Astronomy:170 Maria
 Asteroid Maria passing near a cluster of galaxies as seen by a four inch telescope over a period of nearly two hours. | |
| Discovery | |
|---|---|
| Discovered by | J. Perrotin |
| Discovery date | 10 January 1877 |
| Designations | |
| (170) Maria | |
| Pronunciation | /məˈriːə/ mə-REE-ə |
| A877 AA; 1958 AC | |
| Minor planet category | Main belt (Maria) |
| Orbital characteristics[1] | |
| Epoch 31 July 2016 (JD 2457600.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 116.69 yr (42622 d) |
| |{{{apsis}}}|helion}} | 2.7161 astronomical unit|AU (406.32 Gm) |
| |{{{apsis}}}|helion}} | 2.3923 AU (357.88 Gm) |
| 2.5542 AU (382.10 Gm) | |
| Eccentricity | 0.063388 |
| Orbital period | 4.08 yr (1491.0 d) |
| Mean anomaly | 88.062° |
| Mean motion | 0° 14m 29.184s / day |
| Inclination | 14.377° |
| Longitude of ascending node | 301.34° |
| 159.21° | |
| Earth MOID | 1.4114 AU (211.14 Gm) |
| Jupiter MOID | 2.39948 AU (358.957 Gm) |
| TJupiter | 3.392 |
| Physical characteristics | |
| Dimensions | 44.30±1.0 km |
| Rotation period | 13.120 h (0.5467 d) |
| Geometric albedo | 0.1579±0.007 |
| S[2] | |
| Absolute magnitude (H) | 9.39 |
170 Maria is a Main belt asteroid that was discovered by French astronomer Henri Joseph Perrotin on January 10, 1877.[3] Its orbit was computed by Antonio Abetti, and the asteroid was named after his sister, Maria. This is the namesake of the Maria asteroid family; one of the first asteroid families to be identified by Japanese astronomer Kiyotsugu Hirayama in 1918.[4] This family may be the parent body of the large near-Earth objects 433 Eros and 1036 Ganymed.[5]
In the Tholen classification system, this is categorized as a stony S-type asteroid based on its spectrum.[2] Observations performed at the Palmer Divide Observatory in Colorado Springs, Colorado during 2007 produced a light curve with a period of 13.120 ± 0.002 hours and a brightness range of 0.21 ± 0.02 in magnitude. Previous measurements from 2000 gave 13.14 and 5.510 hour estimates for the period.[6]
An occultation of a star by Maria was observed from Manitoba, Canada, on June 10, 1997.
References
- ↑ Yeomans, Donald K., "170 Maria", JPL Small-Body Database Browser (NASA Jet Propulsion Laboratory), https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=170, retrieved 12 May 2016.
- ↑ 2.0 2.1 DeMeo, Francesca E. et al. (July 2009), "An extension of the Bus asteroid taxonomy into the near-infrared", Icarus 202 (1): 160–180, doi:10.1016/j.icarus.2009.02.005, Bibcode: 2009Icar..202..160D, archived from the original on 2014-03-17, https://web.archive.org/web/20140317200310/https://www.tara.tcd.ie/bitstream/2262/43276/1/PEER_stage2_10.1016/j.icarus.2009.02.005.pdf, retrieved 2013-04-08. See appendix A.
- ↑ "Numbered Minor Planets 1–5000", Discovery Circumstances (IAU Minor Planet center), archived from the original on February 13, 2012, https://web.archive.org/web/20120213005447/http://www.minorplanetcenter.net/iau/lists/NumberedMPs000001.html, retrieved 2013-04-07.
- ↑ Veeder, G. J. et al. (March 1995), "Eos, Koronis, and Maria family asteroids: Infrared (JHK) photometry", Icarus 114 (1): 186–196, doi:10.1006/icar.1995.1053, Bibcode: 1995Icar..114..186V, https://trs.jpl.nasa.gov/bitstream/2014/29296/1/95-0212.pdf.
- ↑ Aljbaae, S. et al. (November 2017), "The Maria asteroid family", Monthly Notices of the Royal Astronomical Society 471 (4): 4820–4826, doi:10.1093/mnras/stx1921, Bibcode: 2017MNRAS.471.4820A.
- ↑ Warner, Brian D. (September 2007), "Asteroid Lightcurve Analysis at the Palmer Divide Observatory", The Minor Planet Bulletin 34 (3): 72, Bibcode: 2007MPBu...34...72W.
External links
- Lightcurve plot of 170 Maria, Palmer Divide Observatory, B. D. Warner (2007)
- Asteroid Lightcurve Database (LCDB), query form (info )
- Dictionary of Minor Planet Names, Google books
- Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend
- Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center
- 170 Maria at AstDyS-2, Asteroids—Dynamic Site
- 170 Maria at the JPL Small-Body Database
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