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CIRCUMPLANETARY DISK FORMATION

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Ward, William R., Canup, Robin M.·2010·The Astronomical Journal
DOI 10.1088/0004-6256/140/5/1168
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Abstract

The development and evolution of a circumplanetary disk during the accretion of a giant planet is examined. The planet gains mass and angular momentum from infalling solar nebula material while simultaneously contracting due to luminosity losses. When the planet becomes rotationally unstable it begins to shed material into a circumplanetary disk. Viscosity causes the disk to spread to a moderate fraction of the Hill radius where it is assumed that a small fraction of the material escapes back into heliocentric orbit, carrying away most of the excess angular momentum. As the planet's contraction continues, its radius can become smaller than the spatial range of the inflow and material begins to fall directly onto the disk, which switches from a spin-out disk to an accretion disk as the planet completes its growth. We here develop a description of the circumplanetary disk, which is combined with models of the planet's contraction and the inflow rate including its angular momentum content to yield a solution for the time evolution of a planet–disk system.

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Crossref · 10.1088/0004-6256/140/5/1168

Cites

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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 Ward & Canup 2010

    The Introduction (page unavailable) says Jupiter’s regular satellites likely formed in circumplanetary disks. But neither the Introduction nor the disk-model discussion reports ξ ≈ 0.1–0.2 for Galilean satellite formation after dissipation; searches for ξ, 0.1–0.2, and post-dissipation formation did not establish that result. (LLM, conf=0.82)

    Experimental — accuracy not yet measured

  • Recent explorations of circumplanetary disks separate the disk evolution into two phases.

    “Recent explorations of circumplanetary disks separate the disk evolution into two phases (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 Ward & Canup 2010

    The Abstract describes a transition from a spin-out disk to an accretion disk, supporting a broad two-phase description. But Section 3.2 (Inflow Stages) says the planet–disk configuration passes through three stages, and the Conclusion describes an intermediate period when both spin-out and direct inflow supply the disk. The paper therefore does not separate its full disk evolution into only two phases. (LLM, conf=0.84)

    Experimental — accuracy not yet measured

  • The 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 Ward & Canup 2010

    Section 3, “Disks with Ongoing Accretion” (page unavailable), describes stages of Jupiter’s circumplanetary disk and reports that Jupiter contracts to within Io’s orbit in less than a million years. The Figure 5 caption in Section 7 (page unavailable) uses a roughly million-year planet-accretion timescale. Neither passage estimates a million-year lifetime for a second phase of Jupiter’s circumstellar disk; the quoted timescales describe planetary contraction and accretion instead. (LLM, conf=0.78)

    Experimental — accuracy not yet measured

  • 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 Ward & Canup 2010

    The Introduction (page not provided) links circumplanetary disks to the formation of Jupiter’s regular satellites and describes satellite-formation disk models. It does not establish that those disks existed after the protosolar nebula dissipated; it also describes an accretion-disk scenario in which the solar nebula is still present. (LLM, conf=0.85)

    Experimental — accuracy not yet measured

  • After 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 Ward & Canup 2010

    The Introduction links circumplanetary disks to satellite formation, and the Conclusion discusses solids in a disk forming satellites. Neither passage says that, after gas is cleared, dust either accretes into moons or remains as rings within the planet’s Roche limit; searches for Roche limits and rings found no such passage. The indexed copy provides section labels but no page numbers. (LLM, conf=0.84)

    Experimental — accuracy not yet measured

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Cites

Flagged first, then by citations

1 of the 63 references couldn’t be matched to a known paper.

Research works printed but not linked: 8

  1. [11]11. Canup, R. M., & Ward, W. R. 2009, in Europa, ed. R. Pappalardo, W. K. McKinnon, & K. Khurana (Tucson, AZ: Univ. Arizona Press), 59
  2. [21]21. Estrada, P. R., Mosqueira, I., Lissauer, J. J., D'Angelo, D., & Cruikshank, D. P. 2009, in Europa, ed. R. Pappalardo, W. K. McKinnon, & K. Khurana (Tucson, AZ: Univ. Arizona Press), 27
  3. [49]49. Murray, C. D., & Dermott, S. 1999, Solor System Dynamics (Cambridge: Cambridge Univ. Press)
  4. [52]52. Pollack, J. B., & Consolmagno, G. 1984, in Saturn, ed. T. Gehrels & M. S. Matthews, M. (Tucson, AZ: Univ. of Arizona Press), 811
  5. [54]54. Pollack, J. B., Lunine, J. I., & Tittemore, W. C. 1991, in Uranus, ed. J. T. Bergstralh et al. (Tucson, AZ: Univ. Arizona Press), 469
  6. [60]60. Shu, F. H., Najita, J. R., Shang, H., & Zhi-Yun, L. 2000, in Protostars & Planets IV, ed. V. Mannings et al. (Tucson, AZ: Univ. Arizona Press), 789
  7. [61]61. Stevenson, D. J., Harris, A. W., & Lunine, J. I. 1986, in Satellites, ed. J. A. Burns & M. S. Matthews (Tucson, AZ: Univ. of Arizona Press), 39
  8. [62]62. Stone, J. M., Gammie, C. F., Balbus, S. A., & Hawley, J. F. 2000, in Protostars & Planets IV, ed. V. Mannings et al. (Tucson, AZ: Univ. Arizona Press), 589

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Authors
Ward, W. R., & Canup, R. M.
Affiliations
Southwest Research Institute (US)
ORCID
Canup, Robin M.
Venue
The Astronomical Journal
Publisher
American Astronomical Society
Published
2010-10-01
Volume
140
Issue
5
Pages
1168-1193
ISSN
  • 0004-6256 (ISSN-L)
  • 1538-3881
DOI
10.1088/0004-6256/140/5/1168
OpenAlex
W1966412445
Semantic Scholar
1d57a2571af074621056b5f6700ff83ad1a21af1
Cited by
116
References
63
Citations by year
2026: 8 · 2025: 5 · 2024: 6 · 2023: 4 · 2022: 3 · 2021: 5 · 2020: 6 · 2019: 8 · 2018: 25 · 2017: 5 · 2016: 7 · 2015: 5 · 2014: 7 · 2013: 4 · 2012: 5
FWCI
3.93
Type
journal article
Language
en
Open access
Locations
The Astronomical Journal (publishedVersion)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
Keywords
circumplanetary disks, giant planet formation, planetary accretion, angular momentum transport, accretion disks, disk viscosity, Hill radius

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