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1332 Marconia

From Wikipedia, the free encyclopedia
Main-belt asteroid

1332 Marconia
Modelled shape ofMarconia from itslightcurve
Discovery[1]
Discovered byL. Volta
Discovery sitePino Torinese Obs.
Discovery date9 January 1934
Designations
(1332) Marconia
Named after
Guglielmo Marconi[2]
(Italian engineer)
1934 AA · 1930 HQ
1932 VC · 1935 FR
1948 SH · 1956 GB
A905 UD · A921 TE
A921 UD · A924 EH
main-belt[1][3] · (outer)[4]
Marconia[5]
Orbital characteristics[3]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc112.02yr (40,916 d)
Aphelion3.4664AU
Perihelion2.6587 AU
3.0626 AU
Eccentricity0.1319
5.36 yr (1,958 d)
2.3975°
0° 11m 2.04s / day
Inclination2.4568°
13.652°
348.94°
Physical characteristics
43.90 km(derived)[4]
44.93±10.33 km[6]
46.03±15.75 km[7]
46.796±0.141 km[8]
49.95±0.61 km[9]
52.009±0.600 km[10]
19.16±0.01 h[11]
19.2264±0.0001 h[12]
32.1201±0.0005 h[13]
0.04±0.02[6]
0.04±0.04[7]
0.0527(derived)[4]
0.0543±0.0105[10]
0.060±0.002[9]
0.063±0.008[8]
SMASS =Ld[3][13]
L(Bus–DeMeo)[13]
10.20[9][10] · 10.50[7]
10.6[3][4] · 10.62[6]

1332 Marconia, provisional designation1934 AA, is a darkasteroid and the parent body of theMarconia family located in the outer regions of theasteroid belt. It measures approximately 46 kilometers (29 miles) in diameter. The asteroid was discovered on 9 January 1934, by Italian astronomerLuigi Volta at theObservatory of Turin in Pino Torinese, northern Italy.[1] It was named for Italian electrical engineerGuglielmo Marconi.[2] The uncommonL-type asteroid has arotation period of 19.2 hours.[4]

Orbit and classification

[edit]

Marconia is theparent body of theMarconia family (636),[5] a tinyasteroid family of less than 50 known members.[14] It orbits the Sun in theouter asteroid belt at a distance of 2.7–3.5 AU once every 5 years and 4 months (1,958 days;semi-major axis of 3.06 AU). Its orbit has aneccentricity of 0.13 and aninclination of 2° with respect to theecliptic.[3]

The asteroid was first observed in October 1905, asA905 UD atHeidelberg Observatory, where the body'sobservation arc begins asA924 EH in March 1924, almost 10 years prior to its official discovery observation at Pino Torinese.[1]

Physical characteristics

[edit]

Marconia has been characterized as anL-type asteroid in the Bus–DeMeo taxonomic system, while in theSMASS classification, it is an Ld-subtype that transitions between the L-type andD-type asteroids.[3][13] The overallspectral type for members of the Marconia family is that of a carbonaceousC-type andX-type.[14]: 23 

Rotation period and poles

[edit]

In September 2012, a first rotationallightcurve ofMarconia was obtained fromphotometric observations byRobert Stephens at his Santana Observatory (646) in California. Lightcurve analysis gave a well-definedrotation period of 19.16 hours with a brightness variation of 0.30magnitude (U=3).[11]

A 2016-published lightcurve, using modeled photometric data from the Lowell Photometric Database, gave a concurring sidereal period of 19.2264 hours, as well as aspin axes of (37.0°, 31.0°) and (220.0°, 31.0°) inecliptic coordinates (λ, β).[12] Conversely, another lightcurve inversion study by an international collaboration gave a longer spin rate of 32.1201 hours.[13]

Diameter and albedo

[edit]

According to the surveys carried out by the JapaneseAkari satellite and theNEOWISE mission of NASA'sWide-field Infrared Survey Explorer,Marconia measures between 44.93 and 52.009 kilometers in diameter and its surface has analbedo between 0.04 and 0.063.[6][7][8][9][10]

TheCollaborative Asteroid Lightcurve Link derives an albedo of 0.0527 and a diameter of 43.90 kilometers based on anabsolute magnitude of 10.6.[4]

Naming

[edit]

Thisminor planet was named afterGuglielmo Marconi (1874–1937), an Italian electrical engineer, pioneer andinventor of radio. In 1909, he received theNobel Prize in Physics together withKarl Ferdinand Braun(also seeList of Nobel laureates in Physics § Laureates). The official naming citation was mentioned inThe Names of the Minor Planets byPaul Herget in 1955 (H 121). The lunar craterMarconi was also named in his honor.[2]

References

[edit]
  1. ^abcd"1332 Marconia (1934 AA)".Minor Planet Center. Retrieved15 March 2018.
  2. ^abcSchmadel, Lutz D. (2007). "(1332) Marconia".Dictionary of Minor Planet Names. Springer Berlin Heidelberg. pp. 108–109.doi:10.1007/978-3-540-29925-7_1333.ISBN 978-3-540-00238-3.
  3. ^abcdef"JPL Small-Body Database Browser: 1332 Marconia (1934 AA)" (2017-11-02 last obs.).Jet Propulsion Laboratory. Retrieved15 March 2018.
  4. ^abcdef"LCDB Data for (1332) Marconia". Asteroid Lightcurve Database (LCDB). Retrieved15 March 2018.
  5. ^ab"Asteroid 1332 Marconia – Nesvorny HCM Asteroid Families V3.0".Small Bodies Data Ferret. Retrieved26 October 2019.
  6. ^abcdNugent, 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.
  7. ^abcdNugent, C. R.; Mainzer, A.; Masiero, J.; Bauer, J.; Cutri, R. M.; Grav, T.; et al. (December 2015)."NEOWISE Reactivation Mission Year One: Preliminary Asteroid Diameters and Albedos".The Astrophysical Journal.814 (2): 13.arXiv:1509.02522.Bibcode:2015ApJ...814..117N.doi:10.1088/0004-637X/814/2/117. Retrieved15 March 2018.
  8. ^abcMasiero, 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.
  9. ^abcdUsui, 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)
  10. ^abcdMainzer, 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.
  11. ^abStephens, Robert D. (January 2013)."Asteroids Observed from Santana and CS3 Observatories: 2012 July - September".The Minor Planet Bulletin.40 (1):34–35.Bibcode:2013MPBu...40...34S.ISSN 1052-8091. Retrieved15 March 2018.
  12. ^abDurech, 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. Retrieved15 March 2018.
  13. ^abcdeDevogèle, M.; Tanga, P.; Bendjoya, P.; Rivet, J. P.; Surdej, J.; Hanus, J.; et al. (July 2017). "Shape and spin determination of Barbarian asteroids".Astronomy and Astrophysics.607: A119.arXiv:1707.07503.Bibcode:2017A&A...607A.119D.doi:10.1051/0004-6361/201630104.
  14. ^abNesvorný, 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.

External links

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