4179 Toutatis

Last updated

4179 Toutatis
Asteroid 4179 Toutatis close-up.jpg
Toutatis imaged by Chang'e 2 during its flyby
Discovery  [1]
Discovered by Christian Pollas
Discovery site Caussols
Discovery date4 January 1989
Designations
(4179) Toutatis
Pronunciation /taʊˈteɪtɪs/
Named after
 Toutatis (Celtic mythology) [2]
  • 1989 AC
  • 1934 CT
Adjectives Toutatian [4]
Orbital characteristics   [3]
Epoch 27 November 2008 (JD  2454797.5)
Uncertainty parameter 0
Observation arc 83.29 yr (30,422 days)
Earliest precovery date10 February 1934
Aphelion 4.1242  AU
Perihelion 0.9399 AU
2.5321 AU
Eccentricity 0.6288
4.03  yr (1,472 days)
5.1220°
0° 14m 40.56s / day
Inclination 0.4460°
124.30°
278.75°
Earth  MOID 0.0064 AU (2.5 LD)
Physical characteristics
Dimensions
  • 4.75 × 1.95 km [5]
  • 4.26 × 2.03 × 1.70 km [6]
Mean diameter
2.45 km [6]
Mass 1.9×1013 kg [7]
Mean density
2.5 g/cm3 [7]
176  h (7.3  d) [8]
0.13 [3]
Sk (SMASSII) [3]
8.8–22.4 [9] [10]
15.30 [3]

    4179 Toutatis (Provisional designation 1989 AC) is an elongated, stony asteroid and slow rotator, [11] classified as a near-Earth object and potentially hazardous asteroid of the Apollo asteroid and Alinda asteroid groups,[ citation needed ] approximately 2.5 kilometers in diameter. Discovered by French astronomer Christian Pollas at Caussols in 1989, the asteroid was named after Toutatis from Celtic mythology. [1] [2]

    Contents

    Toutatis is also a Mars-crosser asteroid with a chaotic orbit produced by a 3:1 resonance with the planet Jupiter, a 1:4 resonance with the planet Earth, and frequent close approaches to the terrestrial planets, including Earth. [12] In December 2012, Toutatis passed within about 18 lunar distances of Earth. The Chinese lunar probe Chang'e 2 flew by the asteroid at a distance of 3.2 kilometers and a relative velocity of 10.73 km/s. [13] Toutatis approached Earth again in 2016, but will not make another notably close approach until 2069. [14]

    Properties

    Toutatis was first sighted on 10 February 1934, as object 1934 CT, but lost soon afterwards. [15] It remained a lost asteroid for several decades until it was rediscovered on 4 January 1989 by French astronomer Christian Pollas, and was named after the Celtic god of tribal protection Toutatis (Teutates). The name of this god is very familiar in France due to the catchphrase Par Toutatis! by the Gauls in the comics Asterix. [16]

    The spectral properties suggest that this is an S-type, or stony asteroid, consisting primarily of silicates. It has a moderate Bond albedo of 0.13. [3] Radar imagery shows that Toutatis is a highly irregular body consisting of two distinct lobes, with maximum widths of about 4.6 km and 2.4 km, respectively. It is hypothesized that Toutatis formed from two originally separate bodies which coalesced at some point (a contact binary), with the resultant asteroid being compared to a rubble pile.

    Its rotation combines two separate periodic motions into a non-periodic result; to someone on the surface of Toutatis, the Sun would seem to rise and set in apparently random locations and at random times at the asteroid's horizon. It has a rotation period around its long axis (Pψ) of 5.38 days. This long axis is precessing with a period (Pφ) of 7.38 days. [17] The asteroid may have lost most of its original angular momentum and entered into this tumbling motion as a result of the YORP effect. [18]

    Orbit

    Animation of 4179 Toutatis's orbit around the Sun .mw-parser-output .legend{page-break-inside:avoid;break-inside:avoid-column}.mw-parser-output .legend-color{display:inline-block;min-width:1.25em;height:1.25em;line-height:1.25;margin:1px 0;text-align:center;border:1px solid black;background-color:transparent;color:black}.mw-parser-output .legend-text{} 4179 Toutatis Sun * Earth * Jupiter Animation of 4179 Toutatis's orbit around Sun.gif
    Animation of 4179 Toutatis's orbit around the Sun
      4179 Toutatis   Sun  ·   Earth  ·   Jupiter

