A common mass scaling for satellite systems of gaseous planets

Canup, R. M.; Ward, William R.

doi:10.1038/nature04860

Cited by 345 publications

(418 citation statements)

References 40 publications

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“…Canup & Ward (2002) proposed the so-called gas-starved disk model for the formation of regular satellites of giant planets, where the satellites are formed in a waning circumplanetary disk at the very end stage of giant planet formation. Canup & Ward (2006) performed N-body simulation of satellite formation based on the above model, and showed that mass fraction of satellite system relative to the host planet is regulated to ∼ 10 −4 , which is consistent with observations. Later studies revised this model and tried to explain the difference between the satellite systems of Jupiter and Saturn (Sasaki et al 2010;Ogihara & Ida 2012).…”

Section: Introductionsupporting

confidence: 76%

Distribution of Captured Planetesimals in Circumplanetary Gas Disks and Implications for Accretion of Regular Satellites

Suetsugu

Ohtsuki

2017

ApJ

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Regular satellites of giant planets are formed by accretion of solid bodies in circumplanetary disks. Planetesimals that are moving on heliocentric orbits and are sufficiently large to be decoupled from the flow of the protoplanetary gas disk can be captured by gas drag from the circumplanetary disk. In the present work, we examine the distribution of captured planetesimals in circumplanetary disks using orbital integrations. We find that the number of captured planetesimals reaches an equilibrium state as a balance between continuous capture and orbital decay into the planet. The number of planetesimals captured into retrograde orbits is much smaller than those on prograde orbits, because the former ones experience strong headwind and spiral into the planet rapidly. We find that the surface number density of planetesimals at the current radial location of regular satellites can be significantly enhanced by gas drag capture, depending on the velocity dispersions of planetesimals and the width of the gap in the protoplanetary disk. Using a simple model, we also examine the ratio of the surface densities of dust and captured planetesimals in the circumplanetary disk, and find that solid material at the current location of regular satellites can be dominated by captured planetesimals when the velocity dispersion of planetesimals is rather small and a wide gap is not formed in the protoplanetary disk. In this case, captured planetesimals in such a region can grow by mutual collision before spiraling into the planet, and would contribute to the growth of regular satellites.

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Section: Introductionsupporting

confidence: 76%

Distribution of Captured Planetesimals in Circumplanetary Gas Disks and Implications for Accretion of Regular Satellites

Suetsugu

Ohtsuki

2017

ApJ

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“…The dependence of the emission power on the exomoon's crosssectional area (pR S 2 ) leads to the question of how large exomoons can be. Formation models suggest that moons can form around Jovian planets with masses up to 10 −4 times the mass of their host planet (Canup & Ward 2006;Heller & Pudritz 2015). Therefore, large exoplanets of M 3 J or larger could form a Mars-sized exomoon, and M 10 J exoplanets could have several Mars-sized exomoons or larger (Heller & Pudritz 2015) (where M 1 J is one Jupiter mass).…”

Section: Basic Mechanismmentioning

confidence: 99%

On the Radio Detection of Multiple-Exomoon Systems Due to Plasma Torus Sharing

Noyola

Satyal

Musielak³

2016

ApJ

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The idea of single exomoon detection due to the radio emissions caused by its interaction with the host exoplanet is extended to multiple-exomoon systems. The characteristic radio emissions are made possible in part by plasma from the exomoon's own ionosphere. In this work, it is demonstrated that neighboring exomoons and the exoplanetary magnetosphere could also provide enough plasma to generate a detectable signal. In particular, the plasma-torus-sharing phenomenon is found to be particularly well suited to facilitate the radio detection of plasmadeficient exomoons. The efficiency of this process is evaluated, and the predicted power and frequency of the resulting radio signals are presented.

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“…(31)] required to enforce coherent disk precession or maintain misalignment of the outer disk may be difficult to achieve in the context of circumplanetary disk formation (e.g. Canup & Ward 2006). Moreover, a massive disk can suffer gravitational instability.…”

Section: Discussionmentioning

confidence: 99%

Extended transiting discs and rings around planets and brown dwarfs: theoretical constraints

Zanazzi¹,

Lai²

2016

Mon. Not. R. Astron. Soc.

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Newly formed planets (or brown dwarfs) may possess disks or rings that occupy an appreciable fraction of the planet's Hill sphere and extend beyond the Laplace radius, where the tidal torque from the host star dominates over the torque from the oblate planet. Such a disk/ring can exhibit unique, detectable transit signatures, provided that the disk/ring is significantly misaligned with the orbital plane of the planet. There exists tentative evidence for an extended ring system around the young K5 star 1 SWASP J140747-354542. We present a general theoretical study of the inclination (warp) profile of circumplanetary disks under the combined influences of the tidal torque from the central star, the torque from the oblate planet and the self-gravity of the disk. We calculate the equilibrium warp profile ("generalized Laplace surface") and investigate the condition for coherent precession of the disk. We find that to maintain non-negligible misalignment between the extended outer disk and the planet's orbital plane, and to ensure coherent disk precession, the disk surface density must be sufficiently large so that the self-gravity torque overcomes the tidal torque from the central star. Our analysis and quantitative results can be used to constrain the parameters of transiting circumplanetary disks that may be detected in the future.

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A common mass scaling for satellite systems of gaseous planets

Cited by 345 publications

References 40 publications

Distribution of Captured Planetesimals in Circumplanetary Gas Disks and Implications for Accretion of Regular Satellites

Distribution of Captured Planetesimals in Circumplanetary Gas Disks and Implications for Accretion of Regular Satellites

On the Radio Detection of Multiple-Exomoon Systems Due to Plasma Torus Sharing

Extended transiting discs and rings around planets and brown dwarfs: theoretical constraints

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