(450894) 2008 BT18

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(450894) 2008 BT18
2008 BT18 arecibo.gif
Radar image of 2008 BT18 and its satellite from Arecibo Observatory in July 2008
Discovery [1]
Discovered by LINEAR
Discovery site Lincoln Lab's ETS
Discovery date31 January 2008
Designations
(450894) 2008 BT18
2008 BT18
Apollo  · NEO  · PHA [1] [2]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 60.59 yr (22,132 days)
Earliest precovery date14 March 1955
Aphelion 3.5401 AU
Perihelion 0.9030 AU
2.2216 AU
Eccentricity 0.5935
3.31 yr (1,209 days)
284.48°
0° 17m 51.72s / day
Inclination 8.1338°
107.67°
139.28°
Known satellites 1 [3] [a] [b]
Earth  MOID 0.0108 AU ·4.2 LD
Physical characteristics
Dimensions 0.6 km [3] [a]
0.650 km (calculated) [4]
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 asteroid and synchronous binary system, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. It was discovered on 31 January 2008, by the LINEAR program at 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]

    Contents

    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 minimum orbit intersection distance of 0.0108 AU (1,620,000 km) which corresponds to 4.2 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 lightcurve for 2008 BT18 was obtained from photometric observations made by astronomer Alberto Silva Betzler at Salvador, Brazil, in July 2008. The lightcurve gave a rotation period of 2.726±0.007 hours with a brightness variation of 0.04 in magnitude ( U=1 ). [5]

    Binary system

    Radar image of 2008 BT18 and its satellite by Arecibo Observatory on 1 July 2008 2008bt18 jul11 arecibo.gif
    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 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 basaltic achondrite, suggesting that its parent body was subjected to sufficiently high temperatures to produce a eutectic melt. [6] The body's surface is thought to be dominated by iron-rich orthopyroxenes with little or no olivine. [6]

    Naming

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

    Notes

    References

    1. 1 2 3 4 5 6
    2. 1 2 3 4
    3. 1 2 3 4
    4. 1 2 3 4 5
    5. 1 2 3 4
    6. 1 2 3 4 5
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