentialA whole-moon thermal history model of Europa: Impact of hydrothermal circulation and salt transport
Travis, B. J., Palguta, J., & Schubert, G. (2012) · Icarus · doi:10.1016/j.icarus.2012.02.008 · Cited by 70 · see citing works
ECCENTRICITY TRAP: TRAPPING OF RESONANTLY INTERACTING PLANETS NEAR THE DISK INNER EDGE
Ogihara, M., Duncan, M. J., & Ida, S. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/721/2/1184 · Cited by 68 · see citing works
“Based on the slow inflow disk model (e.g., Canup & Ward 2002, 2006), cs/vK ∼ 0.06 and we found through a preliminary N -body simulation that e ∼ 0.1 for resonantly trapped satellites.”
MethodInfluentialTHE CENTER OF LIGHT: SPECTROASTROMETRIC DETECTION OF EXOMOONS
Agol, E., Jansen, T., Lacy, B. I., Robinson, T. D., & Meadows, V. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/812/1/5 · Cited by 67 · see citing works
“…around giant planets have been tailored for the Solar System to reproduce, for example, the mass ratio of 10−4 observed for the satellite systems of the giant planets (Canup & Ward 2002; Sasaki et al. 2010), so that giant planets may harbor satellites as large as 0.7R⊕ (Heller & Pudritz 2015b).”
BackgroundMethodORBITAL PERTURBATIONS OF THE GALILEAN SATELLITES DURING PLANETARY ENCOUNTERS
Deienno, R., David Nesvorný, A., Vokrouhlický, D., & Yokoyama, T. (2014) · The Astronomical Journal · doi:10.1088/0004-6256/148/2/25 · Cited by 67 · see citing works
“…MMR with Ganymede (potentially driven there when satellites radially migrated by interacting with the circumplanetary gas nebula, or when Ganymede was pushed out by tides (Yoder & Peale 1981; Canup & Ward 2002, 2006, 2009)), and Callisto was kicked out of the resonance during planetary encounters.”
BackgroundNonhydrostatic effects and the determination of icy satellites’ moment of inertia
Gao, P., & Stevenson, D. J. (2013) · Icarus · doi:10.1016/j.icarus.2013.07.034 · Cited by 66 · see citing works
“This interpretation has influenced models for satellite formation such 70 as the “gas-starved disk” model for the Galilean moons (Stevenson 2001; Canup and Ward 2002), and 71 alternative ways of reducing accretion heating through lengthening the timescale of accretion (e.g. 72 Mosqueira and…”
BackgroundMethodInfluentialMousis, O. J., & Gautier, D. (2004) · Planetary and Space Science · doi:10.1016/j.pss.2003.06.004 · Cited by 66 · see citing works
“Similar conclusions can be derived from the model proposed by Canup and Ward (2002), shown for comparison in Figs.”
BackgroundMethodResultInfluentialQuasi-static contraction during runaway gas accretion onto giant planets
Lambrechts, M., Lega, E., Nelson, R., Crida, A., & Morbidelli, A. (2019) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201834413 · Cited by 40 · see citing works
“In the context of the Solar System, the apparent lack of circumplanetary discs, at least around the lower mass planets in the ice giant mass-regime, argues against scenarios where regular satellites form in circumplanetary discs (Canup & Ward 2002).”
BackgroundCanup, R. M., Righter, K., Dauphas, N., Pahlevan, K., Ćuk, M., Lock, S. J., Stewart, S. T., Salmon, J. J., Rufu, R., Nakajima, M., et al. (2023) · Reviews in Mineralogy and Geochemistry · doi:10.2138/rmg.2023.89.02 · Cited by 64 · see citing works
Self-citationThe Origin and Evolution of Titan
Lunine, J. I., Choukroun, M. N., Stevenson, D. J., & Tobie, G. (2009) · Springer eBooks · doi:10.1007/978-1-4020-9215-2_3 · Cited by 66 · see citing works
THE FATE OF MOONS OF CLOSE-IN GIANT EXOPLANETS
Namouni, F. (2010) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/719/2/l145 · Cited by 65 · see citing works
“Planetary satellites form in the circumplanetary nebula over time scales from 103 to 107 years (Canup and Ward 2002, 2006, Mosqueira and Estrada 2003a,b, Sasaki et al. 2010).”