    With a semimajor axis of 2.5294  AU, or roughly 2.5 times the distance between Earth and the Sun, Toutatis has a 3:1 orbital resonance with Jupiter and a near-1:4 resonance with Earth making it a member of the Alinda asteroid group. [12] [19] It thus completes one orbit around the Sun for every 4.02 annual orbits of Earth. The gravitational perturbations caused by frequent close approaches to the terrestrial planets lead to chaotic behavior in the orbit of Toutatis, [20] making precise long-term predictions of its location progressively inaccurate over time. [20] Estimates in 1993 put the Lyapunov time horizon for predictability at around 50 years, [20] after which the uncertainty region becomes larger with each close approach to a planet. Without the perturbations from the terrestrial planets the Lyapunov time would be close to 10,000 years. [20] The initial observations that showed its chaotic behavior were made by Wiśniewski. [21]

    The low inclination (0.47°) of the orbit allows frequent transits, where the inner planets Mercury, Venus, Earth, and Mars can appear to cross the Sun as seen from the perspective of Toutatis. Earth did this in January 2009, July 2012, July 2016 and 2020. [22]

    Close approaches and collision risk

    Close approaches [14]
    YearAU LD
    19850.28109
    19880.1245
    19920.029
    19960.0314
    20000.0729
    20040.014
    20080.0520
    20120.0518
    20160.2598
    20650.36142
    20690.028

    Toutatis makes frequent close approaches to Earth, with a currently minimum possible distance (Earth MOID) of just 0.006  AU (2.3 times as far as the Moon). [3] The approach on 29 September 2004 was particularly close, at 0.0104 AU [23] (within 4 lunar distances) from Earth, presenting a good opportunity for observation, with Toutatis having an apparent magnitude of 8.8 at its brightest. [9] A close approach of 0.0502  AU (7,510,000  km ; 4,670,000  mi ) happened on 9 November 2008. [14] [23] The most recent close approach was on 12 December 2012, at a distance of 0.046 AU (6,900,000 km; 4,300,000 mi), [14] [23] with a magnitude of 10.7. [24] At magnitude 10.7, Toutatis was not visible to the naked eye, but just visible to experienced observers using high-end binoculars. During the 2012 encounter Toutatis was recovered on 21 May 2012, by the Siding Spring Survey at apparent magnitude 18.9. [25] A close approach will be 5 November 2069, at 0.01985 AU (2,970,000 km). [14]

    Given that Toutatis makes many close approaches to Earth, such as in 1992, 1996, 2000, 2004, 2008, 2012, and 2016, it is listed as a potentially hazardous object. [14] With an uncertainty parameter of 0, [3] the orbit of Toutatis is very well determined for the next few hundred years. [14] The probability of the orbit intersecting Earth is essentially zero for at least the next six centuries. [26] The likelihood of collision in the distant future is considered to be very small. [27] As a planet-crossing asteroid, Toutatis is likely to be ejected from the inner Solar System within a few million years. In 2004 a chain e-mail falsely claimed that Toutatis had a 63% chance of impacting Earth then. In fact, Toutatis passed by at 1.5 million kilometres, or about four Earth–Moon distances, as predicted. [28]

    In 2006 Toutatis came closer than 2 AU to Jupiter; its orbit lies inside of Jupiter's. [14] In the 2100s, it will approach Jupiter many times at a similar distance. [14]

    History of close approaches of large near-Earth objects since 1908 (A)
    PHA DateApproach distance (lunar dist.) Abs.
    mag
    ( H )    		Diameter (C)
    (m)    		Ref (D)
    Nomi-
    nal(B)    		Mini-
    mum    		Maxi-
    mum
    (33342) 1998 WT24 1908-12-163.5423.5373.54717.9556–1795 data
    (458732) 2011 MD5 1918-09-170.9110.9090.91317.9556–1795 data
    (7482) 1994 PC1 1933-01-172.9272.9272.92816.8749–1357 data
    69230 Hermes 1937-10-301.9261.9261.92717.5668–2158 data
    69230 Hermes1942-04-261.6511.6511.65117.5668–2158 data
    (137108) 1999 AN10 1946-08-072.4322.4292.43517.9556–1795 data
    (33342) 1998 WT24 1956-12-163.5233.5233.52317.9556–1795 data
    (163243) 2002 FB3 1961-04-124.9034.9004.90616.41669–1695 data
    (192642) 1999 RD32 1969-08-273.6273.6253.63016.31161–3750 data
    (143651) 2003 QO104 1981-05-182.7612.7602.76116.01333–4306 data
    2017 CH1 1992-06-054.6913.3916.03717.9556–1795 data
    (170086) 2002 XR14 1995-06-244.2594.2594.26018.0531–1714 data
    (33342) 1998 WT24 2001-12-164.8594.8594.85917.9556–1795 data
    4179 Toutatis 2004-09-294.0314.0314.03115.32440–2450 data
    2014 JO25 2017-04-194.5734.5734.57317.8582–1879 data
    (137108) 1999 AN10 2027-08-071.0141.0101.01917.9556–1795 data
    (35396) 1997 XF11 2028-10-262.4172.4172.41816.9881–2845 data
    (154276) 2002 SY50 2071-10-303.4153.4123.41817.6714–1406 data
    (164121) 2003 YT1 2073-04-294.4094.4094.40916.21167–2267 data
    (385343) 2002 LV 2076-08-044.1844.1834.18516.61011–3266 data
    (52768) 1998 OR2 2079-04-164.6114.6114.61215.81462–4721 data
    (33342) 1998 WT24 2099-12-184.9194.9194.91917.9556–1795 data
    (85182) 1991 AQ 2130-01-274.1404.1394.14117.11100 data
    314082 Dryope 2186-07-163.7092.9964.78617.5668–2158 data
    (137126) 1999 CF9 2192-08-214.9704.9674.97318.0531–1714 data
    (290772) 2005 VC 2198-05-051.9511.7912.13417.6638–2061 data
    (A) List includes near-Earth approaches of less than 5 lunar distances (LD) of objects with H brighter than 18.
    (B) Nominal geocentric distance from the Earth's center to the object's center (Earth radius≈0.017 LD).
    (C) Diameter: estimated, theoretical mean-diameter based on H and albedo range between X and Y.
    (D) Reference: data source from the JPL SBDB, with AU converted into LD (1 AU≈390 LD)
    (E) Color codes:   unobserved at close approach  observed during close approach  upcoming approaches

