21509 Lucascavin

21509 Lucascavin, provisional designation 1998 KL35, is a small asteroid from the inner regions of the asteroid belt, approximately 2.5 kilometers (1.6 miles) in diameter. It is the namesake of the tiny Lucascavin family located within the Flora clan. It was discovered on 22 May 1998, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico.[1] The presumed S-type asteroid has a rotation period of 5.8 hours.[4] It was named for the 2005-ISEF awardee Lucas James Cavin.[1]

21509 Lucascavin
Discovery [1]
Discovered byLINEAR
Discovery siteLincoln Lab's ETS
Discovery date22 May 1998
Designations
(21509) Lucascavin
Named after
Lucas James Cavin [1]
(2005 ISEF awardee)
1998 KL35 · 1982 VD3
main-belt [1][2] · (inner)
Lucascavin [3] · Flora [3][4]
Baptistina [3] · Duponta [5]
Orbital characteristics [2]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 0
Observation arc35.44 yr (12,944 d)
Aphelion2.5369 AU
Perihelion2.0276 AU
2.2822 AU
Eccentricity0.1116
3.45 yr (1,259 d)
189.97°
0° 17m 9.24s / day
Inclination5.9813°
70.168°
4.4723°
Physical characteristics
Mean diameter
2.54 km (calculated)[4]
5.784±0.004 h[6]
0.24 (assumed)[4]
S (assumed)[4]
V–R = 0.474±0.016[6]
14.68±0.07 (R)[6]
14.9[1][2]

    Orbit and classification

    According to a HCM-analysis by David Nesvorný, Lucascavin is the namesake of the Lucascavin family (412),[3] a tight, young cluster between 200 and 800 thousand years old,[6][7] which consists of 3 known asteroids only – the others are (180255) and (209570). The cluster in turn belongs to the encompassing Baptistina family (403) within the larger Florian region (402).[3][8] Since other astronomers have ruled out the existence of a Flora family in the first place, Lucascavin has also been grouped to the alternative Duponta family, a core group inside the Florian region.[5]

    Lucascavin orbits the Sun in the inner asteroid belt at a distance of 2.0–2.5 AU once every 3 years and 5 months (1,259 days; semi-major axis of 2.28 AU). Its orbit has an eccentricity of 0.11 and an inclination of 6° with respect to the ecliptic.[2] The body's observation arc begins with its first observation as 1982 VD3 at Kiso Observatory in November 1982, more than 15 years prior to its official discovery observation.[1]

    Naming

    This minor planet was named after Lucas James Cavin (born 1986) who won the second place in the 2005 Intel International Science and Engineering Fair for his engineering project.[1] The official naming citation was published by the Minor Planet Center on 22 August 2005 (M.P.C. 54702).[9] At the time he attended the Chillico High School in Missouri, United States.[1]

    Physical characteristics

    Lucascavin is an assumed S-type asteroid,[4] in agreement with the overall spectral type of the Lucascavin, Baptistina and Flora family groupings.[3][8]:23

    Rotation period

    Between 2006 and 2016, several rotational lightcurves of Lucascavin have been obtained from photometric observations by Czech astronomer Petr Pravec. Best-rated lightcurve analysis from 2013 gave a rotation period of 5.784±0.004 hours with a consolidated brightness amplitude between 0.23 and 0.30 magnitude (U=2/3/3-).[4][6] Pravec also determined a low V–R color index of 0.474.[6]

    Diameter and albedo

    The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.24 – derived from 8 Flora the namesake of the Flora clan – and calculates a diameter of 2.54 kilometers based on an absolute magnitude of 15.14.[4]

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    References
    1. "21509 Lucascavin (1998 KL35)". Minor Planet Center. Retrieved 5 December 2018.
    2. "JPL Small-Body Database Browser: 21509 Lucascavin (1998 KL35)" (2018-04-23 last obs.). Jet Propulsion Laboratory. Retrieved 5 December 2018.
    3. "Asteroid 21509 Lucascavin". Small Bodies Data Ferret. Retrieved 5 December 2018.
    4. "LCDB Data for (21509) Lucascavin". Asteroid Lightcurve Database (LCDB). Retrieved 5 December 2018.
    5. "Asteroid (21509) Lucascavin". AstDyS-2, Asteroids – Dynamic Site. Retrieved 4 December 2018.
    6. Pravec, P.; Fatka, P.; Vokrouhlický, D.; Scheeres, D. J.; Kusnirák, P.; Hornoch, K.; et al. (April 2018). "Asteroid clusters similar to asteroid pairs" (PDF). Icarus. 304: 110–126. Bibcode:2018Icar..304..110P. doi:10.1016/j.icarus.2017.08.008. Retrieved 5 December 2018.
    7. Nesvorný, D.; Vokrouhlický, D. (November 2006). "New Candidates for Recent Asteroid Breakups". The Astronomical Journal. 132 (5): 1950–1958. Bibcode:2006AJ....132.1950N. doi:10.1086/507989.
    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 5 December 2018.

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