Eris (dwarf planet)

Eris (dwarf planet)
Meli thev · CC BY-SA 4.0 · source
Name	Eris
Mp category	Dwarf planet
Satellites	Dysnomia

Eris (dwarf planet) Eris is a trans-Neptunian dwarf planet located in the scattered disc beyond Neptune, notable for its high orbital eccentricity and for triggering the 2006 redefinition of planetary status by the International Astronomical Union. Discovered in the early 21st century, it has been studied with telescopes associated with institutions such as Palomar Observatory, W. M. Keck Observatory, and Hubble Space Telescope. Eris influenced debates involving figures and organizations including Mike Brown, Clyde Tombaugh, Galileo Galilei, Isaac Newton, and the International Astronomical Union General Assembly.

Discovery and naming

The discovery announcement linked teams at Palomar Observatory and individuals such as Mike Brown, Chad Trujillo, and David Rabinowitz using instruments influenced by designs from George Ellery Hale and techniques applied at Mount Wilson Observatory. Initial astrometric work drew on methods used in surveys at Kitt Peak National Observatory, Mauna Kea Observatories, and datasets cross-referenced with archives from Sloan Digital Sky Survey and Two Micron All Sky Survey. The object’s provisional designation joined cataloging schemes from Minor Planet Center protocols and nomenclature overseen later by the International Astronomical Union. Naming considerations referenced mythological traditions and involved cultural bodies similar to those participating in the naming of Pluto and Charon. The IAU decision in 2006 that led to the classification of several bodies, including the status affecting Pluto and Ceres, drew commentary from astronomers affiliated with California Institute of Technology, Harvard-Smithsonian Center for Astrophysics, and Max Planck Institute for Solar System Research.

Orbital characteristics

Eris follows a highly elliptical orbit in the scattered disc, with parameters determined by observations from Hubble Space Telescope, W. M. Keck Observatory, and long-baseline measurements that used reference frames tied to International Celestial Reference Frame standards. Its orbital period, perihelion, aphelion, semimajor axis, eccentricity, and inclination were refined through catalogs maintained by Jet Propulsion Laboratory and computations using algorithms developed in the tradition of Johannes Kepler and Pierre-Simon Laplace. The dynamics of Eris’s orbit interact weakly with resonances studied in the context of Neptune migrations as modeled by researchers influenced by the Nice model and simulations run on systems like Los Alamos National Laboratory clusters and NASA supercomputing facilities. Long-term evolution studies referenced work by teams at University of Arizona, University of California, Berkeley, and Max Planck Institute for Astronomy.

Physical properties

Measurements of Eris’s mass, radius, density, and albedo combined data from stellar occultations observed by networks including American Association of Variable Star Observers contributors and adaptive optics imaging at facilities like Keck Observatory and Very Large Telescope. Mass estimates used orbital analysis of its moon Dysnomia, invoking methods developed by astronomers such as Simon Newcomb and institutions like Jet Propulsion Laboratory and European Space Agency. Spectroscopic signatures in visible and infrared were obtained using instruments related to projects at Infrared Space Observatory, Spitzer Space Telescope, and ground-based arrays operated by groups at Caltech and University of Hawaii. Comparative discussions referenced bodies such as Pluto, Makemake, Haumea, Ceres, and Charon.

Surface and geology

Surface composition inferences combined near-infrared spectroscopy from groups working with Gemini Observatory and laboratory analogs studied at facilities like Smithsonian Institution and Carnegie Institution for Science. Evidence for volatile ices, crystalline phases, and irradiation products drew on analogies with results from missions and studies involving New Horizons, Rosetta, and laboratory experiments influenced by researchers at NASA Ames Research Center. Geological interpretations considered processes discussed in papers from Brown University, MIT, and University of Colorado Boulder about cryovolcanism, impact cratering, and regolith gardening on distant icy bodies.

Atmosphere and exosphere

Searches for a transient atmosphere or exosphere used stellar occultation campaigns coordinated with societies such as International Occultation Timing Association and instrumentation developed by teams at University of California, Santa Cruz and Observatoire de Paris. Models of surface-atmosphere exchange and photochemistry invoked principles from the work of Gerard P. Kuiper and later atmospheric modeling groups at NASA Goddard Space Flight Center and Laboratoire de Météorologie Dynamique. Comparisons were made with tenuous atmospheres detected or inferred on Pluto, Titan, and Triton in studies led by researchers affiliated with Southwest Research Institute and Johns Hopkins University Applied Physics Laboratory.

Moons (Dysnomia)

Eris’s known satellite, Dysnomia, was imaged with adaptive optics at W. M. Keck Observatory and resolved in observations by Hubble Space Telescope, with orbital parameters analyzed by teams at Jet Propulsion Laboratory and European Southern Observatory. Dynamical studies of the binary system referenced tidal evolution theories developed by George Darwin and later applied in studies at University of California, Santa Cruz and University of Michigan. Dysnomia’s discovery stimulated work comparing satellite systems such as Charon, the moons of Pluto, and irregular satellites cataloged by Minor Planet Center and observers at Mount Palomar.

Formation and classification

Hypotheses for Eris’s formation referenced accretion models from researchers at Institut d’Astrophysique de Paris, Max Planck Institute for Astronomy, and proponents of scenarios such as planetesimal-driven migration studied in the context of the Nice model and the Grand Tack hypothesis debates involving teams at University of Lisbon and University of Bern. Classification issues that led to the 2006 IAU definition drew responses from astronomers at Caltech, Harvard University, and Smithsonian Astrophysical Observatory, and remain discussed in symposia convened by organizations like American Astronomical Society and panels at International Astronomical Union General Assembly.

Category:Trans-Neptunian objects