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1192 Prisma
Modelled shape of Prisma from its lightcurve
Discovery [1]
Discovered by A. Schwassmann
Discovery site Bergedorf Obs.
Discovery date17 March 1931
Designations
(1192) Prisma
Named after
Bergedorf Spectral Catalogue
( astronomical catalog) [2]
1931 FE
main-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)
Aphelion2.9762 AU
Perihelion1.7561 AU
2.3661 AU
Eccentricity0.2578
3.64 yr (1,329 days)
297.62 °
0° 16m 14.88s / day
Inclination23.902°
1.3517°
131.44°
Physical characteristics
Dimensions7.22 km (calculated) [3]
7.377±0.193 km [5]
9.27±0.25 km [6]
6.546±0.0170 h [7]
6.558 h [8]
6.55836±0.00005 h [9] [10]
0.144±0.009 [6]
0.220±0.022 [5]
0.23 (assumed) [3]
S [3]
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 ( U=3/3). [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) ( Q=n.a.). [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. ^ a b c d "JPL Small-Body Database Browser: 1192 Prisma (1931 FE)" (2016-12-25 last obs.). Jet Propulsion Laboratory. Retrieved 15 August 2017.
  2. ^ a b c d 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. ^ a b c d e f "LCDB Data for (1192) Prisma". Asteroid Lightcurve Database (LCDB). Retrieved 15 August 2017.
  4. ^ "Asteroid 1192 Prisma – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 26 October 2019.
  5. ^ a b c d 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. arXiv: 1209.5794. Bibcode: 2012ApJ...759L...8M. doi: 10.1088/2041-8205/759/1/L8. Retrieved 15 August 2017.
  6. ^ a b c d 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. Bibcode: 2011PASJ...63.1117U. doi: 10.1093/pasj/63.5.1117. ( online, AcuA catalog p. 153)
  7. ^ a b c 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. arXiv: 1504.04041. Bibcode: 2015AJ....150...75W. doi: 10.1088/0004-6256/150/3/75. Retrieved 15 August 2017.
  8. ^ a b Binzel, R. P.; Mulholland, J. D. (December 1983). "A photoelectric lightcurve survey of small main belt asteroids". Icarus. 56 (3): 519–533. Bibcode: 1983Icar...56..519B. doi: 10.1016/0019-1035(83)90170-7. ISSN  0019-1035. Retrieved 15 August 2017.
  9. ^ a b 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. arXiv: 1309.4296. Bibcode: 2013A&A...559A.134H. doi: 10.1051/0004-6361/201321993. Retrieved 15 August 2017.
  10. ^ a b 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. arXiv: 1510.07422. Bibcode: 2016A&A...586A.108H. doi: 10.1051/0004-6361/201527441.
  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. arXiv: 1506.00762. Bibcode: 2015Icar..261...34V. doi: 10.1016/j.icarus.2015.08.007. Retrieved 15 August 2017.
  12. ^ a b "1192 Prisma (1931 FE)". Minor Planet Center. 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. arXiv: 1502.01628. Bibcode: 2015aste.book..297N. doi: 10.2458/azu_uapress_9780816532131-ch016. ISBN  9780816532131.

External links

Retrieved from " https://en.wikipedia.org/?title=1192_Prisma&oldid=1195680249"
From Wikipedia, the free encyclopedia

1192 Prisma
Modelled shape of Prisma from its lightcurve
Discovery [1]
Discovered by A. Schwassmann
Discovery site Bergedorf Obs.
Discovery date17 March 1931
Designations
(1192) Prisma
Named after
Bergedorf Spectral Catalogue
( astronomical catalog) [2]
1931 FE
main-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)
Aphelion2.9762 AU
Perihelion1.7561 AU
2.3661 AU
Eccentricity0.2578
3.64 yr (1,329 days)
297.62 °
0° 16m 14.88s / day
Inclination23.902°
1.3517°
131.44°
Physical characteristics
Dimensions7.22 km (calculated) [3]
7.377±0.193 km [5]
9.27±0.25 km [6]
6.546±0.0170 h [7]
6.558 h [8]
6.55836±0.00005 h [9] [10]
0.144±0.009 [6]
0.220±0.022 [5]
0.23 (assumed) [3]
S [3]
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 ( U=3/3). [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) ( Q=n.a.). [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. ^ a b c d "JPL Small-Body Database Browser: 1192 Prisma (1931 FE)" (2016-12-25 last obs.). Jet Propulsion Laboratory. Retrieved 15 August 2017.
  2. ^ a b c d 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. ^ a b c d e f "LCDB Data for (1192) Prisma". Asteroid Lightcurve Database (LCDB). Retrieved 15 August 2017.
  4. ^ "Asteroid 1192 Prisma – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 26 October 2019.
  5. ^ a b c d 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. arXiv: 1209.5794. Bibcode: 2012ApJ...759L...8M. doi: 10.1088/2041-8205/759/1/L8. Retrieved 15 August 2017.
  6. ^ a b c d 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. Bibcode: 2011PASJ...63.1117U. doi: 10.1093/pasj/63.5.1117. ( online, AcuA catalog p. 153)
  7. ^ a b c 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. arXiv: 1504.04041. Bibcode: 2015AJ....150...75W. doi: 10.1088/0004-6256/150/3/75. Retrieved 15 August 2017.
  8. ^ a b Binzel, R. P.; Mulholland, J. D. (December 1983). "A photoelectric lightcurve survey of small main belt asteroids". Icarus. 56 (3): 519–533. Bibcode: 1983Icar...56..519B. doi: 10.1016/0019-1035(83)90170-7. ISSN  0019-1035. Retrieved 15 August 2017.
  9. ^ a b 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. arXiv: 1309.4296. Bibcode: 2013A&A...559A.134H. doi: 10.1051/0004-6361/201321993. Retrieved 15 August 2017.
  10. ^ a b 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. arXiv: 1510.07422. Bibcode: 2016A&A...586A.108H. doi: 10.1051/0004-6361/201527441.
  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. arXiv: 1506.00762. Bibcode: 2015Icar..261...34V. doi: 10.1016/j.icarus.2015.08.007. Retrieved 15 August 2017.
  12. ^ a b "1192 Prisma (1931 FE)". Minor Planet Center. 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. arXiv: 1502.01628. Bibcode: 2015aste.book..297N. doi: 10.2458/azu_uapress_9780816532131-ch016. ISBN  9780816532131.

External links

Retrieved from " https://en.wikipedia.org/?title=1192_Prisma&oldid=1195680249"

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