 Orbital diagram | |
| Discovery | |
|---|---|
| Discovered by | Johann Palisa |
| Discovery date | 5 June 1885 |
| Designations | |
| MPC designation | (248) Lameia |
| Pronunciation | /ləˈmiːə/ |
| Named after | Lamia |
| Alternative designations | A885 LA, 1959 LO |
| Minor planet category | Main belt |
| Orbital characteristics | |
| Epoch 31 July 2016 (JD 2457600.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 130.86 yr (47,796 d) |
| Aphelion | 2.64 AU (394.30 Gm) |
| Perihelion | 2.31 AU (345.06 Gm) |
| Semi-major axis | 2.47 AU (369.67 Gm) |
| Eccentricity | 0.066588 |
| Orbital period (sidereal) | 3.88 yr (1,418.9 d) |
| Average orbital speed | 18.95 km/s |
| Mean anomaly | 264.207° |
| Mean motion | 0° 15 13.392 / day |
| Inclination | 4.0581° |
| Longitude of ascending node | 246.845° |
| Argument of perihelion | 10.782° |
| Physical characteristics | |
| Dimensions | 48.66±2.5 km |
| Synodic rotation period | 11.912 h (0.4963 d) |
| Geometric albedo | 0.0615±0.007 |
| Absolute magnitude (H) | 10.2 |
248 Lameia is a typical main belt asteroid. It was discovered by Austrian astronomer Johann Palisa on 5 June 1885 in Vienna and was named after the Lamia, a lover of Zeus in Ancient Greek mythology. 248 Lameia is orbiting the Sun with a period of 3.88 years and a low eccentricity (ovalness) of 0.067. The semimajor axis of 2.47 AU is slightly inward from the 3:1 Kirkwood Gap. Its orbital plane is inclined by 4° to the plane of the ecliptic.
On 27 June 1998 an occultation of the 8th magnitude star PPM 236753 (HD 188960) by 248 Lameia was timed by five observers near Gauteng, South Africa. The chords produced a rough size estimate of a 62 × 53 km ellipse. The size estimate based on IRAS Minor Planet Survey data is ~49 km. The rotation rate of this object is commensurate with the rotation of the Earth, requiring observations from different locations to build a complete light curve. These yield a rotation estimate of 11.912±0.001 h with a brightness variation of 0.17±0.01 magnitude in amplitude. The same data set gives a size estimate of 47±3 km, in agreement with earlier measurements.
Infrared imaging of this body shows a relatively featureless spectra that suggests materials that are similar to carbonaceous chondrite meteorites.
References
- 'Lamea' in Noah Webster (1884) A Practical Dictionary of the English Language
- ^ "248 Lameia". JPL Small-Body Database. NASA/Jet Propulsion Laboratory. Retrieved 12 May 2016.
- ^ Pilcher, Frederick; et al. (April 2015). "Rotation Period and H-G Parameters Determination for 248 Lameia". Bulletin of the Minor Planets Section of the Association of Lunar and Planetary Observers. 42 (2): 137–139. Bibcode:2015MPBu...42..137P.
- Saha, Prasenjit (December 1992). "Simulating the 3:1 Kirkwood gap". Icarus. 100 (2): 434–439. Bibcode:1992Icar..100..434S. doi:10.1016/0019-1035(92)90109-K.
- "HD 188960". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 24 November 2020.
- Fraser, B.; Overbeek, M. D. (1998). "Occultation Observation of PPM 236753 by 248 Lameia, 1998 June 27". Monthly Notes of the Astronomical Society of Southern Africa. 57: 85. Bibcode:1998MNSSA..57...85F.
- Fieber-Beyer, Sherry K.; Gaffey, Michael J. (September 2015). "Near-infrared spectroscopy of 3:1 Kirkwood Gap asteroids III". Icarus. 257: 113–125. Bibcode:2015Icar..257..113F. doi:10.1016/j.icarus.2015.04.034.
External links
- The Asteroid Orbital Elements Database
- Minor Planet Discovery Circumstances
- Asteroid Lightcurve Data File
- 248 Lameia at AstDyS-2, Asteroids—Dynamic Site
- 248 Lameia at the JPL Small-Body Database
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