827 Wolfiana

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827 Wolfiana
Discovery [1]
Discovered by J. Palisa
Discovery site Vienna Obs.
Discovery date29 August 1916
Designations
(827) Wolfiana
Named after
 Max Wolf [2]
(German astronomer)
1916 ZW ·1928 DK
1940 RA
main-belt  ·(inner)
Flora [3] [4]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 100.68 yr (36,773 d)
Aphelion 2.6314 AU
Perihelion 1.9172 AU
2.2743 AU
Eccentricity 0.1570
3.43 yr (1,253 days)
145.31°
0° 17m 14.64s / day
Inclination 3.4231°
172.92°
195.31°
Physical characteristics
Dimensions 6.51 km (calculated) [3]
8.488±0.165 km [5]
8.976±0.020 km [6]
4.0±0.3 h [7]
4.0654±0.0001 h [8]
0.1153±0.0299 [6]
0.129±0.020 [5]
0.24 (assumed) [3]
S (assumed) [3]
13.1 [1] [3]  ·13.2 [6]

    827 Wolfiana, provisional designation 1916 ZW, is a Florian asteroid from the inner regions of the asteroid belt, approximately 8 kilometers in diameter. It was discovered at Vienna Observatory on 29 August 1916, by Austrian astronomer Johann Palisa, who named it after German astronomer Max Wolf. [2] [9] The assumed stony asteroid has a rotation period of 4.0654 hours.

    Contents

    Orbit and classification

    Wolfiana is a member of the Flora family ( 402 ), [3] [4] a giant asteroid family and the largest family of stony asteroids in the main belt. [10] : 23  It orbits the Sun in the inner asteroid belt at a distance of 1.9–2.6  AU once every 3 years and 5 months (1,253 days; semi-major axis of 2.27 AU). Its orbit has an eccentricity of 0.16 and an inclination of 3° with respect to the ecliptic. [1] The body's observation arc begins with its official discovery observation at Vienna. [9]

    Physical characteristics

    Wolfiana is an assumed stony S-type asteroid, [3] which agrees with the overall spectral type for Florian asteroids. [10] : 23 

    Rotation period

    In September 2012, a rotational lightcurve of Wolfiana was obtained from photometric observations by American astronomers Luis Martinez, Arizona, and Frederick Pilcher at Organ Mesa Observatory ( G50 ), New Mexico. Lightcurve analysis gave a well-defined rotation period of 4.0654 hours with a brightness amplitude of 0.20 magnitude ( U=3 ), [8] refining a period of 4.0 hours previously measured in November 2009 ( U=2 ). [7]

    Diameter and albedo

    According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Wolfiana measures 8.488 and 8.976 kilometers in diameter and its surface has an albedo of 0.129 and 0.1153, respectively. [5] [6]

    The Collaborative Asteroid Lightcurve Link assumes a standard albedo of 0.24 – derived from 8 Flora, the parent body of the Flora family – and calculates a diameter of 6.51 kilometers based on an absolute magnitude of 13.1. [3]

    Naming

    This minor planet was named by the discoverer in 1920 ( AN 211;441 ) after German astronomer, colleague and friend, Max Wolf (1863–1932), a professor of astronomy at Heidelberg University and founder and director of the Heidelberg-Königstuhl State Observatory, who discovered several novae, comets and 248 minor planets. [2]

    The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 ( H 82 ). Asteroid 1217 Maximiliana and the lunar crater Wolf were also named in his honor. [2]

    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 827 Wolfiana (1916 ZW)" (2017-05-04 last obs.). Jet Propulsion Laboratory . Retrieved 12 January 2018.
    2. 1 2 3 4 Schmadel, Lutz D. (2007). "(827) Wolfiana". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 76. doi:10.1007/978-3-540-29925-7_828. ISBN   978-3-540-00238-3.
    3. 1 2 3 4 5 6 7 8 "LCDB Data for (827) Wolfiana". Asteroid Lightcurve Database (LCDB). Retrieved 12 January 2018.
    4. 1 2 "Asteroid 827 Wolfiana – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 24 October 2019.
    5. 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.
    6. 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". The Astrophysical Journal. 741 (2): 25. arXiv: 1109.6407 . Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90.
    7. 1 2 Kryszczynska, A.; Colas, F.; Polinska, M.; Hirsch, R.; Ivanova, V.; Apostolovska, G.; et al. (October 2012). "Do Slivan states exist in the Flora family?. I. Photometric survey of the Flora region". Astronomy and Astrophysics. 546: 51. Bibcode:2012A&A...546A..72K. doi: 10.1051/0004-6361/201219199 .
    8. 1 2 Pilcher, Frederick; Martinez, Luis (January 2013). "Rotation Period Determination for 827 Wolfiana". The Minor Planet Bulletin. 40 (1): 21. Bibcode:2013MPBu...40Q..21P. ISSN   1052-8091.
    9. 1 2 "827 Wolfiana (1916 ZW)". Minor Planet Center . Retrieved 12 January 2018.
    10. 1 2 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.
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