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458 Hercynia
Discovery
Discovered by	M. F. Wolf; A. Schwassmann
Discovery site	Heidelberg Obs.
Discovery date	21 September 1900
Designations
MPC designation	(458) Hercynia
Pronunciation	/hərˈsɪniə/
Named after	Hercynian Forest ; (ancient European forest)
Alternative designations	1900 FK · 1947 XB; 2016 FW5 · A902 CA; A915 PD
Minor planet category	main-belt · (outer) ; background
Orbital characteristics
	Epoch 4 September 2017 (JD 2458000.5)
	Uncertainty parameter 0
Observation arc	116.79 yr (42,656 days)
Aphelion	3.7176 AU
Perihelion	2.2784 AU
Semi-major axis	2.9980 AU
Eccentricity	0.2400
Orbital period (sidereal)	5.19 yr (1,896 days)
Mean anomaly	178.41°
Mean motion	0° 11m 23.64s / day
Inclination	12.640°
Longitude of ascending node	134.26°
Argument of perihelion	276.79°
Physical characteristics
Dimensions	33.70±7.94 km; 36.10±0.85 km; 36.698±0.408 km; 38.57 km (derived); 38.75±1.0 km; 41.410±1.172 km; 42.27±0.92 km
Synodic rotation period	15.33±0.04 h; 16 h; 21.806±0.006 h; 22.3 h; 22.41±0.01 h
Geometric albedo	0.1435±0.0205; 0.145±0.007; 0.1654±0.009; 0.19±0.10; 0.191±0.034
Spectral type	Tholen = S ; SMASS = L · L · M ; B–V = 0.885; U–B = 0.471
Absolute magnitude (H)	9.63 · 9.64 · 9.64±0.24 · 9.72

458 Hercynia, provisional designation 1900 FK, is a background asteroid from the outer regions of the asteroid belt, approximately 38 kilometers in diameter. It was discovered on 21 September 1900, by astronomers Max Wolf and Arnold Schwassmann at the Heidelberg-Königstuhl State Observatory in southwest Germany.^[19] The asteroid was named for the ancient Hercynian Forest, known to the Romans as "Hercynia silva".^[4]

Orbit and classification

Hercynia is a non-family asteroid of the main belt's background population.^[6] It orbits the Sun in the outer asteroid belt at a distance of 2.3–3.7 AU once every 5 years and 2 months (1,896 days; semi-major axis of 3.00 AU). Its orbit has an eccentricity of 0.24 and an inclination of 13° with respect to the ecliptic.^[1] The body's observation arc begins two days after to its official discovery observation at Heidelberg.^[19]

Physical characteristics

In the Tholen classification, Hercynia is a common S-type, while in the SMASS classification it is a rare L-type asteroid.^[1] Polarimetric observations also determined an L-type.^[17] Alternatively, the Wide-field Infrared Survey Explorer (WISE) characterized Hercynia as a metallic M-type asteroid.^[11]

Rotation period

Several rotational lightcurves of Hercynia have been obtained from photometric observations since 1985.^[5] Lightcurve analysis gave a consolidated, slightly longer-than average rotation period of 21.806 hours with a brightness amplitude between 0.10 and 0.36 magnitude (U=2/2-/3/2/2).^[13]^[14]^[15]^[16]

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 WISE telescope, Hercynia measures between 33.70 and 42.27 kilometers in diameter and its surface has an albedo between 0.1435 and 0.191.^[7]^[8]^[9]^[10]^[11]^[12]

The Collaborative Asteroid Lightcurve Link adopts an albedo of 0.1654 from IRAS, and derives a diameter of 38.57 kilometers based on an absolute magnitude of 9.64.^[5]^[10]

Naming

This minor planet was named after the ancient Central European Hercynian Forest, known as "Hercynia silva" to the Romans. The mountainous and dense forest stretched from the upper part of the Rhine to the Carpathian Mountains in southeastern Europe. According to Caesar, it required a nine-day journey to cross the forest. (The Black Forest located to the south of the discovering observatory is a remnant of the western part of this forest). The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 50).^[4]

References

^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ "JPL Small-Body Database Browser: 458 Hercynia (1900 FK)" (2017-07-05 last obs.). Jet Propulsion Laboratory. Retrieved 7 November 2017.
^ "hercynian". Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
^ Noah Webster (1884) A Practical Dictionary of the English Language
^ ^a ^b ^c Schmadel, Lutz D. (2007). "(458) Hercynia". Dictionary of Minor Planet Names – (458) Hercynia. Springer Berlin Heidelberg. p. 52. doi:10.1007/978-3-540-29925-7_459. ISBN 978-3-540-00238-3.
^ ^a ^b ^c ^d ^e "LCDB Data for (458) Hercynia". Asteroid Lightcurve Database (LCDB). Retrieved 7 November 2017.
^ ^a ^b "Asteroid 458 Hercynia – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 24 October 2019.
^ ^a ^b ^c ^d 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.
^ ^a ^b ^c ^d Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; et al. (November 2012). "Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. S2CID 46350317.
^ ^a ^b 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. S2CID 119293330.
^ ^a ^b ^c ^d ^e 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.
^ ^a ^b ^c ^d ^e ^f 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. S2CID 35447010.
^ ^a ^b ^c ^d 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)
^ ^a ^b Hawkins, Scot; Ditteon, Richard (March 2008). "Asteroid Lightcurve Analysis at the Oakley Observatory - May 2007". The Minor Planet Bulletin. 35 (1): 1–4. Bibcode:2008MPBu...35....1H. ISSN 1052-8091.
^ ^a ^b ^c Behrend, Raoul. "Asteroids and comets rotation curves – (458) Hercynia". Geneva Observatory. Retrieved 7 November 2017.
^ ^a ^b Aznar Macias, Amadeo; Carreno Garcerain, Alfonso; Arce Masego, Enrique; Brines Rodriguez, Pedro; Lozano de Haro, Juan; Fornas Silva, Alvaro; et al. (July 2016). "Twenty-one Asteroid Lightcurves at Group Observadores de Asteroides (OBAS): Late 2015 to Early 2016". The Minor Planet Bulletin. 43 (3): 257–263. Bibcode:2016MPBu...43..257A. ISSN 1052-8091.
^ ^a ^b ^c Binzel, R. P. (October 1987). "A photoelectric survey of 130 asteroids". Icarus. 72 (1): 135–208. Bibcode:1987Icar...72..135B. doi:10.1016/0019-1035(87)90125-4. ISSN 0019-1035.
^ ^a ^b Belskaya, I. N.; Fornasier, S.; Tozzi, G. P.; Gil-Hutton, R.; Cellino, A.; Antonyuk, K.; et al. (March 2017). "Refining the asteroid taxonomy by polarimetric observations". Icarus. 284: 30–42. Bibcode:2017Icar..284...30B. doi:10.1016/j.icarus.2016.11.003. hdl:11336/63617.
^ 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. S2CID 53493339.
^ ^a ^b "458 Hercynia (1900 FK)". Minor Planet Center. Retrieved 7 November 2017.