Regarding the Accretion of 2003 VB12 (Sedna) and Like Bodies in Distant Heliocentric Orbits

@article{Stern2004RegardingTA,
  title={Regarding the Accretion of 2003 VB12 (Sedna) and Like Bodies in Distant Heliocentric Orbits},
  author={S. Stern},
  journal={The Astronomical Journal},
  year={2004},
  volume={129},
  pages={526-529}
}
  • S. Stern
  • Published 2004
  • Physics
  • The Astronomical Journal
Recently, Brown et al. reported the exciting discovery of an ~800 km radius object, (90377) Sedna, on a distant, eccentric orbit centered at ~490 AU from the Sun. Here we undertake a first look exploring the feasibility of accreting this object and its possible cohorts between 75 AU (Sedna's perihelion distance) and 500 AU (Sedna's semimajor-axis distance) from the Sun. We find such accretion possible in a small fraction of the age of the solar system, if such objects were initially on nearly… Expand

Tables from this paper

Ninth Planet or Wandering Star
We study the gravitational effects of two celestrial bodies on a typical object of the Kuyper Belt. The first body is a kuyperian object itself with fairly large eccentricity and perihelion but withExpand
Upper Limits on the Number of Small Bodies in Sedna-Like Orbits by the TAOS Project
We present the results of a search for occultation events by objects at distances between 100 and 1000 AU in light curves from the Taiwanese-American Occultation Survey. We searched for consecutive,Expand
AN OUTER PLANET BEYOND PLUTO AND THE ORIGIN OF THE TRANS-NEPTUNIAN BELT ARCHITECTURE
Trans-Neptunian objects (TNOs) are remnants of a collisionally and dynamically evolved planetesimal disk in the outer solar system. This complex structure, known as the trans-Neptunian belt (orExpand
The Search for Distant Objects in the Solar System Using Spacewatch
We have completed a low-inclination ecliptic survey for distant and slow-moving bright objects in the outer solar system. This survey used data taken over 34 months by the University of Arizona'sExpand
Kuiperian Objects and Wandering Cosmic Objects
We study the effects of an encounter between a wandering cosmic object (WCO) of 0.1 solar mass and some Kuiperian Objects (KO). First, we let the WCO cross the out-skirt of ou Kuiper belt. SuchExpand
The Search for Planet X: Testing Inferences from the Kuiper Cliff
Abstract : The goal of this project was to search a large archive of astronomical CCD imagery to test the validity of arguments regarding the existence of a hypothetical "Planet X." As proposed byExpand
Detectability of Occultations of Stars by Objects in the Kuiper Belt and Oort Cloud
The serendipitous detection of stellar occultations by outer solar system objects is a powerful method for ascertaining the small end (r 15 km) of the size distribution of Kuiper Belt objects and mayExpand
The Fate of Scattered Planets
As gas giant planets evolve, they may scatter other planets far from their original orbits to produce hot Jupiters or rogue planets that are not gravitationally bound to any star. Here, we considerExpand
Formation of Super-Earth Mass Planets at 125-250 AU from a Solar-type Star
We investigate pathways for the formation of icy super-Earth mass planets orbiting at 125-250 AU around a 1 solar mass star. An extensive suite of coagulation calculations demonstrates that swarms ofExpand
On the Rotation Period of (90377) Sedna
We present precise, ~1%, r-band relative photometry of the unusual solar system object (90377) Sedna. Our data consist of 143 data points taken over eight nights in 2004 October and 2005 JanuaryExpand
...
1
2
...

References

SHOWING 1-10 OF 17 REFERENCES
Scenarios for the Origin of the Orbits of the Trans-Neptunian Objects 2000 CR105 and 2003 VB12 (Sedna)
Explaining the origin of the orbits of 2000 CR105 (a = 230 AU, q = 44 AU) and 2003 VB12 (a = 531 AU, q = 74 AU, unofficially known as Sedna) is a major test for our understanding of the primordialExpand
Evidence for an Extended Scattered Disk
Abstract By telescopic tracking, we have established that the transneptunian object (TNO) 2000 CR 105 has a semimajor axis of 220±1 AU and perihelion distance of 44.14±0.02 AU, beyond the domainExpand
Collisional Erosion in the Primordial Edgeworth-Kuiper Belt and the Generation of the 30-50 AU Kuiper Gap
One of the oustanding questions about the architecture of the outer solar system is how the trans-Neptunian disk of comets and small planet-scale objects known as the solar system's Edgeworth-KuiperExpand
Timescales for planetary accretion and the structure of the protoplanetary disk
Abstract This paper outlines a unified scenario for Solar System formation consistent with astrophysical constraints. Jupiter's core could have grown by runaway accretion of planetesimals to a massExpand
On the Collisional Environment, Accretion Time Scales, and Architecture of the Massive, Primordial Kuiper Belt.
ii Abstract Previous collisional modelling has suggested that the mass of the primordial Kuiper Disk between 30 and 50 AU was probably of order 10M to 50M. We explore the consequences of a massive,Expand
Accretion in the Edgeworth-Kuiper Belt: Forming 100-1000 KM Radius Bodies at 30 AU and Beyond.
We employ a time-dependent collisional evolution code to study the conditions under which the 50{200 km radius Edgeworth-Kuiper Objects (EKOs) in the region between 30 and 50 AU (now called theExpand
Collisions, accretion, and erosion in the Kuiper Belt
Abstract Collisional modeling has been a fertile area of Kuiper Belt research for almost a decade. Such modeling has yielded important results concerning expected KBO surface properties, the KBO sizeExpand
Planet Formation in the Outer Solar System
This paper reviews coagulation models for planet formation in the Kuiper belt, emphasizing links to recent observations of our and other solar systems. At heliocentric distances of 35-50 AU,Expand
Formation of planetary embryos: effects of fragmentation, low relative velocity, and independent variation of eccentricity and inclination.
TLDR
An earlier investigation of the formation of approximately 10(26) g planetary embryos from much smaller planetesimals has been extended to include the effects of collisional fragmentation, the low relative velocity regime in which the effects due to solar gravity are important, and independent perturbations of eccentricity and inclination. Expand
Forming the Dusty Ring in HR 4796A
We describe planetesimal accretion calculations for the dusty ring observed in the nearby A0 star HR 4796A. Models with initial masses of 10-20 times the minimum-mass solar nebula produce a ring withExpand
...
1
2
...