 | |
| Discovery [1] [2] | |
|---|---|
| Discovered by | NEAT |
| Discovery site | Haleakala Obs. |
| Discovery date | 9 August 1996 |
| Designations | |
| 1996 PW | |
|
TNO
[3] ·
damocloid
[4]
[5] distant [1] · unusual [6] | |
| Orbital characteristics [3] | |
| Epoch 27 April 2019 ( JD 2458600.5) | |
| Uncertainty parameter 2 | |
| Observation arc | 1.39 yr (506 d) |
| Aphelion | 504.23 AU |
| Perihelion | 2.4933 AU |
| 253.36 AU | |
| Eccentricity | 0.9902 |
| 4033 yr (1,473,017 d) | |
| 2.0281 ° | |
| 0° 0m 0.72s / day | |
| Inclination | 29.956° |
| 144.38° | |
| 181.60° | |
| TJupiter | 1.7130 |
| Physical characteristics | |
Mean diameter | 7
km
[4] 8 km (est. at 0.15) [2] 15 km (est. at 0.04) [2] |
| 35.44 h [7] [8] | |
|
Ld (
SMASS)
[3]
[7]
[9] D [8] [10] B–R = 0.56±0.04 V–I = 1.03±0.06 V–J = 1.80±0.05 V–H = 2.19±0.05 V–K = 2.32±0.05 [8] | |
| 14.0 [1] [3] | |
1996 PW is an exceptionally eccentric trans-Neptunian object and damocloid on an orbit typical of long-period comets but one that showed no sign of cometary activity around the time it was discovered. [8] The unusual object measures approximately 10 kilometers (6 miles) in diameter and has a rotation period of 35.4 hours and likely an elongated shape. [7]
Description
1996 PW orbits the Sun at a distance of 2.5–504 AU once every 4,033 years ( semi-major axis of 253 AU). Its orbit has an eccentricity of 0.99 and an inclination of 30 ° with respect to the ecliptic. [3]
Simulations indicate that it has most likely come from the Oort cloud, with a roughly equal probability of being an extinct comet and a rocky body that was originally scattered into the Oort cloud. The discovery of 1996 PW prompted theoretical research that suggests that roughly 1 to 2 percent of the Oort cloud objects are rocky. [2] [10]
1996 PW was first observed on 9 August 1996 by the Near-Earth Asteroid Tracking (NEAT) automated search camera on Haleakala Observatory, Hawaii. It is the first object that is not an active comet discovered on an orbit typical of long-period comets. [2]
1996 PW has a rotation period of 35.44±0.02 hours and a double-peaked lightcurve with a high amplitude of 0.44±0.03 magnitude ( U=3). [7] [8] Its spectrum is moderately red and featureless, [11] typical of D-type asteroids and bare comet nuclei. [8] [10] [11] Its spectrum suggests an extinct comet. [11] The upper limit on 1996 PW's dust production is 0.03 kg/ s. [8]
See also
References
- ^ a b c "1996 PW". Minor Planet Center. Retrieved 17 January 2018.
- ^ a b c d e Weissman, Paul R.; Lecison, Harold F. (March 1997). "Origin and evolution of the unusual object 1996 PW". The Astrophysical Journal. 488 (2): 529. Bibcode: 1997LPI....28.1529W. doi: 10.1086/310940.
- ^ a b c d e "JPL Small-Body Database Browser: (1996 PW)" (1997-12-28 last obs.). Jet Propulsion Laboratory. Retrieved 17 January 2018.
- ^ a b Johnston, Wm. Robert (15 October 2017). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 17 January 2018.
- ^ Akimasa Nakamura (2 May 2009). "Table of Damocloid objects, or Oort cloud asteroids". Lowell Observatory. Retrieved 17 January 2018.
- ^ "List Of Other Unusual Objects". Minor Planet Center. Retrieved 14 November 2018.
- ^ a b c d "LCDB Data for (1996+PW)". Asteroid Lightcurve Database (LCDB). Retrieved 20 November 2018.
- ^ a b c d e f g Davies, John K.; McBride, Neil; Green, Simon F.; Mottola, Stefano; Carsenty, Uri; Basran, Devinder; et al. (April 1998). "The Lightcurve and Colors of Unusual Minor Planet 1996 PW". Icarus. 132 (2): 418–430. Bibcode: 1998Icar..132..418D. doi: 10.1006/icar.1998.5888.
- ^ Bus, Schelte J.; Binzel, Richard P. (July 2002). "Phase II of the Small Main-Belt Asteroid Spectroscopic Survey. A Feature-Based Taxonomy" (PDF). Icarus. 158 (1): 146–177. Bibcode: 2002Icar..158..146B. doi: 10.1006/icar.2002.6856. Archived from the original (PDF) on 23 September 2015. Retrieved 20 November 2018.
- ^ a b c Toth, Imre (December 2005). "Connections between asteroids and cometary nuclei". Asteroids. 1: 67–96. Bibcode: 2006IAUS..229...67T. doi: 10.1017/S174392130500668X.
- ^ a b c Hicks, M. D.; Buratti, B. J.; Newburn, R. L.; Rabinowitz, D. L. (February 2000). "Physical Observations of 1996 PW and 1997 SE5: Extinct Comets or D-Type Asteroids?". Icarus. 143 (2): 354–359. Bibcode: 2000Icar..143..354H. doi: 10.1006/icar.1999.6258.
