How Sedna and family were captured in a close encounter with a solar sibling

Jílková, Lucie; Zwart, Simon Portegies; Pijloo, Tjibaria; Hammer, Michael F.

doi:10.1093/mnras/stv1803

Cited by 80 publications

(74 citation statements)

References 44 publications

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“…All TNOs with clones exhibiting diffusive behavior are marked in Figure 5 (red labels). We note that some clones are capable of diffusion, while other clones are stable on Gyr timescales; the process will be more effective for larger-a TNOs, and the phase spaces of some TNOs (e.g., 2014 SR 349 ) show less mobility given their current a, q. Sedna and 2012 VP 113 are not formed by diffusion in the current dynamical environment, which is consistent with previous assessments (Brown et al 2004;Gallardo et al 2012;Jílková et al 2015). However, it is plausible, for the orbit-fit uncertainty parameter space currently occupied by the orbits of other extreme TNOs, that they could be produced by the same inward diffusion from the inner fringe of the Oort cloud that can populate 2013 SY 99 's parameter region.…”

Section: Diffusion As a Way To Populate The Orbital Phase Space Of Exsupporting

confidence: 89%

OSSOS. V. Diffusion in the Orbit of a High-perihelion Distant Solar System Object

Bannister¹,

Shankman²,

Volk³

et al. 2017

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We report the discovery of the minor planet 2013 SY 99 on an exceptionally distant, highly eccentric orbit. With a perihelion of 50.0au, 2013 SY 99 's orbit has a semimajor axis of 730±40au, the largest known for a highperihelion trans-Neptunian object (TNO), and well beyond those of (90377) Sedna and 2012 VP 113 . Yet, with an aphelion of 1420±90au, 2013 SY 99 's orbit is interior to the region influenced by Galactic tides. Such TNOs are not thought to be produced in the current known planetary architecture of the solar system, and they have informed the recent debate on the existence of a distant giant planet. Photometry from the Canada-France-Hawaii Telescope, Gemini North, and Subaru indicate 2013 SY 99 is ∼250km in diameter and moderately red in color, similar to other dynamically excited TNOs. Our dynamical simulations show that Neptune's weak influence during 2013 SY 99 's perihelia encounters drives diffusion in its semimajor axis of hundreds of astronomical units over 4Gyr. The overall symmetry of random walks in the semimajor axis allows diffusion to populate 2013 SY 99 's orbital parameter space from the 1000 to 2000au inner fringe of the Oort cloud. Diffusion affects other known TNOs on orbits with perihelia of 45 to 49au and semimajor axes beyond 250au. This provides a formation mechanism that implies an extended population, gently cycling into and returning from the inner fringe of the Oort cloud.

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Section: Diffusion As a Way To Populate The Orbital Phase Space Of Exsupporting

confidence: 89%

OSSOS. V. Diffusion in the Orbit of a High-perihelion Distant Solar System Object

Bannister¹,

Shankman²,

Volk³

et al. 2017

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“…Several viable theories have been put forth to explain the orbits of IOC objects (Kenyon and Bromley 2004;Morbidelli and Levison 2004;Brown et al 2004;Melita et al 2005;Levison et al 2010;Kaib et al 2011;Jilkova et al 2015;Portegies Zwart and Jilkova 2015). The most popular scenario, until recently, is that the IOC objects were put into place while the Sun was still within its birth cluster (Brasser et al 2012).…”

Section: Introductionmentioning

confidence: 99%

New Extreme Trans-Neptunian Objects: Toward a Super-Earth in the Outer Solar System

