Collisional Growth within the Solar System’s Primordial Planetesimal Disk and the Timing of the Giant Planet Instability

Morgan, Marvin; Seligman, Darryl Z.; Batygin, Konstantin

doi:10.3847/2041-8213/ac1681

Cited by 8 publications

(6 citation statements)

References 45 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Moreover, the age of these interstellar comets could provide us with an estimate for the relative timing of the dynamical instabilities in exoplanetary systems. Based on theoretical modeling of the early timing of the instability in the solar system (Grav et al 2011;Buie et al 2015;Nesvorný et al 2018;Clement et al 2018Clement et al , 2019de Sousa et al 2020;Nesvorný et al 2021;Morgan et al 2021) and the recent discovery of an excess of free-floating planets in the Upper Scorpius <10 Myr stellar association (Miret-Roig et al 2022), it seems feasible that the majority of interstellar comets are ejected within the first <10 Myr of a planetary system's lifetime. If the majority of the population of interstellar comets formed interior to the CO snow line, this would imply that early giant planet migration is common in this region.…”

Section: Discussionmentioning

confidence: 99%

The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets

et al. 2022

Self Cite

View full text Add to dashboard Cite

Based on the occurrence rates implied by the discoveries of 1I/‘Oumuamua and 2I/Borisov, the forthcoming Rubin Observatory Legacy Survey of Space and Time (LSST) should detect ≥one interstellar object every year. We advocate for future measurements of the production rates of H2O, CO2, and CO in these objects to estimate their carbon-to-oxygen ratios, which trace formation locations within their original protoplanetary disks. We review similar measurements for solar system comets, which indicate formation interior to the CO snow line. By quantifying the relative processing in the interstellar medium and solar system, we estimate that production rates will not be representative of primordial compositions for the majority of interstellar comets. Preferential desorption of CO and CO2 relative to H2O in the interstellar medium implies that measured C/O ratios represent lower limits on the primordial ratios. Specifically, production rate ratios of Q(CO)/Q(H2O) < 0.2 and Q(CO)/Q(H2O) > 1 likely indicate formation interior and exterior to the CO snow line, respectively. The high C/O ratio of 2I/Borisov implies that it formed exterior to the CO snow line. We provide an overview of the currently operational facilities capable of obtaining these measurements that will constrain the fraction of ejected comets that formed exterior to the CO snow line. This fraction will provide key insights into the efficiency of and mechanisms for cometary ejection in exoplanetary systems.

show abstract

Section: Discussionmentioning

confidence: 99%

The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets

et al. 2022

Self Cite

View full text Add to dashboard Cite

show abstract

“…In fact, these works are associated with studying a last non-catastrophic stage in the Nice model. In this model, various schemes were discussed, including studies of both the planetary instability stage and the pre-instability stage (e.g., Tsiganis et al 2005;Morbidelli et al 2007;Batygin & Brown 2010;Levison et al 2011;Nesvorný & Morbidelli 2012;Reyes-Ruiz et al 2015;Quarles & Kaib 2019;Ribeiro de Sousa et al 2020;Morgan et al 2021). Fan & Batygin (2017) studied one case from Batygin et al (2011) that included a stage of the planetary instability and they compared simulations with a self-gravitating planetesimal disk and with a non-self-gravitating disk.…”

Section: Discussionmentioning

confidence: 99%

“…On the other hand, Fernández & Ip (1996) noted that objects of masses 1-5 M E are always produced along with Uranus and Neptune in their simulations. Recent numerical experiments of Morgan et al (2021) indicated that it is plausible for ∼1 M E objects to emerge within the primordial trans-Neptunian region on a ∼10 Myr timescale. tested the dependence of the "inclination instability" effect on the number N of massive objects in simulations.…”

Section: Discussionmentioning

confidence: 99%

Dynamical evolution of a self-gravitating planetesimal disk in the distant trans-Neptunian region

