Astronomy:7604 Kridsadaporn

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7604 Kridsadaporn
Orbital trajectory of 7604 Kridsadaporn.png
Orbital diagram of Kridsadaporn
Discovery [1]
Discovered byR. H. McNaught
Discovery siteSiding Spring Obs.
Discovery date31 August 1995
Designations
(7604) Kridsadaporn
Named afterKridsadaporn Ritsmitchai [1]
(Thai astronomer)
1995 QY2 · 1984 QD1
1991 CF3
Minor planet categoryMars-crosser [1][2]
unusual [3] · ACO [4][5]
Orbital characteristics [2]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 0
Observation arc33.89 yr (12,379 d)
|{{{apsis}}}|helion}}4.8989 AU
|{{{apsis}}}|helion}}1.3266 AU
3.1127 AU
Eccentricity0.5738
Orbital period5.49 yr (2,006 d)
Mean anomaly85.061°
Mean motion0° 10m 46.2s / day
Inclination20.449°
Longitude of ascending node147.24°
266.26°
Earth MOID0.522 AU (203 LD)
TJupiter2.8590
Physical characteristics
Mean diameter12 km (est. at 0.057)[6]
SMASS = C [2][7]
Absolute magnitude (H)13.3[1][2]


7604 Kridsadaporn, provisional designation 1995 QY2, is an unusual, carbonaceous asteroid and Mars-crosser on a highly eccentric orbit from the outer regions of the asteroid belt, approximately 12 kilometers (7.5 miles) in diameter. It was discovered on 31 August 1995, by Australian astronomer Robert McNaught at Siding Spring Observatory near Coonabarabran, Australia. Due to its particular orbit, the C-type asteroid belongs to MPC's list of "other" unusual objects,[3] and has been classified as an "asteroid in cometary orbit", or ACO.[4][5] The asteroid was named in memory of Thai astronomer Kridsadaporn Ritsmitchai.[1]

Discovery and naming

Kridsadaporn was discovered using the 0.5-m Uppsala Schmidt Telescope, as part of the Siding Spring Survey, which itself is part of a broader network of Near-Earth object search programs. The then-unnamed asteroid was initially assigned the provisional designation 1995 QY2. In April 2005 it was renamed by its discoverer (Robert McNaught) in honour of Kridsadaporn Ritsmitchai, a then recently deceased friend and colleague at the Research School of Astronomy and Astrophysics at the Australian National University, who worked and resided at Siding Spring Observatory. The official naming citation was published by the Minor Planet Center on 7 April 2005 (M.P.C. 53953).[8]

Context

An approximation known as the Tisserand criteria (T) is applied to cometary encounters with planets (such as Jupiter) and used to describe their orbital inter-relationship.[9] Asteroidal-appearing bodies in elliptical orbits with Jovian Tisserand parameters Tj < 3 only began to appear in search programs in the mid-1980s – Kridsadaporn's Jovian Tisserand parameter is Tj = 2.858.[2] Before this, the failure to identify these objects was used as an argument against the existence of extinct cometary nuclei. Over the past two decades, an increasing number of asteroids, based upon their orbital and physical characteristics, have been suggested as extinct or dormant comets candidates. It is now considered likely that within the asteroid population there exist a significant number of dormant or extinct comets.[10]

More recently, Kridsadaporn has received closer attention after having been included in a number of studies relating to the analysis of spectral properties of asteroids in cometary orbits (ACOs);[5][11] and, collisional activation processes, and the dynamic and physical properties of ACOs.[4][12] The investigation of ACOs is considered important in the understanding of formation processes of cometary dust mantles and the end states of comets, so as to determine the population of Jupiter-family comets, and, to also understand the dynamical processes involved in the transport mechanism of asteroids from typical asteroidal orbits to cometary-like ones.[5]

In earlier studies, ACOs have sometimes been referred to as cometary asteroids or comet-asteroid transition objects.[12]

Orbit

Kridsadaporn orbits the Sun at a distance of 1.3–4.9 AU once every 5 years and 6 months (2,006 days; semi-major axis of 3.11 AU). Its orbit has a high eccentricity of 0.57 and an inclination of 20° with respect to the ecliptic.[2] Its elliptical orbit has similar orbital characteristics to those of the Jupiter-family comets which populate the Jovian Tisserand invariant range between 2 and 3, which supports the scenario that a significant number of asteroids in cometary orbits are extinct or dormant cometary candidates.[4]