External links
- 1996 PW, Small Bodies Data Ferret
- 1996 PW at AstDyS-2, Asteroids—Dynamic Site
- 1996 PW at the JPL Small-Body Database
|
| |
| Discovery [1] [2] | |
|---|---|
| Discovered by | NEAT |
| Discovery site | Haleakala Obs. |
| Discovery date | 9 August 1996 |
| Designations | |
| 1996 PW | |
|
TNO
[3] ·
damocloid
[4]
[5] distant [1] · unusual [6] | |
| Orbital characteristics [3] | |
| Epoch 27 April 2019 ( JD 2458600.5) | |
| Uncertainty parameter 2 | |
| Observation arc | 1.39 yr (506 d) |
| Aphelion | 504.23 AU |
| Perihelion | 2.4933 AU |
| 253.36 AU | |
| Eccentricity | 0.9902 |
| 4033 yr (1,473,017 d) | |
| 2.0281 ° | |
| 0° 0m 0.72s / day | |
| Inclination | 29.956° |
| 144.38° | |
| 181.60° | |
| TJupiter | 1.7130 |
| Physical characteristics | |
Mean diameter | 7
km
[4] 8 km (est. at 0.15) [2] 15 km (est. at 0.04) [2] |
| 35.44 h [7] [8] | |
|
Ld (
SMASS)
[3]
[7]
[9] D [8] [10] B–R = 0.56±0.04 V–I = 1.03±0.06 V–J = 1.80±0.05 V–H = 2.19±0.05 V–K = 2.32±0.05 [8] | |
| 14.0 [1] [3] | |
1996 PW is an exceptionally eccentric trans-Neptunian object and damocloid on an orbit typical of long-period comets but one that showed no sign of cometary activity around the time it was discovered. [8] The unusual object measures approximately 10 kilometers (6 miles) in diameter and has a rotation period of 35.4 hours and likely an elongated shape. [7]
Description
1996 PW orbits the Sun at a distance of 2.5–504 AU once every 4,033 years ( semi-major axis of 253 AU). Its orbit has an eccentricity of 0.99 and an inclination of 30 ° with respect to the ecliptic. [3]
Simulations indicate that it has most likely come from the Oort cloud, with a roughly equal probability of being an extinct comet and a rocky body that was originally scattered into the Oort cloud. The discovery of 1996 PW prompted theoretical research that suggests that roughly 1 to 2 percent of the Oort cloud objects are rocky. [2] [10]
1996 PW was first observed on 9 August 1996 by the Near-Earth Asteroid Tracking (NEAT) automated search camera on Haleakala Observatory, Hawaii. It is the first object that is not an active comet discovered on an orbit typical of long-period comets. [2]
1996 PW has a rotation period of 35.44±0.02 hours and a double-peaked lightcurve with a high amplitude of 0.44±0.03 magnitude ( U=3). [7] [8] Its spectrum is moderately red and featureless, [11] typical of D-type asteroids and bare comet nuclei. [8] [10] [11] Its spectrum suggests an extinct comet. [11] The upper limit on 1996 PW's dust production is 0.03 kg/ s. [8]
See also
References
- ^ a b c "1996 PW". Minor Planet Center. Retrieved 17 January 2018.
- ^ a b c d e Weissman, Paul R.; Lecison, Harold F. (March 1997). "Origin and evolution of the unusual object 1996 PW". The Astrophysical Journal. 488 (2): 529. Bibcode: 1997LPI....28.1529W. doi: 10.1086/310940.
- ^ a b c d e "JPL Small-Body Database Browser: (1996 PW)" (1997-12-28 last obs.). Jet Propulsion Laboratory. Retrieved 17 January 2018.
- ^ a b Johnston, Wm. Robert (15 October 2017). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 17 January 2018.
- ^ Akimasa Nakamura (2 May 2009). "Table of Damocloid objects, or Oort cloud asteroids". Lowell Observatory. Retrieved 17 January 2018.
- ^ "List Of Other Unusual Objects". Minor Planet Center. Retrieved 14 November 2018.
- ^ a b c d "LCDB Data for (1996+PW)". Asteroid Lightcurve Database (LCDB). Retrieved 20 November 2018.
- ^ a b c d e f g Davies, John K.; McBride, Neil; Green, Simon F.; Mottola, Stefano; Carsenty, Uri; Basran, Devinder; et al. (April 1998). "The Lightcurve and Colors of Unusual Minor Planet 1996 PW". Icarus. 132 (2): 418–430. Bibcode: 1998Icar..132..418D. doi: 10.1006/icar.1998.5888.
- ^ Bus, Schelte J.; Binzel, Richard P. (July 2002). "Phase II of the Small Main-Belt Asteroid Spectroscopic Survey. A Feature-Based Taxonomy" (PDF). Icarus. 158 (1): 146–177. Bibcode: 2002Icar..158..146B. doi: 10.1006/icar.2002.6856. Archived from the original (PDF) on 23 September 2015. Retrieved 20 November 2018.
- ^ a b c Toth, Imre (December 2005). "Connections between asteroids and cometary nuclei". Asteroids. 1: 67–96. Bibcode: 2006IAUS..229...67T. doi: 10.1017/S174392130500668X.
- ^ a b c Hicks, M. D.; Buratti, B. J.; Newburn, R. L.; Rabinowitz, D. L. (February 2000). "Physical Observations of 1996 PW and 1997 SE5: Extinct Comets or D-Type Asteroids?". Icarus. 143 (2): 354–359. Bibcode: 2000Icar..143..354H. doi: 10.1006/icar.1999.6258.
External links
- 1996 PW, Small Bodies Data Ferret
- 1996 PW at AstDyS-2, Asteroids—Dynamic Site
- 1996 PW at the JPL Small-Body Database