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110 Lydia

From Wikipedia, the free encyclopedia
Main-belt asteroid

110 Lydia
Lightcurve-based 3D-model ofLydia
Discovery
Discovered byAlphonse Borrelly
Discovery date19 April 1870
Designations
(110) Lydia
Pronunciation/ˈlɪdiə/[1]
Named after
Lydia
A870 HA; 1899 VA;1972 YS1
Orbital characteristics[2]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc145.80 yr (53,255 d)
Aphelion2.9539 AU (441.90 Gm)
Perihelion2.51115 AU (375.663 Gm)
2.7325 AU (408.78 Gm)
Eccentricity0.081021
4.52 yr (1649.9 d)
17.99 km/s
348.344°
0° 13m 5.52s / day
Inclination5.9645°
56.871°
283.499°
TJupiter3.341
Physical characteristics
Dimensions
Mass6.7×1017 kg
0.0241 m/s2
Equatorialescape velocity
0.0455 km/s
  • 10.927 h (0.4553 d)[2]
  • 10.9258 hours[4]
Temperature~168 K
7.80[2][3]

110 Lydia is a largebelt asteroid with anM-type spectrum,[5] and thus may be metallic in composition, consisting primarily ofnickel-iron. It was discovered by French astronomerAlphonse Borrelly on 19 April 1870[6] and was named forLydia, theAsia Minor country populated byPhrygians.[7] TheLydia family of asteroids is named after it.

Observations made during 1958–1959 at theMcDonald Observatory and in 1969 at theKitt Peak National Observatory found an unevenlight curve with a period of 10.9267 hours.[8] In the late 1990s, a network of astronomers worldwide usedlight curves to derive spin states and shape models of 10 new asteroids, including (110) Lydia. They obtained a period of 10.92580 hours, with the brightness varying by no more than 0.2 inmagnitude.[4]

In theTholen classification system, it is categorized as anM-type asteroid, while the Busasteroid taxonomy system lists it as anXk asteroid.[9] Absorption features in the near infrared are attributed to low-iron, low-calciumorthopyroxene minerals. Water content on the surface is estimated at 0.14–0.27 bymass fraction (wt%).[10] Measurements of thethermal inertia of 110 Lydia give a value between 70 and200 J·m−2·K−1·s−1/2, compared to 50 forlunar regolith and 400 for coarse sand in an atmosphere.[3] It is a likely interloper in thePaduafamily of minor planets that share similar dynamic properties.[11]

Lydiaocculted a dimstar on 18 September 1999.

References

[edit]
  1. ^Noah Webster (1884)A Practical Dictionary of the English Language
  2. ^abcdeYeomans, Donald K.,"110 Lydia",JPL Small-Body Database Browser,NASA Jet Propulsion Laboratory, retrieved12 May 2016.
  3. ^abcdDelbo', Marco; Tanga, Paolo (February 2009), "Thermal inertia of main belt asteroids smaller than 100 km from IRAS data",Planetary and Space Science, vol. 57, no. 2, pp. 259–265,arXiv:0808.0869,Bibcode:2009P&SS...57..259D,doi:10.1016/j.pss.2008.06.015.
  4. ^abDurech, J.; et al. (April 2007),"Physical models of ten asteroids from an observers' collaboration network"(PDF),Astronomy and Astrophysics, vol. 465, no. 1, pp. 331–337,Bibcode:2007A&A...465..331D,doi:10.1051/0004-6361:20066347.
  5. ^abDeMeo, Francesca E.; et al. (2011),"An extension of the Bus asteroid taxonomy into the near-infrared"(PDF),Icarus,202 (1):160–180,Bibcode:2009Icar..202..160D,doi:10.1016/j.icarus.2009.02.005, archived fromthe original(PDF) on 17 March 2014, retrieved11 December 2013. See appendix A.
  6. ^"Numbered Minor Planets 1–5000",Discovery Circumstances, IAU Minor Planet center, retrieved7 April 2013.
  7. ^Schmadel, Lutz D. (2003),Dictionary of Minor Planet Names (5th ed.), Springer, p. 23,ISBN 3-540-00238-3.
  8. ^Taylor, R. C.; et al. (March 1971), "Minor Planets and Related Objects. VI. Asteroid (110) Lydia",Astronomical Journal, vol. 76, p. 141,Bibcode:1971AJ.....76..141T,doi:10.1086/111097.
  9. ^DeMeo, Francesca E.; et al. (July 2009),"An extension of the Bus asteroid taxonomy into the near-infrared"(PDF),Icarus, vol. 202, no. 1, pp. 160–180,Bibcode:2009Icar..202..160D,doi:10.1016/j.icarus.2009.02.005, archived fromthe original(PDF) on 17 March 2014, retrieved8 April 2013. See appendix A.
  10. ^Hardersen, Paul S.; Gaffey, Michael J.; Abell, Paul A. (January 1983), "Near-IR spectral evidence for the presence of iron-poor orthopyroxenes on the surfaces of six M-type asteroids",Icarus, vol. 175, no. 1, pp. 141–158,Bibcode:2005Icar..175..141H,doi:10.1016/j.icarus.2004.10.017.
  11. ^Carruba, V. (May 2009), "The (not so) peculiar case of the Padua family",Monthly Notices of the Royal Astronomical Society,395 (1):358–377,Bibcode:2009MNRAS.395..358C,doi:10.1111/j.1365-2966.2009.14523.x.

External links

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