(24835) 1995 SM55

Last updated

(24835) 1995 SM55
Discovery [1] [2]
Discovered by N. Danzl
Discovery site Spacewatch
Kitt Peak National Obs.
Discovery date19 September 1995
Designations
(24835) 1995 SM55
1995 SM55
TNO [1]  · Haumea [3]  · cubewano [4] [5]
Scat-Ext [6]  · distant [2]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 3
Observation arc 34.29 yr (12,523 days)
Aphelion 45.870 AU
Perihelion 37.386 AU
41.628 AU
Eccentricity 0.1019
268.59 yr (98,101 days)
329.45°
0° 0m 13.32s / day
Inclination 27.096°
21.109°
≈ 7 June 2040 [7]
±5 days
72.600°
Physical characteristics
Mean diameter
173 km(estimate) [3]
519.43 km(derived) [8]
610 km(Haumea-derived) [9]
701 km [4]
704 km(upper limit) [10] [11]
8.08±0.02 h [12]
8.08±0.03 h [13]
0.7 (Haumea-derived) [3]
0.040 [4]
0.067 (at least) [10]
0.10 (assumed) [8]
BBb (suspected) [14]  · C [8]
(Neutral)
B–V = 0.65 [8]
V−R = 0.37 [8]
V−I = 0.710 [8]
4.30±0.02(R) [15]
4.352±0.040(R) [16]
4.490±0.030 [17]
4.54 [8] [18]  ·4.6 [1]  ·4.9 [3]

    (24835) 1995 SM55 (provisional designation 1995 SM55) is a trans-Neptunian object and member of the Haumea family that resides in the Kuiper belt, located in the outermost region of the Solar System. It was discovered on 19 September 1995, by American astronomer Nichole Danzl of the Spacewatch program at Kitt Peak National Observatory near Tucson, Arizona, in the United States. [2] It measures approximately 200 kilometers in diameter and was the second-brightest known object in the Kuiper belt, after Pluto, until 1996 TO66 was discovered.

    Contents

    Origin

    1995 SM55 is a member of the Haumea family. [3] It has the highest collisional velocity, a δv of 123.3 m/s, of all confirmed members. [19] Based on their common pattern of IR water-ice absorptions, neutral visible spectrum [20] and the clustering of their orbital elements, the other KBOs 1996 TO66 , 2002 TX300 , 2003 OP32 and 2005 RR43 all appear to be collisional fragments broken off of the dwarf planet Haumea.

    Naming

    As of 2018, this minor planet has not been named by the Minor Planet Center. [2]

    Orbital diagram

    1995 SM55 among other members of the Haumea family Haumea family orbits.png
    1995 SM55 among other members of the Haumea family

    Related Research Articles

    <span class="mw-page-title-main">Classical Kuiper belt object</span> Kuiper belt object, not controlled by an orbital resonance with Neptune

    A classical Kuiper belt object, also called a cubewano ( "QB1-o"), is a low-eccentricity Kuiper belt object (KBO) that orbits beyond Neptune and is not controlled by an orbital resonance with Neptune. Cubewanos have orbits with semi-major axes in the 40–50 AU range and, unlike Pluto, do not cross Neptune's orbit. That is, they have low-eccentricity and sometimes low-inclination orbits like the classical planets.

    <span class="mw-page-title-main">Trans-Neptunian object</span> Solar system objects beyond Neptune

    A trans-Neptunian object (TNO), also written transneptunian object, is any minor planet in the Solar System that orbits the Sun at a greater average distance than Neptune, which has an orbital semi-major axis of 30.1 astronomical units (au).

    5145 Pholus is an eccentric centaur in the outer Solar System, approximately 180 kilometers in diameter, that crosses the orbit of both Saturn and Neptune. It was discovered on 9 January 1992 by American astronomer David Rabinowitz (uncredited) of UA's Spacewatch survey at the Kitt Peak National Observatory in Arizona, United States. The very reddish object has an elongated shape and a rotation period of 9.98 hours. It was named after the centaur Pholus from Greek mythology.