Emelyanenko

2022

A&A

View full text Add to dashboard Cite

Aims. We study the dynamical evolution of a system consisting of the giant planets and a massive planetesimal disk over the age of the Solar System. The main question addressed in this study is whether distant trans-Neptunian objects could have come about as a result of the combined action of planetary perturbations and the self-gravity of the disk. Methods. We carried out a series of full N-body numerical simulations of gravitational interactions between the giant planets and a massive outer disk of planetesimals. Results. Our simulations show that the collective gravity of the giant planets and massive planetesimals produces distant trans-Neptunian objects across a wide range of the initial disk mass. The majority of objects that survive up through the age of the Solar System have perihelion distances of q > 40 au. In this region, there is a tendency toward a slow decrease in eccentricities and an increase in perihelion distances for objects with semimajor axes a > 150 au. Secular resonances between distant planetesimals play a major role in increasing their perihelion distances. This explains the origin of Sedna-type objects. In our integrations for the age of the Solar System, we registered times with both high and low clustering of longitudes of perihelion and arguments of perihelion for objects with q > 40 au, a > 150 au. The resulting distribution of inclinations in our model and the observed distribution of inclinations for distant trans-Neptunian objects have similar average values of around 20°. Conclusions. Distant trans-Neptunian objects are a natural consequence in the models that include migrating giant planets and a self-gravitating planetesimal disk.

show abstract

“…Numerous refinements were then brought to the instability model in order to properly reproduce the structure of the Solar System as we observe it today. The most recent advances favour a very early migration and instability (within 10 Myrs, or even immediately after dispersal of the gas disc), and no relation with the Late heavy bombardment (see Clement et al 2018Clement et al , 2021Nesvorný et al 2018;Morgan et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Tilting Uranus via the migration of an ancient satellite

Saillenfest

Rogoszinski

Lari

et al. 2022

A&A

View full text Add to dashboard Cite

Context. The 98 • -obliquity of Uranus is commonly attributed to giant impacts that occurred at the end of the planetary formation. This picture, however, is not devoid of weaknesses. Aims. On a billion-year timescale, the tidal migration of the satellites of Jupiter and Saturn has been shown to strongly affect their spin-axis dynamics. We aim to revisit the scenario of tilting Uranus in light of this mechanism. Methods. We analyse the precession spectrum of Uranus and identify the candidate secular spin-orbit resonances that could be responsible for the tilting. We determine the properties of the hypothetical ancient satellite required for a capture and explore the dynamics numerically.Results. If it migrates over 10 Uranus' radii, a single satellite with minimum mass 4 × 10 −4 Uranus' mass is able to tilt Uranus from a small obliquity and make it converge towards 90 • . In order to achieve the tilting in less than the age of the Solar System, the mean drift rate of the satellite must be comparable to the Moon's current orbital expansion. Under these conditions, simulations show that Uranus is readily tilted over 80 • . Beyond this point, the satellite is strongly destabilised and triggers a phase of chaotic motion for the planet's spin axis. The chaotic phase ends when the satellite collides into the planet, ultimately freezing the planet's obliquity in either a prograde, or plainly retrograde state (as Uranus today). Spin states resembling that of Uranus can be obtained with probabilities as large as 80%, but a bigger satellite is favoured, with mass 1.7 × 10 −3 Uranus' mass or more. Yet, a smaller ancient satellite is not categorically ruled out, and there is room for improving this basic scenario in future studies. Interactions among several pre-existing satellites is a promising possibility. Conclusions. The conditions required for the tilting seem broadly realistic, but it remains to be determined whether Uranus could have hosted a big primordial satellite subject to substantial tidal migration. The efficiency of tidal energy dissipation within Uranus is required to be much higher than traditionally assumed, more in line with that measured for the migration of Titan. Hints about these issues would be given by a measure of the expansion rate of Uranus' main satellites.

show abstract

Collisional Growth within the Solar System’s Primordial Planetesimal Disk and the Timing of the Giant Planet Instability

Cited by 8 publications

References 45 publications

The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets

The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets

Dynamical evolution of a self-gravitating planetesimal disk in the distant trans-Neptunian region

Tilting Uranus via the migration of an ancient satellite

Contact Info

Product

Resources

About