2002 CY248

Last updated
2002 CY248
Discovery  [1] [2]
Discovered by M. W. Buie
Discovery site Kitt Peak National Obs.
Discovery date 6 February 2002
(first observed only)
Designations
MPC designation 2002 CY248
TNO   [3]  · cubewano   [4] [5]
p-DP   [6]  · distant   [1]
Orbital characteristics   [3]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 3
Observation arc 12.96 yr (4,733 days)
Aphelion 53.081 AU
Perihelion 39.404 AU
46.243 AU
Eccentricity 0.1479
314.47 yr (114,859 d)
233.51°
0° 0m 11.16s / day
Inclination 7.0487°
300.74°
336.77°
Physical characteristics
Mean diameter
 404 km [5]
449 km [6]
0.06 (assumed) [6]
0.09 (assumed) [5]
5.2 [3]  ·5.5 [6]

    2002 CY248 is a trans-Neptunian object and weak dwarf-planet candidate from the classical Kuiper belt in the outermost region of the Solar System, approximately 400–450 kilometers (250–280 mi) in diameter. It was first observed on 6 February 2002, by American astronomer Marc Buie at the Kitt Peak National Observatory in Arizona, United States. [1]

    Trans-Neptunian object any object in the Solar System that orbits the Sun at a greater average distance than Neptune

    A trans-Neptunian object (TNO), also written transneptunian object, is any minor planet in the Solar System that orbits the Sun at a greater average distance than Neptune, which has a semi-major axis of 30.1 astronomical units (AU).

    Solar System planetary system of the Sun

    The Solar System is the gravitationally bound planetary system of the Sun and the objects that orbit it, either directly or indirectly. Of the objects that orbit the Sun directly, the largest are the eight planets, with the remainder being smaller objects, such as the five dwarf planets and small Solar System bodies. Of the objects that orbit the Sun indirectly—the moons—two are larger than the smallest planet, Mercury.

    Kitt Peak National Observatory United States astronomical observatory

    The Kitt Peak National Observatory (KPNO) is a United States astronomical observatory located on Kitt Peak of the Quinlan Mountains in the Arizona-Sonoran Desert on the Tohono O'odham Nation, 88 kilometers (55 mi) west-southwest of Tucson, Arizona. With 22 optical and two radio telescopes, it is the largest, most diverse gathering of astronomical instruments in the northern hemisphere. The observatory is administered by the National Optical Astronomy Observatory (NOAO).

    Contents

    Orbit and classification

    2002 CY248 orbits the Sun at a distance of 39.4–53.1  AU once every 314 years and 6 months (114,859 days; semi-major axis of 46.2 AU). Its orbit has an eccentricity of 0.15 and an inclination of 7° with respect to the ecliptic. [3] The body's observation arc begins at Kitt Peak with its official first observation on 6 February 2002. [1] A 10-million-year integration of the orbit shows that it is a Classical Kuiper belt object that does not get closer to the Sun than 38.8  AU (5.80  billion   km ) or further than 54 AU. [4]

    Astronomical unit mean distance between Earth and the Sun, common length reference in astronomy

    The astronomical unit is a unit of length, roughly the distance from Earth to the Sun. However, that distance varies as Earth orbits the Sun, from a maximum (aphelion) to a minimum (perihelion) and back again once a year. Originally conceived as the average of Earth's aphelion and perihelion, since 2012 it has been defined as exactly 149597870700 metres or about 150 million kilometres. The astronomical unit is used primarily for measuring distances within the Solar System or around other stars. It is also a fundamental component in the definition of another unit of astronomical length, the parsec.

    Orbital eccentricity parameter that determines the amount by which an orbit deviates from a perfect circle

    The orbital eccentricity of an astronomical object is a parameter that determines the amount by which its orbit around another body deviates from a perfect circle. A value of 0 is a circular orbit, values between 0 and 1 form an elliptic orbit, 1 is a parabolic escape orbit, and greater than 1 is a hyperbola. The term derives its name from the parameters of conic sections, as every Kepler orbit is a conic section. It is normally used for the isolated two-body problem, but extensions exist for objects following a Klemperer rosette orbit through the galaxy.

