Astronomy:69 Hesperia

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Short description: Main-belt asteroid
69 Hesperia
69Hesperia (Lightcurve Inversion).png
A three-dimensional model of 69 Hesperia based on its light curve.
Discovery
Discovered byG. Schiaparelli
Discovery dateApril 29, 1861[1]
Designations
(69) Hesperia
Pronunciation/hɛˈspɪəriə/[2]
Named afterHesperia
Minor planet categoryMain belt
AdjectivesHesperian /hɛˈspɪəriən/[3]
Orbital characteristics
Epoch (absent)
|{{{apsis}}}|helion}}3.471 astronomical unit|AU (519.3 Gm)
|{{{apsis}}}|helion}}2.489 astronomical unit|AU (372.3 Gm)
2.980 astronomical unit|AU (445.8 Gm)
Eccentricity0.165
Orbital period1,879 days (5.14 a)
Inclination8.59°
Longitude of ascending node184.99°
288.8°
Physical characteristics
Dimensions138 km (IRAS)[4]
110 ± 15 km[5]
Mass(5.86±1.18)×1018 kg[6]
Mean density4.38±0.99 g/cm3[6]
Rotation period5.655 h[4]
Geometric albedo0.140[4]
M
Absolute magnitude (H)7.05[4]


Hesperia (minor planet designation: 69 Hesperia) is a large, M-type main-belt asteroid. It was discovered by the Italian astronomer Giovanni Schiaparelli on April 29, 1861[1] from Milan, while he was searching for the recently discovered 63 Ausonia.[7] It was his only asteroid discovery. Schiaparelli named it Hesperia in honour of Italy (the word is a Greek term for the peninsula).[8] The asteroid is orbiting the Sun with a period of 5.14 years, a semimajor axis of 2.980 astronomical unit|AU, and eccentricity of 0.165. The orbital plane is inclined by an angle of 8.59° to the plane of the ecliptic.

Hesperia was observed by Arecibo radar in February 2010.[5] Radar observations combined with lightcurve-based shape models, lead to a diameter estimate of 110 ± 15 km (68 ± 9.3 mi). The radar albedo is consistent with a high-metal M-type asteroid.[5] In the near infrared, a weak absorption feature near a wavelength of 0.9 μm can be attributed to orthopyroxenes on the surface.[9] A meteorite analogue of the reflectance spectra from 69 Hesperia is the Hoba ataxite.[10]

References

  1. 1.0 1.1 "Editorial Notice". The Minor Planet Circulars MPC 94743-95312: 94743. 2015-08-29. https://www.minorplanetcenter.net/iau/ECS/MPCArchive/2015/MPC_20150829.pdf. Retrieved 4 September 2015. 
  2. Noah Webster (1884) A Practical Dictionary of the English Language
  3. Hesperian (3rd ed.), Oxford University Press, September 2005, http://oed.com/search?searchType=dictionary&q=Hesperian  (Subscription or UK public library membership required.)
  4. 4.0 4.1 4.2 4.3 "JPL Small-Body Database Browser: 69 Hesperia". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=69. 
  5. 5.0 5.1 5.2 Shepard, Michael K.; Harris, Alan W.; Taylor, Patrick A.; Clark, Beth Ellen; Ockert-Bell, Maureen; Nolan, Michael C. et al. (2011). "Radar observations of Asteroids 64 Angelina and 69 Hesperia". Icarus 215 (2): 547–551. doi:10.1016/j.icarus.2011.07.027. Bibcode2011Icar..215..547S. http://echo.jpl.nasa.gov/asteroids/MBAs/shepard.etal.2011.angelina+hesperia.pdf. 
  6. 6.0 6.1 Carry, B. (December 2012), "Density of asteroids", Planetary and Space Science 73: pp. 98–118, doi:10.1016/j.pss.2012.03.009, Bibcode2012P&SS...73...98C.  See Table 1.
  7. De Meis, S. (2011), "A few aspects of Schiaparelli's studies", Memorie della Societa Astronomica Italiana 82: 290, Bibcode2011MmSAI..82..290D. 
  8. Schmadel, Lutz D. (2003), Dictionary of Minor Planet Names, Springer Science & Business Media, pp. 22, ISBN 978-3-540-00238-3, https://books.google.com/books?id=KWrB1jPCa8AC&pg=PA22. 
  9. Hardersen, Paul S. et al. (May 2005), "Near-IR spectral evidence for the presence of iron-poor orthopyroxenes on the surfaces of six M-type asteroids", Icarus 175 (1): 141−158, doi:10.1016/j.icarus.2004.10.017, Bibcode2005Icar..175..141H. 
  10. Neeley, J. R. et al. (August 2014), "The composition of M-type asteroids II: Synthesis of spectroscopic and radar observations", Icarus 238: 37−50, doi:10.1016/j.icarus.2014.05.008, Bibcode2014Icar..238...37N. 

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