(450894) 2008 BT18

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(450894) 2008 BT18
Synodic rotation period
2.726±0.007 h[5]
0.20 (assumed)[4]
V[5][6] · S (assumed)[4]
18.3[1][4]

(450894) 2008 BT18 is a sub-kilometer

Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, United States.[2] The eccentric asteroid measures approximately 600 meters in diameter and has a composition of a basaltic achondrite.[6]

In 2008, its minor-planet moon, designated S/2008 (450894) 1, was discovered by radar astronomers. It measures approximately 200 meters in diameter, or one third of its primary.[3][b]

Orbit and classification

2008 BT18 orbits the Sun at a distance of 0.9–3.5 AU once every 3 years and 4 months (1,209 days). Its orbit has an eccentricity of 0.59 and an inclination of 8° with respect to the ecliptic.[1] Published by the Digitized Sky Survey, a first precovery was taken at Palomar Observatory in 1955, extending the asteroid's observation arc by 53 years prior to its discovery.[2]

The asteroid has a low Earth

lunar distances (LD). On 14 July 2008, it transited Earth within 0.015 AU (5.9 LD).[1]

Physical characteristics

2008 BT18 has been characterized as a V-type asteroid by astronomers using the SpeX spectrograph at NASA Infrared Telescope Facility, IRTF.[5][6]

Rotation period

A rotational

U=1).[5]

Binary system

Radar image of 2008 BT18 and its satellite by Arecibo Observatory on 1 July 2008

On 6 and 7 July 2008, research conducted using the Arecibo Observatory produced evidence that 2008 BT18 is a synchronous binary asteroid with a minor-planet moon in its orbit. The secondary component, provisionally designated S/2008 (450894) 1, has a diameter of at least 200 meters, about 33% the size of and up to 1.5 kilometers apart from its primary.[3][a][b] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 650 meters, based on an absolute magnitude of 18.3.[4]

There are more than 60 binary near-Earth objects known to exist (2016).

Mineralogy

On 26 July 2008, observations at the IRTF using the SpeX-spectrograph showed that 2008 BT18 is a

orthopyroxenes with little or no olivine.[6]

Naming

As of 2017, this minor planet remains unnamed.[2]

Notes

  1. ^ a b c Benner (2008) web: diameter 0.6 kilometers. Central Bureau Electronic Telegrams, No. 1450, #1 (2008). Summary figures at Collaborative Asteroid Lightcurve Link (CALL) for (450894)
  2. ^ a b c Central Bureau for Astronomical Telegrams, No. 1450, from 29 July 2008:
    Arecibo (2380-MHz, 12.6-cm) and Goldstone (8560-MHz, 3.5-cm) radar observations during July 6, 7, and 11 reveal that minor planet 2008 BT_18 (cf. MPECs 2008-C03, 2008-H06; MPO 140193) is a binary system. Preliminary estimates for the component diameters are about 0.6 km and > 200 m. The maximum distance between the components on July 11 is at least 1.5 km.
    Reported by: L. A. M. Benner, Jet Propulsion Laboratory (JPL), California Institute of Technology (CIT); M. C. Nolan and E. S. Howell, Arecibo Observatory, National Astronomy and Ionosphere Center; C. Magri, University of Maine at Farmington; J. D. Giorgini, S. J. Ostro, and M. Brozovic, JPL/CIT; M. W. Busch, CIT; J. L. Margot and P. A. Taylor, Cornell University; M. K. Shepard, Bloomsburg University; L. M. Carter, Smithsonian Institution; and T. M. Becker, Lehigh University CBET No. 1450

References

  1. ^ a b c d e f "JPL Small-Body Database Browser: 450894 (2008 BT18)" (2015-10-17 last obs.). Jet Propulsion Laboratory. Retrieved 2 June 2017.
  2. ^ a b c d "450894 (2008 BT18)". Minor Planet Center. Retrieved 21 May 2016.
  3. ^ a b c d Johnston, Wm. Robert (18 February 2017). "Asteroids with Satellites Database – (450894) 2008 BT18". Johnston's Archive. Retrieved 15 November 2017.
  4. ^ a b c d e "LCDB Data for (450894)". Asteroid Lightcurve Database (LCDB). Retrieved 21 May 2016.
  5. ^
    ISSN 1052-8091
    . Retrieved 16 November 2017.
  6. ^ . Retrieved 16 November 2017.

External links