BackgroundInterior structures and tidal heating in the TRAPPIST-1 planets
Barr, A. C., Dobos, V., & Kiss, L. L. (2018) · Repository of the Academy's Library (Library of the Hungarian Academy of Sciences) · doi:10.1051/0004-6361/201731992/pdf · Cited by 64 · see citing works
Odert, P., Lammer, H., Erkaev, N., Nikolaou, A., Lichtenegger, H., Johnstone, C., Kislyakova, K., Leitzinger, M., & Tosi, N. (2017) · Icarus (New York, N.Y. 1962) · doi:10.1016/j.icarus.2017.10.031 · Cited by 58 · see citing works
“resemble planetary embryos (such as Earth’s Moon, Mars, the asteroid Vesta, and dwarf planets like Ceres) shows that they have been dierentiated in their interiors like the terrestrial planets (e.g. Canup and Ward, 2002; Schubert et al., 2004; Thomas et al., 2005; Russell et al., 2013). It is thus reasonable to expect…”
BackgroundFormation of Titan in Saturn's subnebula : constraints from Huygens probe measurements
Alibert, Y., & Mousis, O. (2007) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20066402 · Cited by 54 · see citing works
Origin and Evolution of Saturn's Ring System
Charnoz, S., Luke Dones, B., Esposito, L. W., Estrada, P. R., & Hedman, M. M. (2009) · Springer eBooks · doi:10.1007/978-1-4020-9217-6_17 · Cited by 61 · see citing works
Shabram, M., & Boley, A. C. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/767/1/63 · Cited by 60 · see citing works
“These processes have largely been explored in the context of thin-disk theory (e.g., Canup & Ward 2002), so simulations of gas-solid coupling and satellite migration in the context of disks with large scaleheights should be conducted.”
BackgroundMethodPerryman, M. A. C. (2011) · Cambridge University Press eBooks · doi:10.1017/cbo9780511994852.011 · Cited by 71 · see citing works
Schubert, G., Hußmann, H., Lainey, V. J., Matson, D. L., McKinnon, W. B., Sohl, F., Sotin, C., Tobie, G., Turrini, D., & Hoolst, T. V. (2010) · Space Science Reviews · doi:10.1007/s11214-010-9635-1 · Cited by 60 · see citing works
“Peale and Lee (2002) showed how such a scenario could be established by taking into account interactions with the Jovian gas-disk based on the accretion model of Canup and Ward (2002).”
BackgroundRESONANT REMOVAL OF EXOMOONS DURING PLANETARY MIGRATION
Spalding, C., Batygin, K., & Adams, F. C. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/817/1/18 · Cited by 59 · see citing works
“(13) As mentioned earlier, we consider inward planetary migration (increasing np), but do not explicitly consider the case where the moon itself is migrating within a circumplanetary disk (Canup & Ward 2002).”
BackgroundInfluentialEvidence for a Circumplanetary Disk around Protoplanet PDS 70 b
Christiaens, V., Cantalloube, F., Casassus, S., Price, D. J., Absil, O., Pinte, C., Girard, J. H., & Montesinos, M. (2019) · MPG.PuRe (Max Planck Society) · Cited by 58 · see citing works
The oxidation state of hydrothermal systems on early Enceladus
Glein, C. R., Zolotov, M. Y., & Shock, E. L. (2008) · Icarus · doi:10.1016/j.icarus.2008.03.021 · Cited by 58 · see citing works
“A similar argument applies to CO2 because it would not have been a major species in the outer region of the solar nebula (the solar nebula is discussed because the dense subnebula concept is outdated; see Canup and Ward, 2002).”
BackgroundInteriors and Evolution of Icy Satellites
Hußmann, H., Sotin, C., & Lunine, J. I. (2015) · Elsevier eBooks · doi:10.1016/b978-0-444-53802-4.00178-0 · Cited by 58 · see citing works
Szulágyi, J., Mayer, L., & Quinn, T. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2617 · Cited by 45 · see citing works
“The two widely accepted planet formation theories, core accretion (Pollack et al. 1996) and gravitational instability (Boss 1997) both predict that circumplanetary disks form around giant planets (e.g. Quillen & Trilling 1998; Canup & Ward 2002; Ward & Canup 2010).”
Background
- Authors
- Canup, R. M., & Ward, W. R.
- Affiliations
- Southwest Research Institute (US)
- ORCID
- Canup, Robin M.
- Venue
- The Astronomical Journal
- Publisher
- American Astronomical Society
- Published
- 2002-12
- Volume
- 124
- Issue
- 6
- Pages
- 3404-3423
- ISSN
- 0004-6256 (ISSN-L)
- 1538-3881
- OpenAlex
- W2122237670
- Cited by
- 433
- References
- 69
- Citations by year
- 2026: 22 · 2025: 27 · 2024: 20 · 2023: 19 · 2022: 17 · 2021: 16 · 2020: 24 · 2019: 19 · 2018: 21 · 2017: 20 · 2016: 17 · 2015: 22 · 2014: 21 · 2013: 19 · 2012: 17
- FWCI
- 6.50
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astronomical Journal (publishedVersion)
- Funders
- National Aeronautics and Space Administration
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Keywords
- Galilean moons, satellite formation flying, Jupiter, icy satellites, Ganymede, Callisto
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