1374 Isora

1374 Isora, provisional designation 1935 UA, is a stony asteroid and eccentric Mars-crosser from the innermost regions of the asteroid belt, approximately 5 kilometers in diameter. It was discovered on 21 October 1935, by Belgian astronomer Eugène Delporte at Uccle Observatory in Belgium.[3]

1374 Isora
Discovery [1]
Discovered byE. Delporte
Discovery siteUccle Obs.
Discovery date21 October 1935
Designations
(1374) Isora
Named after
Constructed female name
("Rosi" spelled backwards)[2]
1935 UA
Mars-crosser [1][3][4]
Orbital characteristics [1]
Epoch 16 February 2017 (JD 2457800.5)
Uncertainty parameter 0
Observation arc81.05 yr (29,604 days)
Aphelion2.8775 AU
Perihelion1.6230 AU
2.2502 AU
Eccentricity0.2788
3.38 yr (1,233 days)
44.987°
0° 17m 31.2s / day
Inclination5.2943°
302.56°
60.988°
Earth MOID0.6290 AU
Physical characteristics
Dimensions5.48 km (derived)[4]
8±2 h[5]
36.699±0.001 h[6]
0.20 (assumed)[4]
SMASS = Sq [1] · S [4][7][8]
13.00[8] · 13.3[1] · 13.32±0.32[7] · 13.67±0.15[4][5]

    Orbit and classification

    In the SMASS taxonomy, Isora is classified as a Sq-type, an intermediary between the abundant S and rather rare Q-type asteroids. It orbits the Sun at a distance of 1.6–2.9 AU once every 3 years and 5 months (1,233 days). Its orbit has an eccentricity of 0.28 and an inclination of 5° with respect to the ecliptic.[1] Isora's observation arc begins with its official discovery observation at Uccle, as no precoveries were taken and no prior identifications were made.[3]

    Physical characteristics

    In January 2014, a rotational light-curve of Isora was obtained by American astronomer Robert D. Stephens at the Center for Solar System Studies (CS3) in California. Light-curve analysis gave a longer than average rotation period of 36.699 hours with a brightness variation of 0.12 magnitude (U=2+). However, a second period solution of 18.35 hours is also possible.[6] The result supersedes photometric observations taken by Wiesław Z. Wiśniewski in 1989, which rendered a fragmentary light-curve with a period of 8 hours (U=1).[5]

    The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and derives a diameter of 5.48 kilometers using an absolute magnitude of 13.67.[4]

    Naming

    Isora is the backwards spelled feminine name "Rosi" with an appended "a".[2] Naming was proposed by Gustav Stracke (1887–1943) – astronomer at the German Astronomisches Rechen-Institut, and after whom the minor planet 1019 Strackea is named – and first cited by Paul Herget in his The Names of the Minor Planets in 1955 (H 125).[2]

    References
    1. "JPL Small-Body Database Browser: 1374 Isora (1935 UA)" (2016-11-08 last obs.). Jet Propulsion Laboratory. Retrieved 11 January 2017.
    2. Schmadel, Lutz D. (2007). "(1374) Isora". Dictionary of Minor Planet Names – (1374) Isora. Springer Berlin Heidelberg. p. 111. doi:10.1007/978-3-540-29925-7_1375. ISBN 978-3-540-00238-3.
    3. "1374 Isora (1935 UA)". Minor Planet Center. Retrieved 11 January 2017.
    4. "LCDB Data for (1374) Isora". Asteroid Lightcurve Database (LCDB). Retrieved 11 January 2017.
    5. Wisniewski, W. Z.; Michalowski, T. M.; Harris, A. W.; McMillan, R. S. (March 1995). "Photoelectric Observations of 125 Asteroids". Abstracts of the Lunar and Planetary Science Conference. 26: 1511. Bibcode:1995LPI....26.1511W. Retrieved 11 January 2017.
    6. Stephens, Robert D. (July 2014). "Asteroids Observed from CS3: 2014 January - March". The Minor Planet Bulletin. 41 (3): 171–175. Bibcode:2014MPBu...41..171S. ISSN 1052-8091. Retrieved 11 January 2017.
    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 11 January 2017.
    8. Carry, B.; Solano, E.; Eggl, S.; DeMeo, F. E. (April 2016). "Spectral properties of near-Earth and Mars-crossing asteroids using Sloan photometry". Icarus. 268: 340–354. arXiv:1601.02087. Bibcode:2016Icar..268..340C. doi:10.1016/j.icarus.2015.12.047. Retrieved 11 January 2017.

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