Planet-forming material in a protoplanetary disc: the interplay between chemical evolution and pebble drift

Booth, Richard A; Ilee, John D.

doi:10.1093/mnras/stz1488

Cited by 100 publications

(90 citation statements)

References 97 publications

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“…Such detailed comparison motivates the need for the development of more sophisticated models in two different areas. Firstly, detailed chemical evolution models for the evolution and transport of refractory and volatile elements in an evolving protoplanetary disc along the lines of those by Booth et al (2017); Booth & Ilee (2019) rather than just treating "gas" and "dust" as we have done in this work. Secondly, there is almost no understanding of the role of planet-disc interactions in controlling how different species may enter the gas and flow across the planetary gap, or be accreted by the planet's themselves.…”

Section: Discussionmentioning

confidence: 99%

Fingerprints of giant planets in the composition of solar twins

Booth

Owen

2020

Monthly Notices of the Royal Astronomical Society

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The Sun shows a ∼ 10 % depletion in refractory elements relative to nearby solar twins. It has been suggested that this depletion is a signpost of planet formation. The exoplanet statistics are now good enough to show that the origin of this depletion does not arise from the sequestration of refractory material inside the planets themselves. This conclusion arises because most sun-like stars host close-in planetary systems that are on average more massive than the Sun's. Using evolutionary models for the protoplanetary discs that surrounded the young Sun and solar twins we demonstrate that the origin of the depletion likely arises due to the trapping of dust exterior to the orbit of a forming giant planet. In this scenario a forming giant planet opens a gap in the gas disc, creating a pressure trap. If the planet forms early enough, while the disc is still massive, the planet can trap 100 M ⊕ of dust exterior to its orbit, preventing the dust from accreting onto the star in contrast to the gas. Forming giant planets can create refractory depletions of ∼ 5 − 15%, with the larger values occurring for initial conditions that favour giant planet formation (e.g. more massive discs, that live longer). The incidence of solar-twins that show refractory depletion matches both the occurrence of giant planets discovered in exoplanet surveys and "transition" discs that show similar depletion patterns in the material that is accreting onto the star.

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Section: Discussionmentioning

confidence: 99%

Fingerprints of giant planets in the composition of solar twins

Booth

Owen

2020

Monthly Notices of the Royal Astronomical Society

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“…In the case of nitrogen, Booth & Ilee (2019) find an enrichment of elemental nitrogen up to a factor of 2 above solar both within the NH 3 ice line and in an annulus just within the N 2 ice line. The high elemental nitrogen abundances within the NH 3 ice line are strongly dependent on the initial NH 3 abundance.…”

Section: Enriching Jupiter With Nitrogenmentioning

confidence: 93%

“…Recently there have been multiple studies that have looked at the effect of disk evolution, especially the growth and drift of icy grains, at the effect this has on the gas-phase elemental abundances (Ciesla & Cuzzi 2006;Booth et al 2017;Stammler et al 2017;Bosman et al 2018;Krijt et al 2018;Booth & Ilee 2019). In general, it is found that enrichments above solar abundances in a certain element can happen just inside an ice line if radial drift is efficient and the ice line corresponds to a species that is an abundant ( 10%) carrier of that element.…”

Section: Enriching Jupiter With Nitrogenmentioning

confidence: 99%

Jupiter formed as a pebble pile around the N₂ ice line

Bosman

Cridland

Miguel

2019

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Context. The region around the H 2 O ice line, due to its higher surface density, seems to be the ideal location to form planets. The core of Jupiter, as well as the cores of close in gas giants are thus thought to form in this region of the disk. Actually constraining the formation location of individual planets has proven to be difficult, however. Aims. We aim to use the Nitrogen abundance in Jupiter, which is around 4 times solar, in combination with Juno constraints on the total mass of heavy elements in Jupiter, to narrow down its formation scenario. Methods. Different pathways of enrichment of Jupiter's atmosphere, such as the accretion of enriched gas, pebbles or planetesimals are considered and their implications for the oxygen abundance of Jupiter is discussed. Results. The super solar Nitrogen abundance in Jupiter necessitates the accretion of extra N 2 from the proto-solar nebula. The only location of the disk that this can happen is outside, or just inside the N 2 ice line. These constraints favor a pebble accretion origin of Jupiter, both from the composition as well as from a planet formation perspective. We predict that Jupiter's oxygen abundance is between 3.6 and 4.5 times solar.

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“…Since the early work of Öberg et al (2011), several studies have been devoted to understanding the link between the abundances of the two most abundant high-Z elements, carbon (C) and oxygen (O), and the planetary formation process; for more recent discussions, see, e.g., Madhusudhan et al (2016), Mordasini et al (2016), Booth & Ilee (2019), Cridland et al (2019), and references therein. Recently, a few studies have taken a first look at nitrogen (N), as well (Bosman et al 2019;Öberg & Wordsworth 2019).…”

Section: Introductionmentioning

confidence: 99%

Tracing the Formation History of Giant Planets in Protoplanetary Disks with Carbon, Oxygen, Nitrogen, and Sulfur

Turrini

Schisano

Fonte

et al. 2021

ApJ

110

229

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The composition of giant planets is imprinted by their migration history and the compositional structure of their hosting disks. Studies in recent literature have investigated how the abundances of C and O can constrain the formation pathways of giant planets forming within few tens of au from a star. New ALMA observations, however, suggest planet-forming regions possibly extending to hundreds of au. We explore the implications of these wider formation environments through n-body simulations of growing and migrating giant planets embedded in planetesimal disks, coupled with a compositional model of the protoplanetary disk where volatiles are inherited from the molecular cloud and refractories are calibrated against extrasolar and Solar System data. We find that the C/O ratio provides limited insight on the formation pathways of giant planets that undergo large-scale migration. This limitation can be overcome, however, thanks to nitrogen and sulfur. Jointly using the C/N, N/O, and C/O ratios breaks any degeneracy in the formation and migration tracks of giant planets. The use of elemental ratios normalized to the respective stellar ratios supplies additional information on the nature of giant planets, thanks to the relative volatility of O, C, and N in disks. When the planetary metallicity is dominated by the accretion of solids C/N * > C/O * > N/O * ( * denoting this normalized scale), otherwise N/O * > C/O * > C/N * . The S/N ratio provides an additional independent probe into the metallicity of giant planets and their accretion of solids.

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Planet-forming material in a protoplanetary disc: the interplay between chemical evolution and pebble drift

Cited by 100 publications

References 97 publications

Fingerprints of giant planets in the composition of solar twins

Fingerprints of giant planets in the composition of solar twins

Jupiter formed as a pebble pile around the N₂ ice line

Tracing the Formation History of Giant Planets in Protoplanetary Disks with Carbon, Oxygen, Nitrogen, and Sulfur

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Planet-forming material in a protoplanetary disc: the interplay between chemical evolution and pebble drift

Cited by 100 publications

References 97 publications

Fingerprints of giant planets in the composition of solar twins

Fingerprints of giant planets in the composition of solar twins

Jupiter formed as a pebble pile around the N2 ice line

Tracing the Formation History of Giant Planets in Protoplanetary Disks with Carbon, Oxygen, Nitrogen, and Sulfur

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Jupiter formed as a pebble pile around the N₂ ice line