8187 Akiramisawa

8187 Akiramisawa, provisional designation 1992 XL, is an Eos asteroid from the outer region of the asteroid belt. It was discovered by Japanese astronomer Satoru Otomo at Kiyosato Observatory (894) on 15 December 1992.[1] The assumed C-type asteroid has a rotation period of 5.8 hours and measures approximately 12 kilometers (7.5 miles) in diameter. It was named after Japanese botanist Akira Misawa (1942–1994).[3]

8187 Akiramisawa
Akiramisawa modeled from its lightcurve
Discovery [1][2]
Discovered byS. Otomo
Discovery siteKiyosato Obs. (894)
Discovery date15 December 1992
Designations
(8187) Akiramisawa
Named after
Akira Misawa
(Japanese botanist)[3]
1992 XL · 1971 UF4
1971 VV
main-belt [1][2] · (outer) [4]
Eos [5]
Orbital characteristics [2]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc44.79 yr (16,358 days)
Aphelion3.3523 AU
Perihelion2.6219 AU
2.9871 AU
Eccentricity0.1223
5.16 yr (1,886 days)
351.90°
0° 11m 27.24s / day
Inclination11.608°
83.066°
277.60°
Physical characteristics
Mean diameter
11.86 km (calculated)[4]
5.8153±0.0015 h[6]
0.057 (assumed)[4]
C (assumed)[4]
12.8[2] · 13.45±0.27[7] · 12.908±0.007 (R)[6] · 13.36[4]

    Orbit and classification

    Akiramisawa is a member the Eos family (606),[5] the largest asteroid family of the outer main belt consisting of nearly 10,000 known members.[8]:23 It orbits the Sun in the outer asteroid belt at a distance of 2.6–3.4 AU once every 5 years and 2 months (1,886 days). Its orbit has an eccentricity of 0.12 and an inclination of 12° with respect to the ecliptic.[2] In October 1971, it was first identified as 1971 UF4 at the Chilean Cerro El Roble Station, extending the body's observation arc by 21 years prior to its official discovery observation at Kiyosato.[1]

    Naming

    This minor planet was named in honour of Japanese botanist Akira Misawa (1942–1994), a professor at Chiba University , who examined the effects of light pollution on plants.[3] The official naming citation was published by the Minor Planet Center on 9 January 2001 (M.P.C. 41935).[9]

    Physical characteristics

    A rotational lightcurve of Akiramisawa was obtained from photometric observations made at the Palomar Transient Factory in June 2010. Lightcurve analysis gave a rotation period of 5.8153±0.0015 hours with a high brightness amplitude of 0.90 magnitude (U=2).[6] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for carbonaceous asteroids of 0.057, and calculates a diameter of 11.9 kilometers with an absolute magnitude of 13.36.[2]

    gollark: I don't think your 3D printer can print nanoscale circuitry.
    gollark: I can email you a Pi Zero if you work out a way to send structured matter in useful quantities by email.
    gollark: Robbery isn't that expensive. Alternatively, buy a "raspberry pi".
    gollark: Yes. If you steal someone's freezer, and it contains a microcontroller of some sort, it *might* be possible to run uCLinux on it.
    gollark: Muahahahaha, ALL are to enter the frequency domain.

    References
    1. "8187 Akiramisawa (1992 XL)". Minor Planet Center. Retrieved 4 May 2016.
    2. "JPL Small-Body Database Browser: 8187 Akiramisawa (1992 XL)" (2016-08-04 last obs.). Jet Propulsion Laboratory. Retrieved 22 June 2017.
    3. Schmadel, Lutz D. (2007). "(8187) Akiramisawa". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 637. doi:10.1007/978-3-540-29925-7_6888. ISBN 978-3-540-00238-3.
    4. "LCDB Data for (8187) Akiramisawa". Asteroid Lightcurve Database (LCDB). Retrieved 4 May 2016.
    5. "Asteroid 8187 Akiramisawa – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 27 October 2019.
    6. Waszczak, Adam; Chang, Chan-Kao; Ofek, Eran O.; Laher, Russ; Masci, Frank; Levitan, David; et al. (September 2015). "Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry". The Astronomical Journal. 150 (3): 35. arXiv:1504.04041. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. Retrieved 4 May 2016.
    7. Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 4 May 2016.
    8. Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). Identification and Dynamical Properties of Asteroid Families. Asteroids IV. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131.
    9. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 4 May 2016.
    This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.