    Physical characteristics

    Toutatis.jpg
    Goldstone radar image (1996)
    Asteroid 4179 Toutatis.faces model.jpg
    Computer model of Toutatis

    Large amounts of data of Toutatis were obtained during Chang'e 2's flyby. Toutatis is not a monolith, but most likely a coalescence of shattered fragments. This bifurcated asteroid is shown to be mainly consisting of a head (small lobe) and a body (large lobe). The two major parts are not round in shape, and their surfaces have a number of large facets. In comparison with radar models, the proximate observations from Chang'e 2's flyby have revealed several remarkable discoveries concerning Toutatis, among which the presence of the giant basin at the big end appears to be one of the most compelling geological features, and the sharply perpendicular silhouette in the neck region that connects the head and body is also quite novel. A large number of boulders and several short linear structures are also apparent on the surface. [5]

    Giant basin

    The giant basin at the big end of Toutatis has a diameter of ~805 m, suggesting that one or more impactors may have collided with it there. The most significant feature is the ridge around the largest basin. The wall of this basin has a relatively high density of lineaments, some of which seem to be concentric to the basin. These ridges are indicative of an internal structure of small bodies and most of the ridges near the largest basin at the big end are most likely related to the huge stress energy during impact. [5]

    Observation

    Toutatis has been observed with radar imaging from the Arecibo Observatory and the Goldstone Solar System Radar during the asteroid's prior Earth flybys in 1992, 1996, 2000, 2004, and 2008. It was also observed with radar during the December 2012 flyby and observed more distant flyby with radar in December 2016. [29] After 2016, Toutatis will not pass close to Earth again until 2069.

    Resolution of the radar images is as fine as 3.75 m per pixel, [30] providing data to model Toutatis's shape and spin state.

    Exploration

    Images of Toutatis taken by Chang'e 2 probe Asteroid 4179 Toutatis.jpg
    Images of Toutatis taken by Chang'e 2 probe

    The Chinese lunar probe Chang'e 2 departed from the Sun–Earth L2 point in April 2012 [31] and made a flyby of Toutatis on 13 December 2012, with closest approach being 3.2 kilometers and a relative velocity of 10.73 km/s, when Toutatis was near its closest approach to Earth. [13] [32] [33] It took several pictures of the asteroid, revealing it to be a dusty red/orange color.

    See also

    Related Research Articles

    The Alinda asteroids are a dynamical group of asteroids with a semi-major axis of about 2.5 AU and an orbital eccentricity approximately between 0.4 and 0.65. The namesake is 887 Alinda, discovered by Max Wolf in 1918.

    2063 Bacchus, provisional designation 1977 HB, is a stony asteroid and near-Earth object of the Apollo group, approximately 1 kilometer in diameter. The contact binary was discovered on 24 April 1977, by American astronomer Charles Kowal at the Palomar Observatory in California, United States. It was named after Bacchus from Roman mythology.

    <span class="mw-page-title-main">1036 Ganymed</span>

    1036 Ganymed, provisional designation 1924 TD, is a stony asteroid on a highly eccentric orbit, classified as a near-Earth object of the Amor group. It was discovered by German astronomer Walter Baade at the Bergedorf Observatory in Hamburg on 23 October 1924, and named after Ganymede from Greek mythology. With a diameter of approximately 35 kilometers, Ganymed is the largest of all near-Earth objects but does not cross Earth's orbit. The S-type asteroid has a rotation period of 10.3 hours. In October 2024, it is predicted to approach Earth at a distance of 56,000,000 km; 35,000,000 mi (0.374097 AU).

