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324 Bamberga
Main-belt asteroid
Main-belt asteroid
| Field | Value |
|---|---|
| minorplanet | yes |
| background | #D6D6D6 |
| name | 324 Bamberga |
| image | Potw1749a Bamberga crop.png |
| caption | VLT image of Bamberga |
| discoverer | Johann Palisa |
| discovered | 25 February 1892 |
| mpc_name | (324) Bamberga |
| pronounced | |
| adjective | Bambergian |
| named_after | Bamberg |
| mp_category | Main belt |
| epoch | 31 July 2016 (JD 2457600.5) |
| semimajor | 2.68232 AU |
| perihelion | 1.77023 AU |
| aphelion | 3.59442 AU |
| eccentricity | 0.34004 |
| period | 4.39 yr (1604.6 d) |
| inclination | 11.1011° |
| asc_node | 327.883° |
| arg_peri | 44.2409° |
| mean_anomaly | 225.419° |
| flattening | 0.04 |
| mean_diameter | |
| 234.67 ± 7.80 km | |
| 229.4 ± 7.4 km (IRAS) | |
| mass | |
| density | |
| rotation | 1.226 d |
| 29.43 h{{cite web | |
| id | 2008-07-26 last obs |
| title | JPL Small-Body Database Browser: 324 Bamberga |
| url | https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=324 |
| access-date | 11 May 2016}} |
| spectral_type | C-type asteroid |
| abs_magnitude | 6.82 |
| 7.23 | |
| albedo | 0.060 (calculated) |
| mean_motion | / day |
| orbit_ref | |
| observation_arc | 124.08 yr (45321 d) |
| uncertainty | 0 |
234.67 ± 7.80 km 229.4 ± 7.4 km (IRAS)
29.43 h{{cite web |access-date=11 May 2016}} 7.23
324 Bamberga is one of the largest asteroids in the asteroid belt. It was discovered by Johann Palisa on 25 February 1892 in Vienna. It is one of the top-20 largest asteroids in the asteroid belt. Apart from the near-Earth asteroid Eros, it was the last asteroid which is ever easily visible with binoculars to be discovered.
Overall Bamberga is the tenth-brightest main-belt asteroid after, in order, Vesta, Pallas, Ceres, Iris, Hebe, Juno, Melpomene, Eunomia and Flora. Its high eccentricity (for comparison 36% higher than that of Pluto), though, means that at most oppositions other asteroids reach higher magnitudes.
Observation
Although its very high orbital eccentricity means its opposition magnitude varies greatly, at a rare opposition near perihelion Bamberga can reach a magnitude of +8.0, which is as bright as Saturn's moon Titan. Such near-perihelion oppositions occur on a regular cycle every twenty-two years, with the last occurring in 2013 and the next in 2035, when attaining magnitude 8.1 on 13 September. Its brightness at these rare near-perihelion oppositions makes Bamberga the brightest C-type asteroid, roughly one magnitude brighter than 10 Hygiea's maximum brightness of around +9.1. At such an opposition Bamberga can in fact be closer to Earth than any main-belt asteroid with magnitude above +9.5, getting as close as 0.78 AU. For comparison, 7 Iris never comes closer than 0.85 AU and 4 Vesta never closer than 1.13 AU (when it becomes visible to the naked eye in a light pollution-free sky).
Characteristics
The 29-hour rotation period is unusually long for an asteroid more than 150 km in diameter. Its spectral class is intermediate between the C-type and P-type asteroids.
10μ radiometric data collected from Kitt Peak in 1975 gave a diameter estimate of 255 km. An occultation of Bamberga was observed on 8 December 1987, and gave a diameter of about 228 km, in agreement with IRAS results. In 1988 a search for satellites or dust orbiting this asteroid was performed using the UH88 telescope at the Mauna Kea Observatories, but the effort came up empty.
Notes
References
References
- P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. ''Astronomy & Astrophysics'' 54, A56
- Tedesco, E.F.. (2004). "IRAS Minor Planet Survey. IRAS-A-FPA-3-RDR-IMPS-V6.0.". [[Planetary Data System.
- Pitjeva, E. V.. (2005). "High-Precision Ephemerides of Planets—EPM and Determination of Some Astronomical Constants". Solar System Research.
- (2006). "Asteroid Lightcurve Derived Data. EAR-A-5-DDR-DERIVED-LIGHTCURVE-V8.0.". [[Planetary Data System.
- (2005). "Asteroid Taxonomy.EAR-A-5-DDR-TAXONOMY-V5.0.". [[Planetary Data System.
- Donald H. Menzel. (1983). "A Field Guide to the Stars and Planets". [[Houghton Mifflin]].
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