3 Juno

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3 Juno
[[Image:Juno moving among background stars|275px|]]
Discovery A
Discoverer Karl Ludwig Harding
Discovery date September 1, 1804
Alternate
designations
B
none
Category Main belt (Juno clump)
Orbital elements C
Epoch November 25, 2005 (JD 2453699.5)
Eccentricity (e) 0.2583
Semi-major axis (a) 399.155 Gm (2.668 AU)
Perihelion (q) 296.03 Gm (1.979 AU)
Aphelion (Q) 502.276 Gm (3.358 AU)
Orbital period (P) 1591.93 d (4.36 a)
Mean orbital speed 17.93 km/s
Inclination (i) 12.971°
Longitude of the
ascending node
(Ω)
170.125°
Argument of
perihelion
(ω)
247.839°
Mean anomaly (M) 7.879°
Physical characteristics D
Dimensions 290×240×190 km
Mass 3.0×1019 kg[1]
Density 3.4 g/cm³
Surface gravity 0.12 m/s²
Escape velocity 0.18 km/s
Rotation period 0.3004 d
Spectral class S-type asteroid
Absolute magnitude 5.33
Albedo (geometric) 0.238[2]
Mean surface
temperature
~163 K
max: 301 K (+28° C)[5]
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Juno (jew'-noe (key)), designated 3 Juno in the Minor Planet Center catologue system, was the third asteroid to be discovered and is one of the largest main belt asteroids, being the second heaviest of the stony S-type. It was discovered on September 1, 1804 by German astronomer Karl L. Harding and named after the mythological figure Juno, the highest Roman goddess. The adjectival form of the name is Junonian.

Contents

[edit] Characteristics

Size comparison: the first 10 asteroids profiled against Earth's Moon. Juno is third from the left.
Enlarge
Size comparison: the first 10 asteroids profiled against Earth's Moon. Juno is third from the left.

Juno is one of the largest asteroids, containing approximately 1.0% the mass of the entire asteroid belt. In a ranking by size, it is tenth. It vies with 15 Eunomia for the honour of being the largest of the stony S-type asteroids, although the newest estimates put Juno in second place. Amongst S-types it is unusually reflective, which may be indicative of different surface properties. This high reflectivity along with Juno's high eccentricity (the highest of any known object until Polyhymnia was discovered in 1854) explains its relatively high magnitude and its discovery predating that of the larger asteroids Hygiea, Europa, Davida and Interamnia. It is the main body in the Juno family.

Juno was originally considered a planet, along with 1 Ceres, 2 Pallas, and 4 Vesta. It was re-classified as an asteroid, with the other three, when many more additional asteroids were discovered. Juno's small size and irregular shape preclude it from being considered a dwarf planet under the IAU classification.

Juno rotates in a prograde direction, with the north pole pointing towards ecliptic coordinates (β, λ) = (27°, 103°) with a 10° uncertainty[3]. This gives an axial tilt of 51°.

Spectroscopic studies of the Junonian surface permit the conclusion that Juno could be the body of origin of ordinary chondrites, a common group of stony meteorites composed of iron-containing silicates such as olivine and pyroxene[4]. The maximum temperature on the surface, when the sun is overhead, was measured at about 293 K on October 2, 2001. Taking into account also the heliocentric distance at the time, this gives an estimated maximum of 301 K (+28°C) at perihelion [5].

Infrared images reveal that it possesses an approximately 100 km wide crater or ejecta feature, the result of a geologically young impact[6].

[edit] Observations

Some notable observation milestones for Juno include:

Juno was the first asteroid for which an occultation was observed. It passed in front of a dim star (SAO 112328) on February 19, 1958. Since then, several occultations by Juno have been observed, the most fruitful being on December 11, 1979 which was registered by 18 observers[7].

Radio signals from spacecraft in orbit around Mars and/or on its surface have been used to estimate the mass of Juno from the tiny perturbations induced by it onto the motion of Mars.

