Type I planetary migration in a self-gravitating disk

Masset, F.

doi:10.1017/s1743921308016888

Cited by 5 publications

(7 citation statements)

References 19 publications

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“…However, Type-I migration is valid only in isothermal disks. Instead, it has recently been shown that migration can be outwards in disks that transport and dissipate heat inefficiently [43][44][45] .…”

Section: Defining a Plausible Evolution Scenario For The Giant Planetsmentioning

confidence: 99%

A low mass for Mars from Jupiter’s early gas-driven migration

Walsh¹,

Morbidelli²,

Raymond³

et al. 2011

Nature

1,162

1,303

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Jupiter and Saturn formed in a few million years (ref. 1) from a gas-dominated protoplanetary disk, and were susceptible to gas-driven migration of their orbits on timescales of only ∼100,000 years (ref. 2). Hydrodynamic simulations show that these giant planets can undergo a two-stage, inward-then-outward, migration. The terrestrial planets finished accreting much later, and their characteristics, including Mars' small mass, are best reproduced by starting from a planetesimal disk with an outer edge at about one astronomical unit from the Sun (1 au is the Earth-Sun distance). Here we report simulations of the early Solar System that show how the inward migration of Jupiter to 1.5 au, and its subsequent outward migration, lead to a planetesimal disk truncated at 1 au; the terrestrial planets then form from this disk over the next 30-50 million years, with an Earth/Mars mass ratio consistent with observations. Scattering by Jupiter initially empties but then repopulates the asteroid belt, with inner-belt bodies originating between 1 and 3 au and outer-belt bodies originating between and beyond the giant planets. This explains the significant compositional differences across the asteroid belt. The key aspect missing from previous models of terrestrial planet formation is the substantial radial migration of the giant planets, which suggests that their behaviour is more similar to that inferred for extrasolar planets than previously thought.

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Section: Defining a Plausible Evolution Scenario For The Giant Planetsmentioning

confidence: 99%

A low mass for Mars from Jupiter’s early gas-driven migration

Walsh¹,

Morbidelli²,

Raymond³

et al. 2011

Nature

1,162

1,303

View full text Add to dashboard Cite

show abstract

“…However, since the disk seems to be too massive for a planet to open a gap detectable at the current resolution 34 , observations at higher resolution are needed to search for a gap and check for this scenario. In addition, since it has been suggested that the spiral arms in Elias 2-27 are due to a so-far undetected external companion in the disk plane 11 , it is natural to ask whether the spiral arms in the VLA 1 disk can also be driven by an external companion.…”

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confidence: 99%

Spiral structures in an embedded protostellar disk driven by envelope accretion

Lee

Turner

2019

Nat Astron

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Hydrodynamical simulations show that a pair of spiral arms can form in the disk around a rapidly-growing young star and that the arms are crucial in transporting angular momentum as the disk accretes material from the surrounding envelope 1-4 . Here we report the detection of a pair of symmetric spiral structures in a protostellar disk, supporting the formation of spiral arms in the disk around a forming star. The HH 111 VLA 1 source is a young Class I source embedded in a massive infalling protostellar envelope and is actively accreting, driving the prominent HH 111 jet. Previous observations showed a ring of shock emission around the disk's outer edge 5 , indicating accretion of the envelope material onto the disk at a high rate. Now with ALMA observations of thermal emission from dust particles, we detect a pair of spiral arms extending from the inner region to the disk's outer edge, similar to that seen in many simulations 1-4 . Additionally, the disk is massive, with Toomre's Q parameter near unity in the outer parts where the spiral structures are detected, supporting the notion that

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“…( 18) we can infer that the relative mass growth, 1/m(dm/dt), for each object is important. Let us assume we start out with m 1 > m 2 , then we see that this ratio is increasing if the relative growth increases with m, because then the right-hand side in (18) is positive. This is exactly the situation for runaway-growth.…”

Section: Modes Of Growthmentioning

confidence: 98%

Planet Formation and Disk-Planet Interactions

Kley

2019

Saas-Fee Advanced Course

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This review is based on lectures given at the 45th Saas-Fee Advanced Course "From Protoplanetary Disks to Planet Formation" held in March 2015 in Les Diablerets, Switzerland. Starting with an overview of the main characterictics of the Solar System and the extrasolar planets, we describe the planet formation process in terms of the sequential accretion scenario. First the growth processes of dust particles to planetesimals and subsequently to terrestrial planets or planetary cores are presented. This is followed by the formation process of the giant planets either by core accretion or gravitational instability. Finally, the dynamical evolution of the orbital elements as driven by disk-planet interaction and the overall evolution of multi-object systems is presented.

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Type I planetary migration in a self-gravitating disk

Cited by 5 publications

References 19 publications

A low mass for Mars from Jupiter’s early gas-driven migration

A low mass for Mars from Jupiter’s early gas-driven migration

Spiral structures in an embedded protostellar disk driven by envelope accretion

Planet Formation and Disk-Planet Interactions

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