Implications of the interstellar object 1I/'Oumuamua for planetary dynamics and planetesimal formation

@article{Raymond2018ImplicationsOT,
  title={Implications of the interstellar object 1I/'Oumuamua for planetary dynamics and planetesimal formation},
  author={Sean N. Raymond and Philip J. Armitage and Dimitri Veras and Elisa V. Quintana and Thomas Barclay},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2018},
  volume={476},
  pages={3031-3038}
}
'Oumuamua, the first bona-fide interstellar planetesimal, was discovered passing through our Solar System on a hyperbolic orbit. This object was likely dynamically ejected from an extrasolar planetary system after a series of close encounters with gas giant planets. To account for 'Oumuamua's detection, simple arguments suggest that ~1 Earth-mass of planetesimals are ejected per Solar mass of Galactic stars. However, that value assumes mono-sized planetesimals. If the planetesimal mass… 

Figures from this paper

A Hypothesis for the Rapid Formation of Planets

The discovery of 1I/‘Oumuamua confirmed that planetesimals must exist in great numbers in interstellar space. Originally generated during planet formation, they are scattered from their original

Origin of 1I/’Oumuamua. I. An Ejected Protoplanetary Disk Object?

1I/’Oumuamua is the first interstellar interloper to have been detected. Because planetesimal formation and ejection of predominantly icy objects are common by-products of the star and planet

Survivor Bias: Divergent Fates of the Solar System’s Ejected versus Persisting Planetesimals

The orbital architecture of the solar system is thought to have been sculpted by a dynamical instability among the giant planets. During the instability a primordial outer disk of planetesimals was

Hidden Planets: Implications from ’Oumuamua and DSHARP

The discovery of ’Oumuamua (1I/2017 U1), the first interstellar interloper, suggests an abundance of free-floating small bodies whose ejection into galactic space cannot be explained by the current

1I/‘Oumuamua as a Tidal Disruption Fragment from a Binary Star System

1I/‘Oumuamua is the first known interstellar small body, probably being only about 100 m in size. Against expectations based on comets, ‘Oumuamua does not show any activity and has a very elongated

Formation of Terrestrial Planets

The past decade has seen major progress in our understanding of terrestrial planet formation. Yet key questions remain. In this review we first address the growth of 100 km-scale planetesimals as a

Planet seeding through gas-assisted capture of interstellar objects

Planet formation begins with collisional growth of small planetesimals accumulating into larger ones. Such growth occurs while planetesimals are embedded in a gaseous protoplanetary disc. However,

A kinematical age for the interstellar object 1I/’Oumuamua

1I/'Oumuamua is the first interstellar object observed passing through the Solar System. Understanding the nature of these objects will provide crucial information about the formation and evolution

What and whence 1I/`Oumuamua: a contact binary from the debris of a young planetary system?

The first confirmed interstellar interloper in our Solar System, 1I/`Oumuamua, is likely to be a minor body ejected from another star, but its brief flyby and faintness made it difficult to study.

High-drag Interstellar Objects and Galactic Dynamical Streams

  • T. Eubanks
  • Physics, Geology
    The Astrophysical Journal
  • 2019
The nature of 1I/’Oumuamua (henceforth, 1I), the first interstellar object (ISO) known to pass through the solar system, remains mysterious. Feng & Jones noted that the incoming 1I velocity vector
...

References

SHOWING 1-10 OF 112 REFERENCES

PLANET–PLANET SCATTERING IN PLANETESIMAL DISKS. II. PREDICTIONS FOR OUTER EXTRASOLAR PLANETARY SYSTEMS

We develop an idealized dynamical model to predict the typical properties of outer extrasolar planetary systems, at radii comparable to the Jupiter-to-Neptune region of the solar system. The model is

The Demographics of Rocky Free-floating Planets and their Detectability by WFIRST

Planets are thought to form via accretion from a remnant disk of gas and solids around a newly formed star. During this process, material in the disk either remains bound to the star as part of

PLANET–PLANET SCATTERING IN PLANETESIMAL DISKS

We study the final architecture of planetary systems that evolve under the combined effects of planet–planet and planetesimal scattering. Using N-body simulations we investigate the dynamics of

Debris disks as signposts of terrestrial planet formation - II. Dependence of exoplanet architectures on giant planet and disk properties

We present models for the formation of terrestrial planets, and the collisional evolution of debris disks, in planetary systems that contain multiple marginally unstable gas giants. We previousl y

Mini-Oort clouds: compact isotropic planetesimal clouds from planet–planet scattering

Starting from planetary systems with three giant planets and an outer disk of planetesimals, we use dynamical simulations to show how dynamical instabilities can transform planetesimal disks into

Modelling circumbinary protoplanetary disks - II. Gas disk feedback on planetesimal dynamical and collisional evolution in the circumbinary systems Kepler-16 and 34

Aims. We investigate the feasibility of planetesimal growth in circumbinary protoplanetary disks around the observed systems Kepler-16 and Kepler-34 under the gravitational influence of a precessing

A brief visit from a red and extremely elongated interstellar asteroid

TLDR
Observations and analysis of the object 1I/2017 U1 (‘Oumuamua) that demonstrate its extrasolar trajectory, and that enable comparisons to be made between material from another planetary system and from the authors' own, reveal it to be asteroidal with no hint of cometary activity despite an approach within 0.25 astronomical units of the Sun.

Planet Scattering Around Binaries: Ejections, Not Collisions

Transiting circumbinary planets discovered by Kepler provide unique insight into binary star and planet formation. Several features of this new found population, for example the apparent pile-up of

Dynamical Origin of Extrasolar Planet Eccentricity Distribution

We explore the possibility that the observed eccentricity distribution of extrasolar planets arose through planet-planet interactions, after the initial stage of planet formation was complete. Our
...