1077 Campanula

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1077 Campanula
001077-asteroid shape model (1077) Campanula.png
Shape model of Campanula from its lightcurve
Discovery [1]
Discovered by K. Reinmuth
Discovery site Heidelberg Obs.
Discovery date6 October 1926
Designations
(1077) Campanula
Pronunciation /kæmˈpænjʊlə/ [2]
Named after
 Campanula (bellflower) [3]
1926 TK ·1957 AJ
1972 CB
main-belt  ·(inner)
Erigone [4]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 90.56 yr (33,077 days)
Aphelion 2.8655 AU
Perihelion 1.9220 AU
2.3938 AU
Eccentricity 0.1971
3.70 yr (1,353 days)
218.36°
0° 15m 57.96s / day
Inclination 5.3941°
346.20°
13.591°
Physical characteristics
Mean diameter
7.55±1.72 km [5]
9±2 km [6]
9.709±0.278 km [7] [8]
3.847±0.002  h [lower-alpha 1]
3.850±0.001 h [9] [10]
3.850486±0.000001 h [11]
3.85085±0.00005 h [6]
3.852±0.002 h [12]
  • (178.0°, 76.0°) (λ1/β1) [13]
  • (313.0°, 59.0°) (λ2/β2) [13]
0.225±0.017 [7]
0.2253±0.0169 [8]
0.33±0.12 [5]
S [4] V–R = 0.400±0.070 [6]
12.3 [14] [1]

    1077 Campanula, provisional designation 1926 TK, is a presumed Erigonian asteroid, approximately 9 kilometers (5.6 miles) in diameter, located in the inner region of the asteroid belt. It was discovered on 6 October 1926, by German astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany. [14] The asteroid was named after the bellflower Campanula. [3]

    Contents

    Classification and orbit

    Campanula is considered to be a member of the Erigone family ( 406 ), [4] which is named after 163 Erigone, while other sources classify it as a background asteroid, not associated to any known asteroid family. [15] [13] It orbits the Sun in the inner main-belt at a distance of 1.9–2.9  AU once every 3 years and 8 months (1,353 days). Its orbit has an eccentricity of 0.20 and an inclination of 5° with respect to the ecliptic. [1] The body's observation arc begins at Heidelberg, 2 months after its official discovery observation. [14]

    Naming

    This minor planet was named for the bellflower Campanula. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 ( H 102 ). [3]

    Reinmuth's flowers

    Due to his many discoveries, Karl Reinmuth submitted a large list of 66 newly named asteroids in the early 1930s. The list covered his discoveries with numbers between (1009) and (1200). This list also contained a sequence of 28 asteroids, starting with 1054 Forsytia, that were all named after plants, in particular flowering plants (also see list of minor planets named after animals and plants). [16]

    Physical characteristics

    Campanula is an assumed stony S-type asteroid, [4] which is not in line with the darker C- and X-types seen among the Erigonian asteroids. [17] : 23 

    Rotation period and poles

    Several rotational lightcurves of Campanula were obtained from photometric observations. Lightcurve analysis gave a rotation period of 3.847 to 3.852 hours with a brightness variation of 0.24 to 0.40 magnitude ( U=3-/3/3/3 ). [6] [9] [10] [12] [lower-alpha 1] A 2016-published lightcurve, using modeled photometric data from the Lowell Photometric Database (LPD), gave a concurring period of 3.850486 hours ( U=n.a. ), as well as two spin axis of (178.0°, 76.0°) and (313.0°, 59.0°) in ecliptic coordinates (λ, β). [11]

    Diameter and albedo

    According to observations taken at the Balzaretto Observatory ( A81 ) and the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Campanula measures between 7.55 and 9.709 kilometers in diameter and its surface has an albedo between 0.225 and 0.33. [5] [6] [7] [8] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 9.40 kilometers based on an absolute magnitude of 12.50. [4]

    See also

    Notes

    1. 1 2 Higgins (2011) web: rotation period 3.847±0.002 hours with a brightness amplitude of 0.40±0.02 mag. Quality code is 3–. Summary figures for (1077) Campanula at the LCDB.

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    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 1077 Campanula (1926 TK)" (2017-04-28 last obs.). Jet Propulsion Laboratory . Retrieved 30 August 2017.
    2. ↑ "campanula" . Oxford English Dictionary (Online ed.). Oxford University Press.(Subscription or participating institution membership required.)
    3. 1 2 3 Schmadel, Lutz D. (2007). "(1077) Campanula". Dictionary of Minor Planet Names . Springer Berlin Heidelberg. p.  92. doi:10.1007/978-3-540-29925-7_1078. ISBN   978-3-540-00238-3.
    4. 1 2 3 4 5 "LCDB Data for (1077) Campanula". Asteroid Lightcurve Database (LCDB). Retrieved 30 August 2017.
    5. 1 2 3 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 .
    6. 1 2 3 4 5 Franco, Lorenzo (April 2012). "Lightcurve Photometry and H-G Parameters for 1077 Campanula". The Minor Planet Bulletin. 39 (2): 67–69. Bibcode:2012MPBu...39...67F. ISSN   1052-8091 . Retrieved 30 August 2017.
    7. 1 2 3 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 30 August 2017.
    8. 1 2 3 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. 1 2 Aymami, Josep Maria (January 2012). "CCD Photometry and Lightcurve Analysis of Main Belt Asteroids 1077 Campanula and 1151 Ithaka from Observatori Carmelita". The Minor Planet Bulletin. 39 (1): 29. Bibcode:2012MPBu...39...29A. ISSN   1052-8091 . Retrieved 30 August 2017.
    10. 1 2 Klinglesmith, Daniel A. III; Hendrickx, Sebastian; Madden, Karl; Montgomery, Samuel (July 2016). "Asteroid Lightcurves from Estcorn Observatory". The Minor Planet Bulletin. 43 (3): 234–239. Bibcode:2016MPBu...43..234K. ISSN   1052-8091 . Retrieved 30 August 2017.
    11. 1 2 Durech, J.; Hanus, J.; Oszkiewicz, D.; Vanco, R. (March 2016). "Asteroid models from the Lowell photometric database". Astronomy and Astrophysics. 587: 6. arXiv: 1601.02909 . Bibcode:2016A&A...587A..48D. doi:10.1051/0004-6361/201527573 . Retrieved 30 August 2017.
    12. 1 2 Stephens, Robert D. (January 2012). "Asteroids Observed from GMARS and Santana Observatories: 2011 July - September". The Minor Planet Bulletin. 39 (1): 11–12. Bibcode:2012MPBu...39...11S. ISSN   1052-8091 . Retrieved 30 August 2017.
    13. 1 2 3 "Asteroid 1077 Campanula – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 26 October 2019.
    14. 1 2 3 "1077 Campanula (1926 TK)". Minor Planet Center. Retrieved 30 August 2017.
    15. ↑ "AstDyS-2 data for (1077) Campanula". AstDyS – Asteroids Dynamic Site. Retrieved 30 August 2017.
    16. ↑ Schmadel, Lutz D. (2007). "(1054) Forsytia". Dictionary of Minor Planet Names . Springer Berlin Heidelberg. p.  90. doi:10.1007/978-3-540-29925-7_1055. ISBN   978-3-540-00238-3.
    17. ↑ 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   978-0-8165-3213-1.
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