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159 Aemilia

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Main-belt asteroid

159 Aemilia
3D convex shape model of 159 Aemilia
Discovery
Discovered byP. P. Henry
Discovery date26 January 1876
Designations
MPC designation(159) Aemilia
Pronunciation/ɪˈmɪliə/
Named afterVia Aemilia
Alternative designationsA876 BA; 1959 EG1
Minor planet categoryMain belt (Hygiea family)
AdjectivesAemilian /ɪˈmɪliən/
Orbital characteristics
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc112.24 yr (40996 d)
Aphelion3.4377 AU (514.27 Gm)
Perihelion2.76896 AU (414.231 Gm)
Semi-major axis3.1033 AU (464.25 Gm)
Eccentricity0.10775
Orbital period (sidereal)5.47 yr (1996.8 d)
Average orbital speed16.86 km/s
Mean anomaly214.036°
Mean motion0° 10 49.008 / day
Inclination6.1308°
Longitude of ascending node134.132°
Argument of perihelion333.387°
Earth MOID1.78581 AU (267.153 Gm)
Jupiter MOID1.67782 AU (250.998 Gm)
TJupiter3.203
Physical characteristics
Dimensions124.97±2.4 km
127.3 km
Mass~1.4×10 kg
Mean density~1.4 g/cm
Equatorial surface gravity~0.024 m/s
Equatorial escape velocity~0.055 km/s
Synodic rotation period24.476 h (1.0198 d)
~1.05 d
Geometric albedo0.0639±0.003
0.0627 ± 0.0142
Temperature~160 K
max: 239 K (−34 °C; −29 °F)
Spectral typeC (Tholen)
Absolute magnitude (H)8.12, 8.10

159 Aemilia is a large main-belt asteroid. Aemilia was discovered by the French brothers Paul Henry and Prosper Henry on January 26, 1876. The credit for this discovery was given to Paul. It is probably named after the Via Aemilia, a Roman road in Italy that runs from Piacenza to Rimini.

This slowly rotating, dark asteroid has a primitive carbonaceous composition, based upon its classification as a C-type asteroid. Photometric observations made in 2006 gave a rotation period of about 25 hours. Subsequent observations made at the Oakley Observatory in Terre Haute, Indiana found a light curve period of 16.37 ± 0.02 hours, with variation in brightness of 0.24 ± 0.04 in magnitude.

It orbits within the Hygiea family, although it may be an unrelated interloping asteroid, as it is too big to have arisen from the cratering process that most probably produced that family. Three stellar occultations by Aemilia have been recorded so far, the first in 2001, the second in 2003 and the third in 2016

References

  1. Noah Webster (1884) A Practical Dictionary of the English Language
  2. "Emilian, Æmilian". Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
  3. ^ Yeomans, Donald K., "159 Aemilia", JPL Small-Body Database Browser, NASA Jet Propulsion Laboratory, retrieved 12 May 2016.
  4. ^ Pravec, P.; et al. (May 2012), "Absolute Magnitudes of Asteroids and a Revision of Asteroid Albedo Estimates from WISE Thermal Observations", Asteroids, Comets, Meteors 2012, Proceedings of the conference held May 16–20, 2012 in Niigata, Japan, vol. 1667, no. 1667, p. 6089, Bibcode:2012LPICo1667.6089P. See Table 4.
  5. Krasinsky, G. A.; et al. (July 2002), "Hidden Mass in the Asteroid Belt", Icarus, 158 (1): 98–105, Bibcode:2002Icar..158...98K, doi:10.1006/icar.2002.6837.
  6. "Asteroid Lightcurve Data Base (LCDB) | PDS SBN Asteroid/Dust Subnode".
  7. Ditteon, Richard; Hawkins, Scot (September 2007), "Asteroid Lightcurve Analysis at the Oakley Observatory - October-November 2006", The Minor Planet Bulletin, 34 (3): 59–64, Bibcode:2007MPBu...34...59D.
  8. 2016/09/01 | 159 | Aemilia | TYC 6349-00855-1

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