324 Bamberga

Short description: Main-belt asteroid

324 Bamberga

VLT image of Bamberga

Discovery
Discovered by| Johann Palisa
Discovery date| 25 February 1892
Designations

MPC designation

| (324) Bamberga
Pronunciation| /bæmˈbɜːrɡə/
Named after| Bamberg
Minor planet category| Main belt
Adjectives| Bambergian /bæmˈbɜːrdʒiən, -ɡiən/
Orbital characteristics[1]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc| 124.08 yr (45321 d)
|{{{apsis}}}|helion}}| 3.59442 astronomical unit|AU (537.718 Gm)
|{{{apsis}}}|helion}}| 1.77023 AU (264.823 Gm)

Semi-major axis

| 2.68232 AU (401.269 Gm)
Eccentricity| 0.34004
Orbital period| 4.39 yr (1604.6 d)
Mean anomaly| 225.419°
Mean motion| 0° 13m 27.682s / day
Inclination| 11.1011°
Longitude of ascending node| 327.883°

|{{{apsis}}}|helion}}

| 44.2409°
Physical characteristics
Dimensions| c/a = 0.96±0.05[2]
Mean diameter| 227±3 km[2]
234.67 ± 7.80 km[3]
229.4 ± 7.4 km (IRAS)[4]
Mean density| 1.67±0.16 g/cm3[2]
1.52±0.20 g/cm3[3]
Rotation period| 1.226 d[5]
29.43 h (1.226 d)[1]
Geometric albedo| 0.060 (calculated)[2]
0.0628±0.004[4]

Spectral type

| C-type asteroid[6]
Absolute magnitude (H)| 6.82[1][4]

Bamberga (minor planet designation: 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.

## Contents

* 1 Observation
* 2 Characteristics
* 3 References
* 4 External links

## Observation

Bamberga's orbit

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,[7] 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.[8] Its spectral class is intermediate between the C-type and P-type asteroids.[6]

10μ radiometric data collected from Kitt Peak in 1975 gave a diameter estimate of 255 km.[9] 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.[10]

## References

1. ↑ 1.0 1.1 1.2 "JPL Small-Body Database Browser: 324 Bamberga". https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=324.
2. ↑ 2.0 2.1 2.2 2.3 P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. Astronomy & Astrophysics 54, A56
3. ↑ 3.0 3.1 Carry, B. (December 2012), "Density of asteroids", Planetary and Space Science 73: pp. 98–118, doi:10.1016/j.pss.2012.03.009, Bibcode: 2012P&SS...73...98C. See Table 1.
4. ↑ 4.0 4.1 4.2 Tedesco, E.F.; Noah, P.V. (2004). "IRAS Minor Planet Survey. IRAS-A-FPA-3-RDR-IMPS-V6.0.". NASA Planetary Data System. http://www.psi.edu/pds/resource/imps.html.
5. ↑ Harris, A. W.; Warner, B.D.; Pravec, P., eds (2006). "Asteroid Lightcurve Derived Data. EAR-A-5-DDR-DERIVED-LIGHTCURVE-V8.0.". NASA Planetary Data System. http://www.psi.edu/pds/resource/lc.html.
6. ↑ 6.0 6.1 Neese, C., ed (2005). "Asteroid Taxonomy.EAR-A-5-DDR-TAXONOMY-V5.0.". NASA Planetary Data System. http://www.psi.edu/pds/resource/taxonomy.html.
7. ↑ Donald H. Menzel; Jay M. Pasachoff (1983). A Field Guide to the Stars and Planets (2nd ed.). Boston, MA: Houghton Mifflin. p. 391. ISBN 0-395-34835-8. https://archive.org/details/fieldguidetostar00menz_0/page/391.
8. ↑ "JPL Small-Body Database Search Engine: diameter > 150 (km) and rot_per > 24 (h)". JPL Solar System Dynamics. http://ssd.jpl.nasa.gov/sbdb_query.cgi?obj_group=all;obj_kind=all;obj_numbered=all;OBJ_field=0;ORB_field=0;combine_mode=AND;c1_group=OBJ;c1_item=Ap;c1_op=>;c1_value=150;c2_group=OBJ;c2_item=As;c2_op=>;c2_value=24;table_format=HTML;max_rows=50;format_option=comp;c_fields=AcBhBgBjBiBnBsAiApAs;.cgifields=format_option;.cgifields=ast_orbit_class;.cgifields=combine_mode;.cgifields=table_format;.cgifields=obj_kind;.cgifields=obj_group;.cgifields=obj_numbered;.cgifields=com_orbit_class&query=1&c_sort=AsD.
9. ↑ Morrison, D.; Chapman, C. R. (March 1976), "Radiometric diameters for an additional 22 asteroids", Astrophysical Journal 204: pp. 934–939, doi:10.1142/9789812834300_0469, Bibcode: 2008mgm..conf.2594S.
10. ↑ Gradie, J.; Flynn, L. (March 1988), "A Search for Satellites and Dust Belts Around Asteroids: Negative Results", Abstracts of the Lunar and Planetary Science Conference 19: pp. 405–406, Bibcode: 1988LPI....19..405G.

## External links

* 324 Bamberga at AstDyS-2, Asteroids—Dynamic Site
* Ephemeris * Observation prediction * Orbital info * Proper elements * Observational info
* 324 Bamberga at the JPL Small-Body Database
* Close approach * Discovery * Ephemeris * Orbit diagram * Orbital elements * Physical parameters

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