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.
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,[8] 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.[9] Its spectral class is intermediate between the C-type and P-type asteroids.[7]
10μ radiometric data collected from Kitt Peak in 1975 gave a diameter estimate of 255 km.[10] 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.[11]
References
^ abc"JPL Small-Body Database Browser: 324 Bamberga". 2008-07-26 last obs. Retrieved 11 May 2016.
^ abcdeP. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. Astronomy & Astrophysics 54, A56
^ abcCarry, B. (December 2012), "Density of asteroids", Planetary and Space Science, vol. 73, pp. 98–118, arXiv:1203.4336, Bibcode:2012P&SS...73...98C, doi:10.1016/j.pss.2012.03.009. See Table 1.
^ abcTedesco, E.F.; Noah, P.V.; Noah, M.; Price, S.D. (2004). "IRAS Minor Planet Survey. IRAS-A-FPA-3-RDR-IMPS-V6.0". NASA Planetary Data System. Archived from the original on 17 January 2010. Retrieved 15 March 2007.
^Pitjeva, E. V. (2005). (PDF). Solar System Research. 39 (3): 176. Bibcode:2005SoSyR..39..176P. doi:10.1007/s11208-005-0033-2. Archived from the original (PDF) on 31 October 2008.
^Harris, A. W.; Warner, B.D.; Pravec, P., eds. (2006). . NASA Planetary Data System. Archived from the original on 28 January 2007. Retrieved 15 March 2007.
^ abNeese, C., ed. (2005). . NASA Planetary Data System. Archived from the original on 10 March 2007. Retrieved 15 March 2007.
^Donald H. Menzel & Jay M. Pasachoff (1983). A Field Guide to the Stars and Planets (2nd ed.). Boston, MA: Houghton Mifflin. p. 391. ISBN0-395-34835-8.
^"JPL Small-Body Database Search Engine: diameter > 150 (km) and rot_per > 24 (h)". JPL Solar System Dynamics. Retrieved 6 June 2015.
^Morrison, D.; Chapman, C. R. (March 1976), "Radiometric diameters for an additional 22 asteroids", Astrophysical Journal, vol. 204, pp. 934–939, Bibcode:2008mgm..conf.2594S, doi:10.1142/9789812834300_0469.
^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, vol. 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
Close approach · Discovery · Ephemeris · Orbit diagram · Orbital elements · Physical parameters
January 07, 2023
bamberga, bamberga, minor, planet, designation, largest, asteroids, asteroid, belt, discovered, johann, palisa, february, 1892, vienna, largest, asteroids, asteroid, belt, apart, from, near, earth, asteroid, eros, last, asteroid, which, ever, easily, visible, . 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 324 BambergaVLT image of BambergaDiscoveryDiscovered byJohann PalisaDiscovery date25 February 1892DesignationsMPC designation 324 BambergaPronunciation b ae m ˈ b ɜːr ɡ e Named afterBambergMinor planet categoryMain beltAdjectivesBambergian b ae m ˈ b ɜːr dʒ i e n ɡ i e n Orbital characteristics 1 Epoch 31 July 2016 JD 2457600 5 Uncertainty parameter 0Observation arc124 08 yr 45321 d Aphelion3 59442 AU 537 718 Gm Perihelion1 77023 AU 264 823 Gm Semi major axis2 68232 AU 401 269 Gm Eccentricity0 34004Orbital period sidereal 4 39 yr 1604 6 d Mean anomaly225 419 Mean motion0 13m 27 682s dayInclination11 1011 Longitude of ascending node327 883 Argument of perihelion44 2409 Physical characteristicsDimensionsc a 0 96 0 05 2 Mean diameter227 3 km 2 234 67 7 80 km 3 229 4 7 4 km IRAS 4 Mass 10 2 0 9 1018 kg 2 11 1018 kg 5 10 3 1 0 1018 kg 3 Mean density1 67 0 16 g cm3 2 1 52 0 20 g cm3 3 Synodic rotation period1 226 d 6 29 43 h 1 226 d 1 Geometric albedo0 060 calculated 2 0 0628 0 004 4 Spectral typeC type asteroid 7 Absolute magnitude H 6 82 1 4 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 linksObservation Edit 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 8 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 EditThe 29 hour rotation period is unusually long for an asteroid more than 150 km in diameter 9 Its spectral class is intermediate between the C type and P type asteroids 7 10m radiometric data collected from Kitt Peak in 1975 gave a diameter estimate of 255 km 10 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 11 References Edit a b c JPL Small Body Database Browser 324 Bamberga 2008 07 26 last obs Retrieved 11 May 2016 a b c d e P Vernazza et al 2021 VLT SPHERE imaging survey of the largest main belt asteroids Final results and synthesis Astronomy amp Astrophysics 54 A56 a b c Carry B December 2012 Density of asteroids Planetary and Space Science vol 73 pp 98 118 arXiv 1203 4336 Bibcode 2012P amp SS 73 98C doi 10 1016 j pss 2012 03 009 See Table 1 a b c Tedesco E F Noah P V Noah M Price S D 2004 IRAS Minor Planet Survey IRAS A FPA 3 RDR IMPS V6 0 NASA Planetary Data System Archived from the original on 17 January 2010 Retrieved 15 March 2007 Pitjeva E V 2005 High Precision Ephemerides of Planets EPM and Determination of Some Astronomical Constants PDF Solar System Research 39 3 176 Bibcode 2005SoSyR 39 176P doi 10 1007 s11208 005 0033 2 Archived from the original PDF on 31 October 2008 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 Archived from the original on 28 January 2007 Retrieved 15 March 2007 a b Neese C ed 2005 Asteroid Taxonomy EAR A 5 DDR TAXONOMY V5 0 NASA Planetary Data System Archived from the original on 10 March 2007 Retrieved 15 March 2007 Donald H Menzel amp 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 JPL Small Body Database Search Engine diameter gt 150 km and rot per gt 24 h JPL Solar System Dynamics Retrieved 6 June 2015 Morrison D Chapman C R March 1976 Radiometric diameters for an additional 22 asteroids Astrophysical Journal vol 204 pp 934 939 Bibcode 2008mgm conf 2594S doi 10 1142 9789812834300 0469 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 vol 19 pp 405 406 Bibcode 1988LPI 19 405G External links Edit324 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 Retrieved from https en wikipedia org w index php title 324 Bamberga amp oldid 1123252243, wikipedia, wiki, book, books, library,
