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| (136199) Eris | |
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| Name | (136199) Eris |
(136199) Eris Eris is a trans-Neptunian dwarf planet in the scattered disc that is one of the most massive known minor planets in the Solar System. It has been central to debates involving Kuiper belt, Pluto, International Astronomical Union, Mike Brown, Caltech, and the 2006 redefinition of planet. Eris's discovery reshaped surveys of trans-Neptunian objects, influenced studies by institutions such as Hubble Space Telescope, Palomar Observatory, and motivated missions conceptually related to New Horizons.
Eris was discovered in 2005 by a team led by Mike Brown at Palomar Observatory using the Samuel Oschin Telescope, during surveys that also identified Haumea and Makemake. The announcement intersected with media outlets like Nature (journal), Science (journal), and public discussions at NASA, provoking responses from the International Astronomical Union and figures such as Gordon L. Kane and Alan Stern. The provisional designation preceded the formal numbering granted by the Minor Planet Center, and the chosen name draws on Eris (mythology), invoking connections to ancient Greek literature and iconography preserved in collections such as the British Museum and discussed by scholars like Homer and Hesiod.
Eris follows a highly eccentric, inclined orbit in the scattered disc with aphelion and perihelion positions that place it beyond Neptune and occasionally farther than Sedna (planetoid). Its orbital parameters have been refined through observations by Hubble Space Telescope, Keck Observatory, and astrometric reductions using techniques developed at Jet Propulsion Laboratory and the European Space Agency. Debates over classification involved committees within the International Astronomical Union and drew comparisons to Pluto, Ceres, and objects catalogued by the Minor Planet Center.
Eris's mass and radius measurements, constrained via observations of its satellite discovered at Palomar Observatory and follow-up by Hubble Space Telescope, indicate a mass greater than that of Pluto and a density consistent with a rock-ice mixture similar to Haumea and Makemake. Photometric and spectroscopic campaigns using instruments on Keck Observatory, Very Large Telescope, and Spitzer Space Telescope have informed estimates of its albedo and rotation period, with contributions from modeling groups at Caltech, University of Arizona, and MIT.
Spectroscopy of Eris in the near-infrared and visible, performed with facilities like Keck Observatory, Very Large Telescope, and the Gemini Observatory, reveals strong signatures attributed to frozen methane similar to spectra of Triton and Pluto. Comparisons to laboratory work at institutions such as NASA Ames Research Center and Max Planck Institute for Solar System Research support interpretations of volatile ices layered on a predominantly water-ice and silicate substrate analogous to bodies studied by Voyager 2 and Cassini–Huygens.
Eris's extreme distance from Sun suggests surface temperatures comparable to other distant trans-Neptunian objects; thermal modeling by teams affiliated with Jet Propulsion Laboratory and European Southern Observatory uses data from Spitzer Space Telescope and Herschel Space Observatory to estimate effective temperatures and volatile retention. While no persistent atmosphere like that of Pluto has been firmly detected, transient sublimation-driven exospheres analogous to those proposed for Comet 67P/Churyumov–Gerasimenko and seasonal models developed for Triton remain subjects of study by groups at Cornell University and University of California, Berkeley.
Eris hosts one known satellite discovered in 2005 using the Hubble Space Telescope; photometric and dynamical analysis of the satellite's orbit allowed direct determination of Eris's mass by teams at Caltech and University of Arizona. The system has been compared to other satellite-bearing minor planets such as Pluto–Charon and Haumea; searches for additional moons or ring material have employed instruments on Hubble Space Telescope, Keck Observatory, and adaptive optics systems deployed by European Southern Observatory.
The origin of Eris is interpreted within frameworks involving planetesimal accretion, dynamical scattering by ice giants like Neptune and migration scenarios articulated in the Nice model and alternatives developed by groups at CEA Saclay and University of Bern. Collisional histories inferred from comparisons to family-forming events such as those hypothesized for Haumea and models of early Solar System evolution studied at Harvard–Smithsonian Center for Astrophysics inform hypotheses about Eris's internal differentiation, volatile inventory, and long-term orbital evolution influenced by resonances with Neptune and past interactions with passing stars discussed in work connected to Gaia (spacecraft).