3353 Jarvis

3353 Jarvis, or by its provisional designation, 1981 YC, is a carbonaceous Hungaria asteroid, slow rotator and suspected tumbler from the inner regions of the asteroid belt, approximately 10 kilometers in diameter.

3353 Jarvis
Discovery [1]
Discovered byE. Bowell
Discovery siteAnderson Mesa Stn.
Discovery date20 December 1981
Designations
(3353) Jarvis
Named after
Gregory Jarvis
(Challenger crew member)[2]
1981 YC
main-belt · (inner) [1] · Hungaria [3][4]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc36.76 yr (13,427 days)
Aphelion2.0208 AU
Perihelion1.7050 AU
1.8629 AU
Eccentricity0.0848
2.54 yr (929 days)
158.84°
0° 23m 15.36s / day
Inclination21.809°
245.60°
34.803°
Physical characteristics
Dimensions9.70 km (derived)[4]
9.72±0.5 km[5]
10.062±0.030 km[6]
10.07±1.07 km[7]
10.528±0.044 km[8]
11.01±2.52 km[9]
12.49±0.29 km[10]
40.8±0.1 h (dated)[11]
202.0±0.5 h[12][lower-alpha 1]
0.030±0.005[6]
0.046±0.003[10]
0.0487±0.0028[8]
0.05±0.01[9]
0.06±0.01[7]
0.0622 (derived)[4]
0.0744±0.007[5]
C · ES [4][lower-alpha 1]
12.91±0.51[13] · 13.5[5][8][10] · 13.60[9] · 13.7[1][4] · 13.75[7]

    It was discovered on 20 December 1981, by American astronomer Edward Bowell at Lowell's Anderson Mesa Station near Flagstaff, Arizona, and named after Gregory Jarvis, who died in the Space Shuttle Challenger disaster.[2][3]

    Orbit and classification

    Jarvis is a member of the Hungaria family, which form the innermost dense concentration of asteroids in the Solar System. It orbits the Sun at a distance of 1.7–2.0 AU once every 2 years and 6 months (929 days). Its orbit has an eccentricity of 0.08 and an inclination of 22° with respect to the ecliptic.[1] A first precovery was taken at the Siding Spring Observatory in 1980, extending the body's observation arc by more than one year prior to its official discovery at Anderson Mesa.[3]

    Physical characteristics

    Slow rotator

    In July 2007, a rotational lightcurve of Jarvis was obtained from photometric observations by astronomer Brian Warner at his Palmer Divide Station, Colorado, in collaboration with Robert Stephens, Alan Harris and Petr Pravec. The re-examined lightcurve analysis gave a rotation period of 202 hours with a brightness amplitude of 0.50 in magnitude, superseding the original period solution of 40.8 hours (U=2+/2).[12][lower-alpha 1]

    Due to an improved long-term calibration of the obtained photometric data points, a much longer period of 202 hours has been derived for Jarvis, which is now among the Top 300 slowest rotators known to exist, as most minor planets have spin rates between 2.2 and 24 hours only.[12]

    The observations also suggest that Jarvis might be a tumbling asteroid in a non-principal axis rotation, which are typically slow rotators (T0).[4]

    Diameter and albedo

    According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Jarvis measures between 9.72 and 12.49 kilometers in diameter, and its surface has an albedo between 0.030 and 0.074.[5][6][7][8][9][10] The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0622 and a diameter of 9.70 kilometers based on an absolute magnitude of 13.7.[4]

    While most members of the Hungaria family are E-type asteroids with extremely bright surfaces and albedos in the order of 0.30, Jarvis has an unusually low albedo, typically seen for carbonaceous asteroids.

    Naming

    This minor planet was named in memory of Gregory Jarvis (1944–1986), American astronaut and payload specialist, who died in the Space Shuttle Challenger disaster on 28 January 1986.[2] The asteroids 3350 Scobee, 3351 Smith, 3352 McAuliffe, 3354 McNair, 3355 Onizuka, and 3356 Resnik commemorate the other crew members. The approved naming citation was published by the Minor Planet Center on 26 March 1986 (M.P.C. 10550).[14]

    Notes
    1. Warner (2007), lightcurve plot of (3353) Jarvis with a rotation period of 202±0.5 hours with a brightness amplitude of 0.5 magnitude. Quality code of 2+.

    References
    1. "JPL Small-Body Database Browser: 3353 Jarvis (1981 YC)" (2016-11-24 last obs.). Jet Propulsion Laboratory. Retrieved 17 June 2017.
    2. Schmadel, Lutz D. (2007). "(3353) Jarvis". Dictionary of Minor Planet Names – (3353) Jarvis. Springer Berlin Heidelberg. p. 279. doi:10.1007/978-3-540-29925-7_3354. ISBN 978-3-540-00238-3.
    3. "3353 Jarvis (1981 YC)". Minor Planet Center. Retrieved 18 March 2017.
    4. "LCDB Data for (3353) Jarvis". Asteroid Lightcurve Database (LCDB). Retrieved 18 March 2017.
    5. Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. 12: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T. Retrieved 22 October 2019.
    6. Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Dailey, J.; et al. (November 2011). "Main Belt Asteroids with WISE/NEOWISE. I. Preliminary Albedos and Diameters". The Astrophysical Journal. 741 (2): 20. arXiv:1109.4096. Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68. Retrieved 18 March 2017.{{cite journal}}: CS1 maint: multiple names: authors list (link)
    7. Nugent, C. R.; Mainzer, A.; Bauer, J.; Cutri, R. M.; Kramer, E. A.; Grav, T.; et al. (September 2016). "NEOWISE Reactivation Mission Year Two: Asteroid Diameters and Albedos". The Astronomical Journal. 152 (3): 12. arXiv:1606.08923. Bibcode:2016AJ....152...63N. doi:10.3847/0004-6256/152/3/63. Retrieved 18 March 2017.
    8. Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90.
    9. Nugent, C. R.; Mainzer, A.; Masiero, J.; Bauer, J.; Cutri, R. M.; Grav, T.; et al. (December 2015). "NEOWISE Reactivation Mission Year One: Preliminary Asteroid Diameters and Albedos". The Astrophysical Journal. 814 (2): 13. arXiv:1509.02522. Bibcode:2015ApJ...814..117N. doi:10.1088/0004-637X/814/2/117. Retrieved 18 March 2017.
    10. Usui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi; et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey". Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. (online, AcuA catalog p. 153)
    11. Warner, Brian D. (March 2007). "Asteroid Lightcurve Analysis at the Palmer Divide Observatory - June-September 2006". The Minor Planet Bulletin. 34 (1): 8–10. Bibcode:2007MPBu...34....8W. ISSN 1052-8091. Retrieved 18 March 2017.
    12. Warner, Brian D.; Stephens, Robert, D.; Harris, Alan W.; Pravec, Petr (October 2009). "A Re-examination of the Lightcurves for Seven Hungaria Asteroids". The Minor Planet Bulletin. 36 (4): 176–179. Bibcode:2009MPBu...36..176W. ISSN 1052-8091. Retrieved 18 March 2017.{{cite journal}}: CS1 maint: multiple names: authors list (link)
    13. 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 18 March 2017.
    14. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 18 March 2017.

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