Mars-crossing orbit

Kridsadaporn is amongst another group of bodies [Mars-crossing (MC) and/or near-Earth object (NEO) populations] that may have originated from the main asteroid belt as fragments injected into a mean-motion resonance or secular resonance, developing increasingly higher orbital eccentricity over time resulting in the perihelion distance becoming smaller than the aphelion distances of the inner planets. At their birth, near-earth asteroids (NEAs) and MC orbits are in resonance, and when their orbital eccentricity becomes large enough, to the point that their orbits cross those of the inner planets, their orbits then become modified in a random-walk fashion. This results in a complex interplay between planetary encounters and resonances which may lead to a range of unexpected outcomes including cometary-type orbits; solar collisions; or, eventual ejection from the Solar System.[12][13]

Orbital evolution

Detailed investigations into Kridsadaporn's dynamic evolution have been carried out by creating 15 "clone" orbits, integrated forward over a period of 12 million years, by changing the last digit of its orbital parameters. Nine (9) clones demonstrated moderate chaotic behavior jumping between the Jovian mean-motion resonances of 15:7, 9:4, and 11:5 with some orbits becoming Earth-crossers within the integration period. The remaining six (6) clones grew in orbital eccentricity until becoming Jupiter-crossers, and then, behaving as Jupiter-family comets, they were ejected from the Solar System over periods in the order of 105 years.[12]

There are several prominent dips in the distribution of asteroids in the main belt. These gaps are more sparingly populated with objects of higher orbital eccentricity. Known as Kirkwood gaps, these dips in distribution density correspond to the location of orbital resonances with Jupiter. Objects with eccentric orbits continue to increase in orbital eccentricity over longer time-scales to eventually break out of resonance due to close encounters with a major planet.[14] Kridsadaporn, with a semi-major axis of 3.11 AU,[2] corresponds to a very narrow gap associated with the 11:7 resonance[12] within a series of weaker and less sculpted gaps.

Physical characteristics

In the SMASS classification, Kridsadaporn is a common, carbonaceous C-type asteroid.[2][7]

A number of studies[5][11] included Kridsadaporn within a sample of asteroids in cometary orbits in order to understand the relationships in spectral characteristics between ACOs, the Jupiter-family comets, and the outer main belt asteroids. The only finding was that comets present neutral or red feature-less spectra.[5] Earlier studies[15] suggested that comets in all stages of evolution - active; dormant; and, dead - were very dark, often reddish, objects with spectra similar to D-type, P-type and C-type asteroids of the outer Solar System with probably carbonaceous dust containing reddish organic compounds controlling their colour and albedo characteristics.[5]

Origins of ACO objects

Studies analyzing the albedo distribution of a sample of asteroids in cometary orbits,[16] found in general that they exhibit lower albedos than objects with Tj > 3 and further concluded that all ACOs in that sample with Tj < 2.6 had albedos pV < 0.075 - similar to those measured for cometary nuclei - suggesting cometary origins.[5]

A sample of objects, which included Kridsadaporn, was used in a study[5] of the relationship between the Jovian Tisserand invariant and spectral properties of asteroids in cometary orbits, which determined that all observed ACOs within the sample with Tj < 2.9 were feature-less. Kridsadaporn, with its Jovian Tisserand invariant of 2.858,[2] falls within the feature-less (without bands) comet-like spectral group. These studies also concluded that ACOs with featured spectra (with bands) typical of the main belt had Tj ≥ 2.9 while those with Tj < 2.9 demonstrated comet-like spectra, suggesting that the subsample of ACOs with 2.9 ≤ Tj ≤ 3.0 could be populated by a large fraction of interlopers from the inner part of the belt.[4]

Kridsadaporn has a perihelion distance q = 1.3224 AU.[2] A study of the relationship between the size distribution profile and perihelion distances of ACOs[17] concluded that a sub-sample of ACOs with a perihelion distance q > 1.3 AU had a size distribution profile similar to that of the Jupiter family comets, suggesting that sub-sample to be composed of a significant fraction of dormant comets, while a large fraction of ACOs with q < 1.3 AU could more likely be scattered objects from the outer main belt.[4]