    8405 Asbolus is a centaur orbiting in the outer Solar System between the orbits of Jupiter and Neptune. It was discovered on 5 April 1995, by James Scotti and Robert Jedicke of Spacewatch (credited) at Kitt Peak Observatory in Arizona, United States. It is named after Asbolus, a centaur in Greek mythology and measures approximately 80 kilometers in diameter.

    <span class="nowrap">(19308) 1996 TO<sub>66</sub></span> Trans-Neptunian object in the Kuiper belt

    (19308) 1996 TO66 (provisional designation 1996 TO66) is a trans-Neptunian object that was discovered in 1996 by Chadwick Trujillo, David Jewitt and Jane Luu. Until 20000 Varuna was discovered, it was the second-largest known object in the Kuiper belt, after Pluto.

    <span class="nowrap">(55565) 2002 AW<sub>197</sub></span> Classical Kuiper belt object

    (55565) 2002 AW197 (provisional designation 2002 AW197) is a classical, non-resonant trans-Neptunian object from the Kuiper belt in the outermost region of the Solar System, also known as a cubewano. With a likely diameter of at least 700 kilometers (430 miles), it is approximately tied with 2002 MS4 and 2013 FY27 (to within measurement uncertainties) as the largest unnamed object in the Solar System. It was discovered at Palomar Observatory in 2002.

    <span class="mw-page-title-main">10199 Chariklo</span> Small body of the outer Solar System

    10199 Chariklo is the largest confirmed centaur. It orbits the Sun between Saturn and Uranus, grazing the orbit of Uranus. On 26 March 2014, astronomers announced the discovery of two rings around Chariklo by observing a stellar occultation, making it the first minor planet known to have rings.

    <span class="mw-page-title-main">10370 Hylonome</span>

    10370 Hylonome (; prov. designation: 1995 DW2) is a minor planet orbiting in the outer Solar System. The dark and icy body belongs to the class of centaurs and measures approximately 72 kilometers (45 miles) in diameter. It was discovered on 27 February 1995, by English astronomer David C. Jewitt and Vietnamese American astronomer Jane Luu at the U.S. Mauna Kea Observatory in Hawaii, and later named after the mythological creature Hylonome.

    <span class="nowrap">(55636) 2002 TX<sub>300</sub></span> Kuiper Belt object

    (55636) 2002 TX300 is a bright Kuiper belt object in the outer Solar System estimated to be about 286 kilometres (178 mi) in diameter. It is a large member of the Haumea family that was discovered on 15 October 2002 by the Near-Earth Asteroid Tracking (NEAT) program.

    <span class="nowrap">(84922) 2003 VS<sub>2</sub></span> Trans-Neptunian object

    (84922) 2003 VS2 is a trans-Neptunian object discovered by the Near Earth Asteroid Tracking program on 14 November 2003. Like Pluto, it is in a 2:3 orbital resonance with Neptune and is thus a plutino. Analysis of light-curve suggests that it is not a dwarf planet.

    (79983) 1999 DF9 (provisional designation 1999 DF9) is a trans-Neptunian object of the Kuiper belt, classified as a non-resonant cubewano, that measures approximately 270 kilometers in diameter.

    <span class="nowrap">(120178) 2003 OP<sub>32</sub></span>

    (120178) 2003 OP32, also written as (120178) 2003 OP32, is a trans-Neptunian object (TNO) that resides in the Kuiper belt. It was discovered on July 26, 2003 by Michael E. Brown, Chad Trujillo and David L. Rabinowitz at Palomar Mountain in California.

    <span class="nowrap">(145453) 2005 RR<sub>43</sub></span>

    (145453) 2005 RR43 (provisional designation 2005 RR43) is a trans-Neptunian object (TNO) estimated to be about 250 km in diameter. It was discovered on 9 September 2005 by Andrew Becker, Andrew Puckett and Jeremy Kubica at Apache Point Observatory in Sunspot, New Mexico.

    <span class="nowrap">(40314) 1999 KR<sub>16</sub></span>

    (40314) 1999 KR16 is a trans-Neptunian object on an eccentric orbit in the outermost region of the Solar System, approximately 254 kilometers (158 miles) in diameter. It was discovered on 16 May 1999, by French astronomer Audrey Delsanti and Oliver Hainaut at ESO's La Silla Observatory in northern Chile. The very reddish object is a dwarf planet candidate and has a rotation period of 11.7 hours.

