Astronomy:1192 Prisma

From HandWiki
1192 Prisma
001192-asteroid shape model (1192) Prisma.png
Modelled shape of Prisma from its lightcurve
Discovery[1]
Discovered byA. Schwassmann
Discovery siteBergedorf Obs.
Discovery date17 March 1931
Designations
(1192) Prisma
Named afterBergedorf Spectral Catalogue
(astronomical catalog)[2]
1931 FE
Minor planet categorymain-belt · (inner)
Phocaea[3][4]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc85.77 yr (31,328 days)
|{{{apsis}}}|helion}}2.9762 AU
|{{{apsis}}}|helion}}1.7561 AU
2.3661 AU
Eccentricity0.2578
Orbital period3.64 yr (1,329 days)
Mean anomaly297.62°
Mean motion0° 16m 14.88s / day
Inclination23.902°
Longitude of ascending node1.3517°
131.44°
Physical characteristics
Dimensions7.22 km (calculated)[3]
7.377±0.193 km[5]
9.27±0.25 km[6]
Rotation period6.546±0.0170 h[7]
6.558 h[8]
6.55836±0.00005 h[9][10]
Geometric albedo0.144±0.009[6]
0.220±0.022[5]
0.23 (assumed)[3]
S[3]
Absolute magnitude (H)12.497±0.008 (R)[7] · 12.87±0.47[11] · 12.92[1][3][5][6]


1192 Prisma, provisional designation 1931 FE, is an elongated Phocaea asteroid from the inner regions of the asteroid belt, approximately 7 kilometers in diameter. It was discovered by German astronomer Friedrich Schwassmann at the Bergedorf Observatory in Hamburg on 17 March 1931.[12] The asteroid was named after the Bergedorf Spectral Catalogue, an astronomical catalog.[2]

Classification and orbit

Prisma is a member of the Phocaea family (701), a prominent family of S-type asteroids with their largest members being 25 Phocaea and 587 Hypsipyle. There are many Mars-crossers among this family of relatively eccentric inner main-belt asteroids .[13]

The asteroid orbits the Sun at a distance of 1.8–3.0 AU once every 3 years and 8 months (1,329 days). Its orbit has an eccentricity of 0.26 and an inclination of 24° with respect to the ecliptic.[1] The body's observation arc begins at Bergedorf, one week after its official discovery observation.[12]

Physical characteristics

Rotation, shape and pole

Photometric observations of Prisma gave a well defined rotational lightcurve with a period between 6.546 and 6.558 hours and a high brightness variation of 0.85–1.16 magnitude, which strongly indicates that the body has an elongated, non-spheroidal shape ({{{1}}}).[7][8]

A modeled lightcurve based on optical data from a large collaboration network also found a spin axis of (133.0°, −78.0°) in ecliptic coordinates (λ, β) ({{{1}}}).[9][10]

Diameter and albedo

According to the surveys carried out by the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Prisma measures between 7.38 and 9.27 kilometers in diameter and its surface has an albedo between 0.144 and 0.220.[5][6] The Collaborative Asteroid Lightcurve Link assumes a standard albedo of 0.23 and calculates a diameter of 7.22 kilometers based on an absolute magnitude of 12.92.[3]

Naming

This minor planet was named "Prisma" (prism) in honour of the Bergedorf Spectral Catalogue (German: Bergedorfer Spektralkatalog), as prisms are one method of obtaining spectra.[2] The official naming citation was also published in Paul Herget's The Names of the Minor Planets in 1955 (H 111).[2]

References

  1. ↑ 1.0 1.1 1.2 1.3 "JPL Small-Body Database Browser: 1192 Prisma (1931 FE)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2001192. Retrieved 15 August 2017. 
  2. ↑ 2.0 2.1 2.2 2.3 Schmadel, Lutz D. (2007). "(1192) Prisma". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 100. doi:10.1007/978-3-540-29925-7_1193. ISBN 978-3-540-00238-3. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 "LCDB Data for (1192) Prisma". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=1192%7CPrisma. Retrieved 15 August 2017. 
  4. ↑ "Asteroid 1192 Prisma – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. https://sbntools.psi.edu/ferret/SimpleSearch/results.action?targetName=1192+Prisma#Asteroid%201192%20PrismaEAR-A-VARGBDET-5-NESVORNYFAM-V3.0. Retrieved 26 October 2019. 
  5. ↑ 5.0 5.1 5.2 5.3 Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C. et al. (November 2012). "Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids". The Astrophysical Journal Letters 759 (1): 5. doi:10.1088/2041-8205/759/1/L8. Bibcode: 2012ApJ...759L...8M. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2012ApJ...759L...8M. Retrieved 15 August 2017. 
  6. ↑ 6.0 6.1 6.2 6.3 Usui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey". Publications of the Astronomical Society of Japan 63 (5): 1117–1138. doi:10.1093/pasj/63.5.1117. Bibcode: 2011PASJ...63.1117U.  (online, AcuA catalog p. 153)
  7. ↑ 7.0 7.1 7.2 Waszczak, Adam; Chang, Chan-Kao; Ofek, Eran O.; Laher, Russ; Masci, Frank; Levitan, David et al. (September 2015). "Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry". The Astronomical Journal 150 (3): 35. doi:10.1088/0004-6256/150/3/75. Bibcode: 2015AJ....150...75W. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2015AJ....150...75W. Retrieved 15 August 2017. 
  8. ↑ 8.0 8.1 Binzel, R. P.; Mulholland, J. D. (December 1983). "A photoelectric lightcurve survey of small main belt asteroids". Icarus 56 (3): 519–533. doi:10.1016/0019-1035(83)90170-7. ISSN 0019-1035. Bibcode: 1983Icar...56..519B. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=1983Icar...56..519B. Retrieved 15 August 2017. 
  9. ↑ 9.0 9.1 Hanus, J.; Broz, M.; Durech, J.; Warner, B. D.; Brinsfield, J.; Durkee, R. et al. (November 2013). "An anisotropic distribution of spin vectors in asteroid families". Astronomy and Astrophysics 559: 19. doi:10.1051/0004-6361/201321993. Bibcode: 2013A&A...559A.134H. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2013A&A...559A.134H. Retrieved 15 August 2017. 
  10. ↑ 10.0 10.1 Hanus, J.; Durech, J.; Oszkiewicz, D. A.; Behrend, R.; Carry, B.; Delbo, M. et al. (February 2016). "New and updated convex shape models of asteroids based on optical data from a large collaboration network". Astronomy and Astrophysics 586: 24. doi:10.1051/0004-6361/201527441. Bibcode: 2016A&A...586A.108H. 
  11. ↑ Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus 261: 34–47. doi:10.1016/j.icarus.2015.08.007. Bibcode: 2015Icar..261...34V. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2015Icar..261...34V. Retrieved 15 August 2017. 
  12. ↑ 12.0 12.1 "1192 Prisma (1931 FE)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=1192. Retrieved 15 August 2017. 
  13. ↑ Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131. Bibcode: 2015aste.book..297N. 

External links



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:1192_Prisma&oldid=3340804"