A study by James L. Hilton (1999) suggests that Juno's orbit changed (slightly) around 1839[8], "very likely" due to perturbations from a passing asteroid, whose identity has not been determined yet. An alternate yet unlikely explanation is an impact by a sizeable body.

In 1996, Juno was imaged by the Hooker Telescope at Mount Wilson Observatory, using adaptive optics. The images spanned a whole rotation period and revealed an irregular (lumpy) shape with a dark feature, interpreted as a fresh impact site.


[edit] Aspects

Stationary,
retrograde
Opposition Distance to
Earth (AU)
Maximum
brightness (mag)
Stationary,
prograde
Conjunction
to Sun
November 2, 2005 December 9, 2005 1.06025 7.5 January 16, 2006 February 24, 2005
February 19, 2007 April 10, 2007 2.13320 9.7 June 5, 2007 September 2, 2006
April 18, 2008 June 12, 2008 2.28071 10.1 August 10, 2008 November 14, 2007
August 15, 2009 September 21, 2009 1.18972 7.6 October 31, 2009 January 18, 2009
January 24, 2011 March 13, 2011 1.78236 8.9 May 1, 2011 July 10, 2010
March 27, 2012 May 20, 2012 2.37727 10.2 July 20, 2012 October 23, 2011
June 14, 2013 August 4, 2013 1.67506 8.9 September 21, 2013 December 23, 2012
December 17, 2014 February 1, 2015 1.33782 8.2 March 12, 2015 April 13, 2014
March 7, 2016 April 28, 2016 2.30641 10.0 June 27, 2016 September 28, 2015
May 9, 2017 July 3, 2017 2.07904 9.7 August 27, 2017 November 30, 2016
October 20, 2018 November 22, 2018 1.03276 7.4 December 31, 2018 February 16, 2018
February 14, 2020 April 4, 2020 2.07425 9.6 May 29, 2020 August 25, 2019
April 14, 2021 June 8, 2021 2.31368 10.1 August 6, 2021 November 9, 2020

[edit] References

  1. ^ E. V. Pitjeva, Estimations of Masses of the Largest Asteroids and the Main Asteroid Belt From Ranging to Planets, Mars Orbiters And Landers Solar System Resarch, Vol. 39 pp. 176 (2005).
  2. ^ Supplemental IRAS Minor Planet Survey
  3. ^ M. Kaasalainen et al Models of Twenty asteroids from photometric data, Icarus, Vol. 159, p. 369 (2002).
  4. ^ M. J. Gaffey Mineralogical variations within the S-type asteroid class, icarus, Vol. 106, pp. 573 (1993).
  5. ^ L. F. Lim et al Thermal infrared (8-13μm) spectra of 29 asteroids: the Cornell Mid-Infrared Asteroid Spectroscopy (MIDAS) Survey, Icarus, Vol. 173, pp. 385 (2005).
  6. ^ Mt Wilson Observatory S. Baliunas et al Multispectral analysis of asteroid 3 Juno taken with the 100-inch telescope at Mount Wilson Observatory, Icarus, Vol. 163, pp 135 (2003).
  7. ^ L. Millis et al The diameter of Juno from its occultation of AG+0°1022, The Astronomical Journal, Vol. 86, pp. 306 (1981).
  8. ^ James L. Hilton, U.S. Naval Observatory Ephemerides of the Largest Asteroids The Astronomical Journal, Vol. 117 pp. 1077 (1999)

[edit] External links

[edit] See also


Minor planets
Previous minor planet 3 Juno Next minor planet
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Small Solar System bodies
Vulcanoids | Near-Earth asteroids | Main belt | Jupiter Trojans | Centaurs | Damocloids | Comets | Trans-Neptunians (Kuiper belt · Scattered disc · Oort cloud)
For other objects and regions, see: asteroid groups and families, binary asteroids, asteroid moons and the Solar system
For a complete listing, see: List of asteroids. See also Pronunciation of asteroid names and Meanings of asteroid names.