    <span class="mw-page-title-main">32532 Thereus</span>

    32532 Thereus, provisional designation: 2001 PT13, is a centaur from the outer Solar System, approximately 80 kilometers (50 miles) in diameter. It was discovered on 9 August 2001, by astronomers of the Near-Earth Asteroid Tracking program at the Palomar Observatory in California, United States. This minor planet was named for the phrase thēreios bia 'beastly strength', used to describe centaurs in Greek mythology.

    <span class="mw-page-title-main">Haumea family</span>

    The Haumea or Haumean family is the only identified trans-Neptunian collisional family; that is, the only group of trans-Neptunian objects (TNOs) with similar orbital parameters and spectra that suggest they originated in the disruptive impact of a progenitor body. Calculations indicate that it is probably the only trans-Neptunian collisional family. Members are known as Haumeids.

    (55638) 2002 VE95 (provisional designation 2002 VE95) is a trans-Neptunian object from the outermost region of the Solar System. It was discovered on 14 November 2002, by astronomers with the Near-Earth Asteroid Tracking program at the Palomar Observatory in California, United States. This resonant trans-Neptunian object is a member of the plutino population, locked in a 2:3 resonance with Neptune. The object is likely of primordial origin with a heterogeneous surface and a notably reddish color (RR) attributed to the presence of methanol and tholins. It has a poorly defined rotation period of 6.8 hours and measures approximately 250 kilometers (160 miles) in diameter, too small to be a dwarf planet candidate. As of 2021, it has not yet been named.

    (469306) 1999 CD158 (provisional designation 1999 CD158) is a trans-Neptunian object from the circumstellar disc of the Kuiper belt, located in the outermost region of the Solar System. The relatively bright hot classical Kuiper belt object measures approximately 310 kilometers (190 miles) in diameter. It was discovered on 10 February 1999, by American astronomers Jane Luu, David Jewitt and Chad Trujillo at Mauna Kea Observatories on the Big Island of Hawaii, United States.

    <span class="nowrap">(82158) 2001 FP<sub>185</sub></span>

    (82158) 2001 FP185 (provisional designation 2001 FP185) is a highly eccentric trans-Neptunian object from the scattered disc in the outermost part of the Solar System, approximately 330 kilometers in diameter. It was discovered on 26 March 2001, by American astronomer Marc Buie at Kitt Peak National Observatory in Arizona, United States.

    <span class="nowrap">(416400) 2003 UZ<sub>117</sub></span>

    (416400) 2003 UZ117 (provisional designation 2003 UZ117) is a trans-Neptunian object and suspected member of the Haumea family, located in the Kuiper belt in the outermost region of the Solar System. It was discovered on 24 October 2003, by astronomers of the Spacewatch survey project at Kitt Peak Observatory, Arizona. The object may also be a non-resonant cubewano.