Sheppard

Trujillo

2016

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We are conducting a wide and deep survey for extreme distant solar system objects. Our goal is to understand the high perihelion objects Sedna and 2012 VP113 and determine if an unknown massive planet exists in the outer solar system. The discovery of new extreme objects from our survey of some 1080 square degrees of sky to over 24th magnitude in the r-band are reported. Two of the new objects, 2014 SR349 and 2013 FT28, are extreme detached trans-Neptunian objects, which have semi-major axes greater than 150 AU and perihelia well beyond Neptune (q > 40 AU). Both new objects have orbits with arguments of perihelia within the range of the clustering of this angle seen in the other known extreme objects. One of these objects, 2014 SR349, has a longitude of perihelion similar to the other extreme objects, but 2013 FT28 is about 180 degrees away or anti-aligned in its longitude of perihelion. We also discovered the first outer Oort cloud object with a perihelion beyond Neptune, 2014 FE72. We discuss these and other interesting objects discovered in our ongoing survey. All the high semi-major axis (a > 150 AU) and high perihelion (q > 35 AU) bodies follow the previously identified argument of perihelion clustering as first reported and explained as being from an unknown massive planet by Trujillo and Sheppard (2014), which some have called Planet X or Planet 9. With the discovery of 2013 FT28 on the opposite side of the sky, we now report that the argument of perihelion is significantly correlated with the longitude of perihelion and orbit pole angles for extreme objects and find there are two distinct extreme clusterings anti-aligned with each other. This previously unnoticed correlation is further evidence of an unknown massive planet on a distant eccentric inclined orbit, as extreme eccentric objects with perihelia on opposite sides of the sky (180 degree longitude of perihelion differences) would approach the inclined planet at opposite points in their orbits, thus making the extreme objects prefer to stay away

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“…Hence, they produce a "live" population in which perihelia are repeatedly, and slowly, elevated and depressed. This is in contrast to a "fossil" population induced by stellar encounters (Morbidelli & Levison 2004), where q changes are almost instantaneous, or capture of these bodies from a passing star (Jílková et al 2015). An excess of classical and large semimajor axis Centaurs, which are icy bodies with q among the giant planets and a > 100 au, would be natural in the continuously disturbed population (Gomes et al 2015).…”

Section: Sednoidsmentioning

confidence: 89%

Towards an explanation of orbits in the extreme trans-Neptunian region: The effect of Milgromian dynamics

Paučo

2017

A&A

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Context. Milgromian dynamics (MD or MOND) uniquely predicts motion in a galaxy from the distribution of its stars and gas in a remarkable agreement with observations so far. In the solar system, MD predicts the existence of some possibly non-negligible dynamical effects, which can be used to constrain the freedom in MD theories. Known extreme trans-Neptunian objects (ETNOs) have their argument of perihelion, longitude of ascending node, and inclination distributed in highly non-uniform fashion; ETNOs are bodies with perihelion distances greater than the orbit of Neptune and with semimajor axes greater than 150 au and less than ∼ 1500 au. It is as if these bodies have been systematically perturbed by some external force. Aims. We investigated a hypothesis that the puzzling orbital characteristics of ETNOs are a consequence of MD. Methods. We set up a dynamical model of the solar system incorporating the external field effect (EFE), which is anticipated to be the dominant effect of MD in the ETNOs region. We used constraints available on the strength of EFE coming from radio tracking of the Cassini spacecraft. We performed several numerical experiments, concentrating on the long-term orbital evolution of primordial (randomised) ETNOs in MD. Results. The EFE could produce distinct non-uniform distributions of the orbital elements of ETNOs that are related to the orientation of an orbit in space. If we demand that EFE is solely responsible for the detachment of Sedna and 2012 VP 113 , then these distributions are at odds with the currently observed statistics on ETNOs unless the EFE quadrupole strength parameter Q 2 has values that are unlikely (with probability < 1%) in light of the Cassini data.

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How Sedna and family were captured in a close encounter with a solar sibling

Cited by 80 publications

References 44 publications

OSSOS. V. Diffusion in the Orbit of a High-perihelion Distant Solar System Object

OSSOS. V. Diffusion in the Orbit of a High-perihelion Distant Solar System Object

New Extreme Trans-Neptunian Objects: Toward a Super-Earth in the Outer Solar System

Towards an explanation of orbits in the extreme trans-Neptunian region: The effect of Milgromian dynamics

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