Reassessing the formation of the inner Oort cloud in an embedded star cluster

• Published in: Icarus (New York, N.Y. 1962) Vol. 217; no. 1; pp. 1 - 19
• Main Authors: Brasser, R., Duncan, M.J., Levison, H.F., Schwamb, M.E., Brown, M.E.
• Format: Journal Article
• Language: English
• Published: Amsterdam Elsevier Inc 2012; Elsevier
• Subjects: Astronomy; Clouds; Clusters; Comets; Comets, Dynamics; Earth, ocean, space; Exact sciences and technology; Mathematical models; Oort cloud; Origin, Solar System; Outer solar system; Planetary dynamics; Sedna (planet); Solar system; Stars; Origin, Solar System; Comets, Dynamics; Planetary dynamics; Comets; Collapse; Origin; Hyperbolic system; Digital simulation; Solar System Comets; N body system; Orbits; Star clusters; Jupiter planet; Sun; Saturn planet; Relaxation; Initial conditions; Dynamics; Disturbances; Oort cloud; Models; Solar system
• ISSN: 0019-1035; 1090-2643
• DOI: 10.1016/j.icarus.2011.10.012

► We study the formation of the inner Oort cloud in a star cluster. ► The generation of Sedna is a generic outcome. ► The location of Sedna coincides with the inner edge of the cloud. ► We cannot constrain the size of the Sun’s birth cluster. We re-examine the formation of the inner Oort comet cloud while the Sun was in its birth cluster with the aid of numerical simulations. This work is a continuation of an earlier study (Brasser, R., Duncan, M.J., Levison, H.F. [2006]. Icarus 184, 59–82) with several substantial modifications. First, the system consisting of stars, planets and comets is treated self-consistently in our N-body simulations, rather than approximating the stellar encounters with the outer Solar System as hyperbolic fly-bys. Second, we have included the expulsion of the cluster gas, a feature that was absent previously. Third, we have used several models for the initial conditions and density profile of the cluster – either a Hernquist or Plummer potential – and chose other parameters based on the latest observations of embedded clusters from the literature. These other parameters result in the stars being on radial orbits and the cluster collapses. Similar to previous studies, in our simulations the inner Oort cloud is formed from comets being scattered by Jupiter and Saturn and having their pericentres decoupled from the planets by perturbations from the cluster gas and other stars. We find that all inner Oort clouds formed in these clusters have an inner edge ranging from 100 AU to a few hundred AU, and an outer edge at over 100,000 AU, with little variation in these values for all clusters. All inner Oort clouds formed are consistent with the existence of (90377) Sedna, an inner Oort cloud dwarf planetoid, at the inner edge of the cloud: Sedna tends to be at the innermost 2% for Plummer models, while it is 5% for Hernquist models. We emphasise that the existence of Sedna is a generic outcome. We define a ‘concentration radius’ for the inner Oort cloud and find that its value increases with increasing number of stars in the cluster, ranging from 600 AU to 1500 AU for Hernquist clusters and from 1500 AU to 4000 AU for Plummer clusters. The increasing trend implies that small star clusters form more compact inner Oort clouds than large clusters. We are unable to constrain the number of stars that resided in the cluster since most clusters yield inner Oort clouds that could be compatible with the current structure of the outer Solar System. The typical formation efficiency of the inner Oort cloud is 1.5%, significantly lower than previous estimates. We attribute this to the more violent dynamics that the Sun experiences as it rushes through the centre of the cluster during the latter’s initial phase of violent relaxation.