1332 Marconia

1332 Marconia, provisional designation 1934 AA, is a dark asteroid and the parent body of the Marconia family located in the outer regions of the asteroid belt. It measures approximately 46 kilometers (29 miles) in diameter. The asteroid was discovered on 9 January 1934, by Italian astronomer Luigi Volta at the Observatory of Turin in Pino Torinese, northern Italy.[1] It was named for Italian electrical engineer Guglielmo Marconi.[2] The uncommon L-type asteroid has a rotation period of 19.2 hours.[4]

1332 Marconia
Modelled shape of Marconia from its lightcurve
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 arc112.02 yr (40,916 d)
Aphelion3.4664 AU
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
Mean diameter
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]

    Orbit and classification

    Marconia is the parent body of the Marconia family (636),[5] a tiny asteroid family of less than 50 known members.[14] It orbits the Sun in the outer 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 an eccentricity of 0.13 and an inclination of 2° with respect to the ecliptic.[3]

    The asteroid was first observed in October 1905, as A905 UD at Heidelberg Observatory, where the body's observation arc begins as A924 EH in March 1924, almost 10 years prior to its official discovery observation at Pino Torinese.[1]

    Physical characteristics

    Marconia has been characterized as an L-type asteroid in the Bus–DeMeo taxonomic system, while in the SMASS classification, it is an Ld-subtype that transitions between the L-type and D-type asteroids.[3][13] The overall spectral type for members of the Marconia family is that of a carbonaceous C-type and X-type.[14]:23

    Rotation period and poles

    In September 2012, a first rotational lightcurve of Marconia was obtained from photometric observations by Robert Stephens at his Santana Observatory (646) in California. Lightcurve analysis gave a well-defined rotation period of 19.16 hours with a brightness variation of 0.30 magnitude (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 a spin axes of (37.0°, 31.0°) and (220.0°, 31.0°) in ecliptic 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

    According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Marconia measures between 44.93 and 52.009 kilometers in diameter and its surface has an albedo between 0.04 and 0.063.[6][7][8][9][10]

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

    Naming

    This minor planet was named after Guglielmo Marconi (1874–1937), an Italian electrical engineer, pioneer and inventor of radio. In 1909, he received the Nobel Prize in Physics together with Karl Ferdinand Braun (also see List of Nobel laureates in Physics § Laureates). The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 121). The lunar crater Marconi was also named in his honor.[2]

    References
    1. "1332 Marconia (1934 AA)". Minor Planet Center. Retrieved 15 March 2018.
    2. Schmadel, Lutz D. (2007). "(1332) Marconia". Dictionary of Minor Planet Names – (1332) Marconia. Springer Berlin Heidelberg. pp. 108–109. doi:10.1007/978-3-540-29925-7_1333. ISBN 978-3-540-00238-3.
    3. "JPL Small-Body Database Browser: 1332 Marconia (1934 AA)" (2017-11-02 last obs.). Jet Propulsion Laboratory. Retrieved 15 March 2018.
    4. "LCDB Data for (1332) Marconia". Asteroid Lightcurve Database (LCDB). Retrieved 15 March 2018.
    5. "Asteroid 1332 Marconia – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 26 October 2019.
    6. 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. Retrieved 15 March 2018.
    7. Nugent, 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. Retrieved 15 March 2018.
    8. 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.
    9. 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 17 October 2019. (online, AcuA catalog p. 153)
    10. 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.
    11. Stephens, 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. Retrieved 15 March 2018.
    12. 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 15 March 2018.
    13. Devogèle, 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. 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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