1291 Phryne

1291 Phryne
Lightcurve-based 3D-model of Phryne
Discovery [1]
Discovered by E. Delporte
Discovery site Uccle Obs.
Discovery date 15 September 1933
Designations
MPC designation (1291) Phryne
Named after
 Phryne [2]
(ancient Greek courtesan)
1933 RA · 1931 DX
1932 KJ · 1953 JS
A907 TA · A922 NA
main-belt · (outer)
Eos [3][4]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 109.08 yr (39,843 days)
Aphelion 3.2977 AU
Perihelion 2.7292 AU
3.0134 AU
Eccentricity 0.0943
5.23 yr (1,911 days)
29.198°
0° 11m 18.24s / day
Inclination 9.1061°
215.38°
118.83°
Physical characteristics
Dimensions 24.954±0.275 km[5]
26.52 km (derived)[3]
26.78±2.2 km[6]
27.418±0.149 km[7]
31.13±0.52 km[8]
5.55 h[9]
5.58410±0.00007 h[10]
5.584139±0.000001 h[11]
5.58414±0.00005 h[12]
0.127±0.019[7]
0.1355 (derived)[3]
0.141±0.005[8]
0.1537±0.0198[5]
0.1818±0.033[6]
S [3]
B–V = 0.835 [1]
U–B = 0.395 [1]
10.3[1] · 10.33[6][8] · 10.67[3][5][9]

    1291 Phryne, provisional designation 1933 RA, is an Eoan asteroid from the outer regions of the asteroid belt, approximately 27 kilometers in diameter. It was discovered on 15 September 1933, by Belgian astronomer Eugène Delporte at the Royal Observatory of Belgium in Uccle.[13] The asteroid was named after the ancient Greek courtesan Phryne.

    Orbit and classification

    Phryne is a member the Eos family (606),[4] the largest asteroid family in the outer main belt consisting of nearly 10,000 asteroids.[14]:23 It orbits the Sun at a distance of 2.7–3.3 AU once every 5 years and 3 months (1,911 days). Its orbit has an eccentricity of 0.09 and an inclination of 9° with respect to the ecliptic.[1] The body's observation arc begins with its first identification as A907 TA at Heidelberg Observatory in October 1907.[13]

    Physical characteristics

    Phryne is an assumed stony S-type asteroid,[3] while the Eon family's overall spectral type is that of a K-type.[14]:23

    Rotation period

    In May 1984, a rotational lightcurve of Phryne was obtained by astronomer Richard Binzel. Lightcurve analysis gave a well-defined rotation period of 5.55 hours with a brightness variation of 0.86 magnitude (U=3).[9] In August 2006, from photometric observations by French amateur astronomer Pierre Antonini gave a period of 5.58410 hours and an amplitude of 0.38 magnitude (U=3)[10]

    Poles

    In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a period 5.58414 hours, as well as two spin axis of (106.0°, 35.0°) and (277.0°, 59.0°) in ecliptic coordinates (λ, β).[12] In 2017, a new study of the same international collaboration about the rotational states of Eoan asteroids gave a revised shape model with a period of 5.584139 hours and two spin axis of (109.0°, 33.0°) and (281.0°, 56.0°).[11]

    Diameter and albedo

    According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Phryne measures between 24.954 and 31.13 kilometers in diameter and its surface has an albedo between 0.127 and 0.1818.[5][6][7][8]

    The Collaborative Asteroid Lightcurve Link derives an albedo of 0.1355 and a diameter of 26.52 kilometers based on an absolute magnitude of 10.67.[3]

    Naming

    This minor planet was named after Phryne, the beautiful ancient Greek courtesan (hetaira) of the 4th century B.C. Supposedly, she was the model for the statue Aphrodite of Knidos by ancient Greek sculptor Praxiteles (see asteroid 5983), who was also her lover. It was the first nude statue of a woman from ancient Greece. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 118).[2]

    References

    1. 1 2 3 4 5 6 "JPL Small-Body Database Browser: 1291 Phryne (1933 RA)" (2016-11-03 last obs.). Jet Propulsion Laboratory. Retrieved 14 September 2017.
    2. 1 2 Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1291) Phryne. Springer Berlin Heidelberg. p. 106. ISBN 978-3-540-00238-3. Retrieved 14 September 2017.
    3. 1 2 3 4 5 6 7 "LCDB Data for (1291) Phryne". Asteroid Lightcurve Database (LCDB). Retrieved 14 September 2017.
    4. 1 2 "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Retrieved 14 September 2017.
    5. 1 2 3 4 Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results" (PDF). The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 14 September 2017.
    6. 1 2 3 4 Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. Bibcode:2004PDSS...12.....T. Retrieved 14 September 2017.
    7. 1 2 3 Masiero, Joseph R.; Grav, T.; Mainzer, A. K.; Nugent, C. R.; Bauer, J. M.; Stevenson, R.; et al. (August 2014). "Main-belt Asteroids with WISE/NEOWISE: Near-infrared Albedos". The Astrophysical Journal. 791 (2): 11. arXiv:1406.6645. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. Retrieved 14 September 2017.
    8. 1 2 3 4 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. Retrieved 14 September 2017.
    9. 1 2 3 Binzel, R. P. (October 1987). "A photoelectric survey of 130 asteroids". Icarus: 135–208. Bibcode:1987Icar...72..135B. doi:10.1016/0019-1035(87)90125-4. ISSN 0019-1035. Retrieved 14 September 2017.
    10. 1 2 Behrend, Raoul. "Asteroids and comets rotation curves – (1291) Phryne". Geneva Observatory. Retrieved 14 September 2017.
    11. 1 2 Hanus, J.; Delbo', M.; Alí-Lagoa, V.; Bolin, B.; Jedicke, R.; Durech, J.; et al. (January 2018). "Spin states of asteroids in the Eos collisional family" (PDF). Icarus. 299: 84–96. arXiv:1707.05507. Bibcode:2018Icar..299...84H. doi:10.1016/j.icarus.2017.07.007. Retrieved 14 September 2017.
    12. 1 2 Hanus, J.; Durech, J.; Broz, M.; Warner, B. D.; Pilcher, F.; Stephens, R.; et al. (June 2011). "A study of asteroid pole-latitude distribution based on an extended set of shape models derived by the lightcurve inversion method". Astronomy & Astrophysics. 530: 16. arXiv:1104.4114. Bibcode:2011A&A...530A.134H. doi:10.1051/0004-6361/201116738. Retrieved 14 September 2017.
    13. 1 2 "1291 Phryne (1933 RA)". Minor Planet Center. Retrieved 14 September 2017.
    14. 1 2 Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families" (PDF). Asteroids IV: 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. Retrieved 14 September 2017.
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