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3247 Di Martino

From Wikipedia, the free encyclopedia

3247 Di Martino
Shape model of Di Martino from its lightcurve
Discovery [1]
Discovered byE. Bowell
Discovery siteAnderson Mesa Stn.
Discovery date30 December 1981
Designations
(3247) Di Martino
Named after
Mario di Martino [1]
(Italian astronomer)
1981 YE · 1968 HR
1979 HO1 · A909 BL
Orbital characteristics [2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc109.09 yr (39,844 d)
Aphelion2.6824 AU
Perihelion2.0727 AU
2.3776 AU
Eccentricity0.1282
3.67 yr (1,339 d)
229.54°
0° 16m 7.68s / day
Inclination3.9342°
45.601°
146.34°
Physical characteristics
11.267±2.644 km[6]
11.74±3.06 km[7]
12.42±2.19 km[8]
13.60±5.23 km[9]
13.72 km (derived)[3]
13.75±1.0 km[10]
15.60±0.51 km[11]
5.443±0.0014 h[12]
5.4446±0.0007 h[13]
5.445 h[14]
5.44517±0.00005 h[15]
  • (53.0°, −70.0°) (λ1/β1)[15]
  • (231.0°, −75.0°) (λ2/β2)[15]
0.05±0.10[8]
0.053±0.004[11]
0.0540 (derived)[3]
0.060±0.060[9]
0.0647±0.011[10]
0.08±0.09[7]
0.0925±0.0544[6]
S (assumed)[3]
12.90[10][11]
13.00[7][9]
13.1[2][3]
13.116±0.003 (R)[12]
13.26[6]
13.51[8]

3247 Di Martino (prov. designation: 1981 YE) is a dark Nysa family asteroid from the inner regions of the asteroid belt. It was discovered on 30 December 1981, by American astronomer Edward Bowell at Lowell's Anderson Mesa Station near Flagstaff, Arizona, in the United States.[1] The asteroid has a rotation period of 5.4 hours and measures approximately 13 kilometers (8 miles) in diameter.[3] It was named for Italian astronomer Mario di Martino.[1]

Orbit and classification

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Di Martino is member of the Nysa–Polana complex (405),[4][5] one of the largest asteroid families.[16] Its low albedo (see below) it likely belongs to the Polana family within the larger Nysa–Polana complex. The asteroid orbits the Sun in the inner main-belt at a distance of 2.1–2.7 AU once every 3 years and 8 months (1,339 days; semi-major axis of 2.38 AU). Its orbit has an eccentricity of 0.13 and an inclination of 4° with respect to the ecliptic.[2] The body's observation arc begins with its first observation as A909 BL at Heidelberg Observatory in January 1909, almost 73 years prior to its official discovery observation at Anderson Mesa.[1]

Naming

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This minor planet was named after Mario di Martino (born 1947), Italian astronomer and photometrist of lightcurves at the Turin Observatory. The official naming proposed by the discoverer. The citation was prepared by Alain Harris and published by the Minor Planet Center on 14 April 1987 (M.P.C. 11749).[17]

Physical characteristics

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Di Martino is an assumed S-type asteroid,[3] while its low albedo indicates a carbonaceous composition.

Rotation period

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Three rotational lightcurve of Di Martino have been obtained from photometric observations by French amateur astronomer Pierre Antonini and at the Palomar Transient Factory and Haute Provence Observatory (U=2/3/3).[12][13][14] Lightcurve analysis gave a rotation period of 5.445 hours with a consolidated brightness amplitude between 0.32 and 0.51 magnitude (U=2/3/3), indicative of a somewhat elongated shape.[3]

In 2016, a modeled lightcurve gave a concurring sidereal period of 5.44517 hours using photometric data from a large international collaboration of astronomers. The study also determined two spin axes of (53.0°, −70.0°) and (231.0°, −75.0°) in ecliptic coordinates (λ, β).[15]

Diameter and albedo

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According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Di Martino measures between 11.267 and 15.60 kilometers in diameter and its surface has an albedo between 0.05 and 0.0925.[6][7][8][9][10][11] The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0540 and a diameter of 13.72 kilometers based on an absolute magnitude of 13.1.[3]

References

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  1. ^ a b c d e f "3247 Di Martino (1981 YE)". Minor Planet Center. Retrieved 9 May 2018.
  2. ^ a b c d "JPL Small-Body Database Browser: 3247 Di Martino (1981 YE)" (2018-02-25 last obs.). Jet Propulsion Laboratory. Retrieved 9 May 2018.
  3. ^ a b c d e f g h i "LCDB Data for (3247) Di Martino". Asteroid Lightcurve Database (LCDB). Retrieved 9 May 2018.
  4. ^ a b "Asteroid 3247 Di Martino – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 26 October 2019.
  5. ^ a b Zappalà, V.; Bendjoya, Ph.; Cellino, A.; Farinella, P.; Froeschle, C. (1997). "Asteroid Dynamical Families". NASA Planetary Data System: EAR-A-5-DDR-FAMILY-V4.1. Retrieved 18 March 2020.} (PDS main page)
  6. ^ a b c d Masiero, Joseph R.; Nugent, C.; Mainzer, A. K.; Wright, E. L.; Bauer, J. M.; Cutri, R. M.; et al. (October 2017). "NEOWISE Reactivation Mission Year Three: Asteroid Diameters and Albedos". The Astronomical Journal. 154 (4): 10. arXiv:1708.09504. Bibcode:2017AJ....154..168M. doi:10.3847/1538-3881/aa89ec.
  7. ^ a b c d 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.
  8. ^ 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.
  9. ^ 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.
  10. ^ a b c d 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.
  11. ^ 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)
  12. ^ a b c Waszczak, Adam; Chang, Chan-Kao; Ofek, Eran O.; Laher, Russ; Masci, Frank; Levitan, David; et al. (September 2015). "Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry". The Astronomical Journal. 150 (3): 35. arXiv:1504.04041. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75.
  13. ^ a b Behrend, Raoul. "Asteroids and comets rotation curves – (3247) Di Martino". Geneva Observatory. Retrieved 9 May 2018.
  14. ^ a b Birlan, M.; Barucci, M. A.; Angeli, C. A.; Doressoundiram, A.; De Sanctis, M. C. (June 1996). "Rotational properties of asteroids: CCD observations of nine small asteroids". Planetary and Space Science. 44 (6): 555–558. Bibcode:1996P&SS...44..555B. doi:10.1016/0032-0633(96)00019-0.
  15. ^ a b c d Hanus, J.; Durech, J.; Oszkiewicz, D. A.; Behrend, R.; Carry, B.; Delbo, M.; et al. (February 2016). "New and updated convex shape models of asteroids based on optical data from a large collaboration network". Astronomy and Astrophysics. 586: 24. arXiv:1510.07422. Bibcode:2016A&A...586A.108H. doi:10.1051/0004-6361/201527441.
  16. ^ 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.
  17. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 9 May 2018.
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