    Orbital inclination angle between a reference plane and the plane of an orbit

    Orbital inclination measures the tilt of an object's orbit around a celestial body. It is expressed as the angle between a reference plane and the orbital plane or axis of direction of the orbiting object.

    Physical characteristics

    Based on an absolute magnitude of 5.2, [3] and an assumed albedo of 0.09, the Johnston's archive estimates a mean-diameter of approximately 404 kilometers (251 mi), [5] while astronomer Michael Brown assumes an albedo of 0.06 and calculates a diameter of 449 kilometers (279 mi) using a fainter magnitude of 5.5. Brown also characterizes the object as a "probable dwarf planet", an intermediate category in his classification scheme (also see list of candidates). [6]

    Absolute magnitude is a measure of the luminosity of a celestial object, on a logarithmic astronomical magnitude scale. An object's absolute magnitude is defined to be equal to the apparent magnitude that the object would have if it were viewed from a distance of exactly 10 parsecs, with no extinction of its light due to absorption by interstellar dust particles. By hypothetically placing all objects at a standard reference distance from the observer, their luminosities can be directly compared on a magnitude scale. As with all astronomical magnitudes, the absolute magnitude can be specified for different wavelength ranges corresponding to specified filter bands or passbands; for stars a commonly quoted absolute magnitude is the absolute visual magnitude, which uses the visual (V) band of the spectrum. Absolute magnitudes are denoted by a capital M, with a subscript representing the filter band used for measurement, such as MV for absolute magnitude in the V band.

    Michael E. Brown American planetary astronomer

    Michael E. Brown is an American astronomer, who has been professor of planetary astronomy at the California Institute of Technology (Caltech) since 2003. His team has discovered many trans-Neptunian objects (TNOs), notably the dwarf planet Eris, which was originally thought to be bigger than Pluto.

    As of 2018, no rotational lightcurve of this object has been obtained from photometric observations. The object's rotation period, pole and shape remain unknown. [3]

    Photometry is a technique of astronomy concerned with measuring the flux, or intensity of an astronomical object's electromagnetic radiation. When photometry is performed over broad wavelength bands of radiation, where not only the amount of radiation but also its spectral distribution is measured, the term spectrophotometry is used.

    Rotation period (of a celestial object) time that it takes to complete one revolution around its axis of rotation relative to the background stars

    In astronomy, the rotation period of a celestial object is the time that it takes to complete one revolution around its axis of rotation relative to the background stars. It differs from the planet's solar day, which includes an extra fractional rotation needed to accommodate the portion of the planet's orbital period during one day.

    The poles of astronomical bodies are determined based on their axis of rotation in relation to the celestial poles of the celestial sphere. Astronomical bodies include stars, planets, dwarf planets and small Solar System bodies such as comets and minor planets, as well as natural satellites and minor-planet moons.

    Numbering and naming

    As of 2018, this minor planet has not been numbered or named. [1]

    Minor planet astronomical object in direct orbit around a star that is neither a planet nor originally classified as a comet

    A minor planet is an astronomical object in direct orbit around the Sun that is neither a planet nor exclusively classified as a comet. Before 2006 the International Astronomical Union (IAU) officially used the term minor planet, but during that year's meeting it reclassified minor planets and comets into dwarf planets and small Solar System bodies (SSSBs).

    See also

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    References

    1. 1 2 3 4 5 "2002 CY248". Minor Planet Center. Retrieved 23 February 2018.
    2. ↑ "List Of Transneptunian Objects". Minor Planet Center. Retrieved 23 February 2018.
    3. 1 2 3 4 5 6 "JPL Small-Body Database Browser: (2002 CY248)" (2015-01-22 last obs.). Jet Propulsion Laboratory . Retrieved 23 February 2018.
    4. 1 2 Buie, Marc W. "Orbit Fit and Astrometric record for 02CY248". SwRI (Space Science Department). Retrieved 2018-02-17.
    5. 1 2 3 4 Johnston, Wm. Robert (30 December 2017). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 23 February 2018.
    6. 1 2 3 4 5 Brown, Michael E. "How many dwarf planets are there in the outer solar system?". California Institute of Technology . Retrieved 23 February 2018.

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