147 Protogeneia

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147 Protogeneia
147Protogeneia (Lightcurve Inversion).png
A three-dimensional model of 147 Protogeneia based on its light curve
Discovery[1]
Discovered by Lipót Schulhof
Discovery date 10 July 1875
Designations
MPC designation (147) Protogeneia
Named after
Protogeneia
Main belt
Orbital characteristics[1][2]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc 132.02 yr (48222 d)
Aphelion 3.2230 AU (482.15 Gm)
Perihelion 3.04727 AU (455.865 Gm)
3.13512 AU (469.007 Gm)
Eccentricity 0.028020
5.55 yr (2027.6 d)
16.82 km/s
92.9051°
0° 10m 39.184s / day
Inclination 1.9309°
248.357°
100.692°
Earth MOID 2.03996 AU (305.174 Gm)
Jupiter MOID 1.90385 AU (284.812 Gm)
Jupiter Tisserand parameter 3.211
Physical characteristics
Mean radius
66.465±2.55 km[2]
59.22 ± 5.225 km[3]
Mass (1.23 ± 0.05) × 1019 kg[3]
Mean density
14.13 ± 3.78 g/cm3[3]
Equatorial surface gravity
0.0371 m/s²
Equatorial escape velocity
0.0703 km/s
7.8528 h (0.32720 d)[2][4]
0.0492±0.004[2]
Temperature ~157 K
C
12.4 to 14.5
8.27[4]
8.8[2]

147 Protogeneia is a large main belt asteroid that was discovered by the Hungarian astronomer Lipót Schulhof on July 10, 1875, from the Vienna Observatory; it was his only asteroid discovery. Its name is Greek for "first born" and was chosen by Karl L. Littrow in allusion to the fact that this was the first asteroid discovered by an astronomer who was already known for work in other fields of astronomy.[5]

This object has a low orbital eccentricity and inclination, with an orbital period roughly double that of the planet Jupiter, it has been identified as a member of the Hecuba group of asteroids that share a 2:1 mean-motion orbital resonance with the giant planet.[6] Based upon its spectrum, it has a Tholen classification as a C-type asteroid,[7] which indicates has a dark surface and probably a primitive composition of carbonaceous material.

Photometric observations of this asteroid at the Altimira Observatory in 2004 gave a light curve with a period of 7.8528 ± 0.0008 hours and a brightness variation of 0.28 in magnitude.[4] A photometric study was reported in 2006 from the Yunnan Observatory in China, finding a matching period of 7.852 hours and a brightness variation of 0.25 magnitude. They estimate the ratio of the lengths for the asteroid's major and minor axes is at least 1.26:1.[8]

There is one reported stellar occultation by Protogeneia, on May 28, 2002, from Texas.[citation needed]

References[edit]

  1. ^ "The Asteroid Orbital Elements Database". astorb. Lowell Observatory. 
  2. ^ a b c d e Yeomans, Donald K., "147 Protogeneia", JPL Small-Body Database Browser, NASA Jet Propulsion Laboratory, retrieved 6 May 2016. 
  3. ^ a b c Carry, B. (December 2012), "Density of asteroids", Planetary and Space Science, 73: 98–118, arXiv:1203.4336Freely accessible, Bibcode:2012P&SS...73...98C, doi:10.1016/j.pss.2012.03.009.  See Table 1.
  4. ^ a b c Buchheim, Robert K. (June 2005), "Lightcurve of 147 Protogeneia", The Minor Planet Bulletin, 32 (2): 35–36, Bibcode:2005MPBu...32...35B, ISSN 1052-8091. 
  5. ^ Schmadel, Lutz D. (2003), Dictionary of Minor Planet Names (5th ed.), Springer, p. 28, ISBN 3540002383. 
  6. ^ Levy, Sophia H. (August 1939), "Mean Elements and Perturbations by the Berkeley Tables of Minor Planets of the Hecuba Group", Publications of the Astronomical Society of the Pacific, 51 (302): 225, Bibcode:1939PASP...51..224L, doi:10.1086/125066. 
  7. ^ Bel'Skaya, I. N.; et al. (1991), "Polarimetry of CMEU asteroids. II. A peculiarity of M-type asteroids", Kinematics and Physics of Celestial Bodies, 7 (6): 8–11, Bibcode:1991KPCB....7....8B. 
  8. ^ Zhang, Xi-Liang; et al. (December 2006), "CCD Photometry of Asteroid (147) Protogeneia", Chinese Journal of Astronomy & Astrophysics, 6 (6): 729–732, Bibcode:2006ChJAA...6..729Z, doi:10.1088/1009-9271/6/6/12. 

External links[edit]