Jupiter formed as a pebble pile around the N2 ice line

@article{Bosman2019JupiterFA,
  title={Jupiter formed as a pebble pile around the N2 ice line},
  author={Arthur D. Bosman and Alex J. Cridland and Yamila Miguel},
  journal={arXiv: Earth and Planetary Astrophysics},
  year={2019}
}
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. We aim to use the Nitrogen abundance in Jupiter, which is around 4 times solar, in combination with \textit{Juno} constraints on the total mass of heavy… Expand

Figures and Tables from this paper

The composition of hot Jupiter atmospheres assembled within chemically evolved protoplanetary discs
The radial-dependent positions of snowlines of abundant oxygen- and carbon-bearing molecules in protoplanetary discs will result in systematic radial variations in the C/O ratios in the gas and ice.Expand
Four annular structures in a protostellar disk less than 500,000 years old.
TLDR
Whether or not planets already exist in the disk of IRS 63 is clear that the planet- formation process begins in the initial protostellar phases, earlier than predicted by current planet-formation theories. Expand
Inner Workings: Was Jupiter born beyond the current orbits of Neptune and Pluto?
  • K. Croswell
  • History, Medicine
  • Proceedings of the National Academy of Sciences
  • 2020
Ancient people named the planet Jupiter well. Both its brilliance and its slow, regal movement across the sky evoked a king among gods. Today we know much more about the influence of Jupiter, aExpand
Exploring the link between star and planet formation with Ariel
The goal of the Ariel space mission is to observe a large and diversified population of transiting planets around a range of host star types to collect information on their atmospheric composition.Expand
The homogeneous characterisation of Ariel host stars
TLDR
A structured approach for the characterisation of Ariel stars that accounts for the concepts of homogeneity and coherence among a large set of stellar parameters and preliminary results for elemental abundances of Na, Al, Mg, Si, C, N. Expand
Connecting planet formation and astrochemistry
(Abridged) The chemical composition of planetary atmospheres has long been thought to store information regarding where and when a planet accretes its material. Predicting this chemical compositionExpand
Tracing the Formation History of Giant Planets in Protoplanetary Disks with Carbon, Oxygen, Nitrogen, and Sulfur
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 CExpand
A New Window into Planet Formation and Migration: Refractory-to-Volatile Elemental Ratios in Ultra-hot Jupiters
A primary goal of exoplanet characterization is to use a planet’s current composition to understand how that planet formed. For example, the C/O ratio has long been recognized as carrying importantExpand
Astrochemistry and compositions of planetary systems
Abstract Planets form and obtain their compositions in disks of gas and dust around young stars. The chemical compositions of these planet-forming disks regulate all aspects of planetary compositionsExpand
Beyond Equilibrium Temperature: How the Atmosphere/Interior Connection Affects the Onset of Methane, Ammonia, and Clouds in Warm Transiting Giant Planets
The atmospheric pressure-temperature profiles for transiting giant planets cross a range of chemical transitions. Here we show that the particular shape of these irradiated profiles for warm giantExpand
...
1
2
...

References

SHOWING 1-10 OF 66 REFERENCES
Jupiter's Composition Suggests its Core Assembled Exterior to the N2 Snowline
Jupiter's atmosphere is enriched in C, N, S, P, Ar, Kr and Xe with respect to solar abundances by a factor of ~3. Gas Giant envelopes are mainly enriched through the dissolution of solids in theExpand
A low-temperature origin for the planetesimals that formed Jupiter
TLDR
It is shown that argon, krypton and xenon in Jupiter's atmosphere are enriched to the same extent as the other heavy elements, which suggests that the planetesimals carrying these elements must have formed at temperatures lower than predicted by present models of giant-planet formation. Expand
A low mass for Mars from Jupiter’s early gas-driven migration
TLDR
Simulation of the early Solar System shows 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. Expand
Formation of planetary systems by pebble accretion and migration : Growth of gas giants
Giant planets migrate though the protoplanetary disc as they grow their solid core and attract their gaseous envelope. Previously, we have studied the growth and migration of an isolated planet in anExpand
Efficiency of radial transport of ices in protoplanetary disks probed with infrared observations : the case of CO2
The efficiency of radial transport of icy solid material from outer disk to the inner disk is currently unconstrained. Efficient radial transport of icy dust grains could significantly alter theExpand
The Origin and Evolution of Saturn, with Exoplanet Perspective
Saturn formed beyond the snow line in the primordial solar nebula that made it possible for it to accrete a large mass. Disk instability and core accretion models have been proposed for Saturn'sExpand
Transport of CO in Protoplanetary Disks: Consequences of Pebble Formation, Settling, and Radial Drift
Current models of (exo)planet formation often rely on a large influx of so-called `pebbles' from the outer disk into the planet formation region. In this paper, we investigate how the formation ofExpand
Redistribution of CO at the location of the CO ice line in evolving gas and dust disks
Context. Ice lines are suggested to play a significant role in grain growth and planetesimal formation in protoplanetary disks. Evaporation fronts directly influence the gas and ice abundances ofExpand
Reduced gas accretion on super-Earths and ice giants
A large fraction of giant planets have gaseous envelopes that are limited to about 10 % of their total mass budget. Such planets are present in the Solar System (Uranus, Neptune) and are frequentlyExpand
Constraining Gas-Phase Carbon, Oxygen, and Nitrogen in the IM Lup Protoplanetary Disk
We present new constraints on gas-phase C, N, and O abundances in the molecular layer of the IM Lup protoplanetary disk. Building on previous physical and chemical modeling of this disk, we use newExpand
...
1
2
3
4
5
...