Objects with a Jovian Tisserand invariant Tj ≤ 3 and taxonomic properties consistent with a low albedo, however, are not enough to imply that they are dormant or extinct comets. The fraction of low albedo, Tj ≤ 3, objects actually being dormant or extinct comets is estimated to be 65% ± 10%.[11]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 "7604 Kridsadaporn (1995 QY2)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=7604. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 2.8 2.9 "JPL Small-Body Database Browser: 7604 Kridsadaporn (1995 QY2)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2007604. 
  3. ↑ 3.0 3.1 "List Of Other Unusual Objects". Minor Planet Center. 14 November 2018. https://www.minorplanetcenter.net/iau/lists/t_others.html. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 Díaz, C. G.; Gil-Hutton, R. (August 2008). "Collisional activation of asteroids in cometary orbits". Astronomy and Astrophysics 487 (1): 363–367. doi:10.1051/0004-6361:20079236. Bibcode: 2008A&A...487..363D. https://www.aanda.org/articles/aa/pdf/2008/31/aa9236-07.pdf. Retrieved 14 November 2018. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 5.8 Licandro, J.; Alvarez-Candal, A.; de León, J.; Pinilla-Alonso, N.; Lazzaro, D.; Campins, H. (April 2008). "Spectral properties of asteroids in cometary orbits". Astronomy and Astrophysics 481 (3): 861–877. doi:10.1051/0004-6361:20078340. Bibcode: 2008A&A...481..861L. http://www.aanda.org/index.php?option=com_article&access=standard&Itemid=129&url=/articles/aa/pdf/2008/31/aa9236-07.pdf. Retrieved 14 November 2018. 
  6. ↑ "Asteroid Size Estimator". CNEOS NASA/JPL. https://cneos.jpl.nasa.gov/tools/ast_size_est.html. 
  7. ↑ 7.0 7.1 "Asteroid 7604 Kridsadaporn". Small Bodies Data Ferret. https://sbntools.psi.edu/ferret/SimpleSearch/results.action?targetName=7604+Kridsadaporn. 
  8. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. https://www.minorplanetcenter.net/iau/ECS/MPCArchive/MPCArchive_TBL.html. 
  9. ↑ Brant, John C.; Chapman, Robert D. (2004), Introduction to asteroids, Cambridge University Press, p. 69, ISBN 978-0-521-00466-4 
  10. ↑ Weissman, Paul R.; A'Hearn, M. F.; McFadden, L. A.; Rickman, H. (December 1988). "Evolution of comets into asteroids". Asteroids II; Proceedings of the Conference, Tucson, AZ, Mar. 8-11, 1988 (A90-27001 10-91): 880–920. Bibcode: 1989aste.conf..880W. 
  11. ↑ 11.0 11.1 11.2 Binzel, Richard P.; Rivkin, Andrew S.; Stuart, J. Scott; Harris, Alan W.; Bus, Schelte J.; Burbine, Thomas H. (August 2004). "Observed spectral properties of near-Earth objects: results for population distribution, source regions, and space weathering processes". Icarus 170 (2): 259–294. doi:10.1016/j.icarus.2004.04.004. Bibcode: 2004Icar..170..259B. http://www.mtholyoke.edu/courses/tburbine/tomburbine/binzel.2004.pdf. Retrieved 14 November 2018. 
  12. ↑ 12.0 12.1 12.2 12.3 12.4 di Martino, M.; Carusi, A.; Dotto, E.; Lazzarin, M.; Marzari, F.; Migliorini, F. (January 1998). "Dynamical and physical properties of comet--asteroid transition objects". Astronomy and Astrophysics 329: 1145–1151. Bibcode: 1998A&A...329.1145D. 
  13. ↑ Froeschle, Ch.; Hahn, G.; Gonczi, R.; Morbidelli, A.; Farinella, P. (September 1995). "Secular resonances and the dynamics of Mars-crossing and Near-Earth asteroids.". Icarus 117 (1): 45–61. doi:10.1006/icar.1995.1141. Bibcode: 1995Icar..117...45F. 
  14. ↑ Tsiganis, Kleomenis; Varvoglis, Harry; Hadjidemetriou, John D. (October 2002). "Stable Chaos versus Kirkwood Gaps in the Asteroid Belt: A Comparative Study of Mean Motion Resonances". Icarus 159 (2): 284–299. doi:10.1006/icar.2002.6927. Bibcode: 2002Icar..159..284T. http://www.astro.auth.gr/~varvogli/kirkwood-gaps.pdf. Retrieved 15 November 2018. 
  15. ↑ Hartmann, W. K.; Tholen, D. J.; Cruikshank, D. P. (January 1987). "The relationship of active comets, 'extinct' comets, and dark asteroids". Icarus 69 (1): 33–50. doi:10.1016/0019-1035(87)90005-4. ISSN 0019-1035. Bibcode: 1987Icar...69...33H. 
  16. ↑ Fernández, Yanga R.; Jewitt, David C.; Sheppard, Scott S. (July 2005). "Albedos of Asteroids in Comet-Like Orbits". The Astronomical Journal 130 (1): 308–318. doi:10.1086/430802. Bibcode: 2005AJ....130..308F. 
  17. ↑ Alvarez-Candal, A.; Licandro, J. (November 2006). "The size distribution of asteroids in cometary orbits and related populations". Astronomy and Astrophysics 458 (3): 1007–1011. doi:10.1051/0004-6361:20064971. Bibcode: 2006A&A...458.1007A. https://www.aanda.org/articles/aa/pdf/2006/42/aa4971-06.pdf. Retrieved 14 November 2018. 

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