    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 24835 (1995 SM55)" (2016-12-29 last obs.). Jet Propulsion Laboratory . Retrieved 8 February 2018.
    2. 1 2 3 4 "24835 (1995 SM55)". Minor Planet Center. Retrieved 8 February 2018.
    3. 1 2 3 4 5 Michael E. Brown. "How many dwarf planets are there in the outer solar system?". California Institute of Technology . Retrieved 8 February 2018.
    4. 1 2 3 Johnston, Wm. Robert (15 October 2017). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 8 February 2018.
    5. ↑ "MPEC 2009-R09 :Distant Minor Planets (2009 SEPT. 16.0 TT)". IAU Minor Planet Center. 4 September 2009. Retrieved 4 October 2009.
    6. ↑ Marc W. Buie. "Orbit Fit and Astrometric record for 24835" (2004-11-02 using 119 of 123 observations). SwRI (Space Science Department). Retrieved 4 October 2009.
    7. ↑ JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 3-sigma.)
    8. 1 2 3 4 5 6 7 "LCDB Data for (24835)". Asteroid Lightcurve Database (LCDB). Retrieved 8 February 2018.
    9. ↑ "Asteroid Size Estimator". CNEOS NASA/JPL. Retrieved 8 February 2018.
    10. 1 2 Grundy, W. M.; Noll, K. S.; Stephens, D. C. (July 2005). "Diverse albedos of small trans-neptunian objects". Icarus. 176 (1): 184–191. arXiv: astro-ph/0502229 . Bibcode:2005Icar..176..184G. doi:10.1016/j.icarus.2005.01.007. S2CID   118866288.
    11. ↑ John Stansberry; Will Grundy; Mike Brown; Dale Cruikshank; John Spencer; David Trilling; et al. (2007). Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope. arXiv: astro-ph/0702538 . Bibcode:2008ssbn.book..161S.
    12. ↑ Thirouin, Audrey; Sheppard, Scott S.; Noll, Keith S.; Moskovitz, Nicholas A.; Ortiz, Jose Luis; Doressoundiram, Alain (June 2016). "Rotational Properties of the Haumea Family Members and Candidates: Short-term Variability". The Astronomical Journal. 151 (6): 20. arXiv: 1603.04406 . Bibcode:2016AJ....151..148T. doi: 10.3847/0004-6256/151/6/148 . S2CID   118510175.
    13. ↑ Sheppard, Scott S.; Jewitt, David C. (June 2003). "Hawaii Kuiper Belt Variability Project: An Update". Earth, Moon, and Planets. 92 (1): 207–219. Bibcode:2003EM&P...92..207S. doi:10.1023/B:MOON.0000031943.12968.46. S2CID   189905992.
    14. ↑ Belskaya, Irina N.; Barucci, Maria A.; Fulchignoni, Marcello; Dovgopol, Anatolij N. (April 2015). "Updated taxonomy of trans-neptunian objects and centaurs: Influence of albedo". Icarus. 250: 482–491. Bibcode:2015Icar..250..482B. doi:10.1016/j.icarus.2014.12.004.
    15. ↑ Jewitt, David; Peixinho, Nuno; Hsieh, Henry H. (November 2007). "U-Band Photometry of Kuiper Belt Objects". The Astronomical Journal. 134 (5): 2046–2053. Bibcode:2007AJ....134.2046J. doi: 10.1086/522787 .
    16. ↑ Peixinho, N.; Delsanti, A.; Guilbert-Lepoutre, A.; Gafeira, R.; Lacerda, P. (October 2012). "The bimodal colors of Centaurs and small Kuiper belt objects". Astronomy and Astrophysics. 546: 12. arXiv: 1206.3153 . Bibcode:2012A&A...546A..86P. doi:10.1051/0004-6361/201219057. S2CID   55876118.
    17. ↑ Rabinowitz, David L.; Schaefer, Bradley E.; Schaefer, Martha; Tourtellotte, Suzanne W. (October 2008). "The Youthful Appearance of the 2003 EL61 Collisional Family". The Astronomical Journal. 136 (4): 1502–1509. arXiv: 0804.2864 . Bibcode:2008AJ....136.1502R. doi:10.1088/0004-6256/136/4/1502. S2CID   117167835.
    18. ↑ Romanishin, W.; Tegler, S. C. (December 2005). "Accurate absolute magnitudes for Kuiper belt objects and Centaurs". Icarus. 179 (2): 523–526. Bibcode:2005Icar..179..523R. doi:10.1016/j.icarus.2005.06.016.
    19. ↑ Snodgrass, C.; Carry, B.; Dumas, C.; Hainaut, O. (February 2010). "Characterisation of candidate members of (136108) Haumea's family". Astronomy and Astrophysics. 511: 9. arXiv: 0912.3171 . Bibcode:2010A&A...511A..72S. doi:10.1051/0004-6361/200913031. S2CID   62880843.
    20. ↑ Pinilla-Alonso, N.; Licandro, J.; Gil-Hutton, R.; Brunetto, R. (June 2007). "The water ice rich surface of (145453) 2005 RR43: a case for a carbon-depleted population of TNOs?". Astronomy and Astrophysics. 468 (1): L25. arXiv: astro-ph/0703098 . Bibcode:2007A&A...468L..25P. doi:10.1051/0004-6361:20077294. S2CID   18546361.
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