    <span class="mw-page-title-main">6489 Golevka</span>

    6489 Golevka is an Apollo, Mars-crosser, and Alinda asteroid discovered in 1991 by Eleanor F. Helin.

    <span class="nowrap">(53319) 1999 JM<sub>8</sub></span> Largest known potentially hazardous near-Earth asteroid

    (53319) 1999 JM8 is an asteroid, slow rotator and tumbler, classified as a near-Earth object and potentially hazardous asteroid (PHA) of the Apollo group, approximately 7 kilometers (4 miles) in diameter, making it the largest PHA known to exist. It was discovered on 13 May 1999, by astronomers of the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico.

    <span class="nowrap">(33342) 1998 WT<sub>24</sub></span> Sub-kilometer asteroid

    (33342) 1998 WT24 is a bright, sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid (PHA) of the Aten group, located in Venus's zone of influence that has frequent close encounters with Mercury, Venus, and Earth. It made a close approach to Earth on 11 December 2015, passing at a distance of about 4.2 million kilometers (2.6 million miles, 11 lunar distances) and reaching about apparent magnitude 11.

    <span class="mw-page-title-main">3752 Camillo</span>

    3752 Camillo is an inclined contact-binary asteroid, classified as near-Earth object of the Apollo group, approximately 2.3 kilometers in diameter. It was discovered on 15 August 1985, by astronomers Eleanor Helin and Maria Barucci using a 0.9-metre (35 in) telescope at the CERGA Observatory in Caussols, France. Lightcurve studies by Petr Pravec in 1998 suggest that the assumed S-type asteroid has an elongated shape and a longer-than average rotation period of 38 hours.

    <span class="nowrap">2007 TU<sub>24</sub></span>

    2007 TU24 is an Apollo near-Earth asteroid that was discovered by the Catalina Sky Survey in Arizona on 11 October 2007. Imaging radar has estimated that it is 250 meters (820 ft) in diameter. The asteroid passed 554,209 kilometer (344,370 mile or 1.4-lunar distance) from Earth on 29 January 2008 at 08:33 UTC. (At the time of the passage it was believed the closest for any known potentially hazardous asteroid (PHA) of this size before 2027, but in 2010 2005 YU55 was measured to be 400 meters in diameter.) At closest approach the asteroid had an apparent magnitude of 10.3 and was about 50 times fainter than the naked eye can see. It required about a 3-inch (76 mm) telescope to be seen.

    <span class="nowrap">(153591) 2001 SN<sub>263</sub></span>

    (153591) 2001 SN263 is a carbonaceous trinary asteroid, classified as near-Earth object and former potentially hazardous asteroid of the Amor group, approximately 2.6 kilometers (1.6 miles) in diameter. It was discovered by the Lincoln Near-Earth Asteroid Research project at Lincoln Lab's Experimental Test Site in Socorro, New Mexico, on 20 September 2001. The two synchronous minor-planet moons measure approximately 770 and 430 meters and have an orbital period of 16.46 and 150 hours, respectively.

    <span class="mw-page-title-main">3122 Florence</span> Near-Earth asteroid with 2 moons

    3122 Florence is a stony trinary asteroid of the Amor group. It is classified as a near-Earth object and potentially hazardous asteroid. It measures approximately 5 kilometers in diameter. It orbits the Sun at a distance of 1.0–2.5 AU once every 2 years and 4 months ; the orbit has an eccentricity of 0.42 and an inclination of 22° with respect to the ecliptic. Florence has two moons.

    1915 Quetzálcoatl, provisional designation 1953 EA, is a very eccentric, stony asteroid classified as near-Earth object, about half a kilometer in diameter. It was discovered on 9 March 1953, by American astronomer Albert George Wilson at Palomar Observatory, California. It was named for Quetzalcoatl from Aztec mythology.

    <span class="mw-page-title-main">Chang'e 2</span> Chinese Moon orbiter

    Chang'e 2 is a Chinese uncrewed lunar probe that was launched on 1 October 2010. It was a follow-up to the Chang'e 1 lunar probe, which was launched in 2007. Chang'e 2 was part of the first phase of the Chinese Lunar Exploration Program, and conducted research from a 100-km-high lunar orbit in preparation for the December 2013 soft landing by the Chang'e 3 lander and rover. Chang'e 2 was similar in design to Chang'e 1, although it featured some technical improvements, including a more advanced onboard camera. Like its predecessor, the probe was named after Chang'e, an ancient Chinese moon goddess.

    <span class="nowrap">(308635) 2005 YU<sub>55</sub></span> Potentially hazardous near-Earth asteroid

    (308635) 2005 YU55, provisionally named 2005 YU55, is a potentially hazardous asteroid 360±40 meters in diameter, as measured after its Earth flyby. Previously it was estimated to be 310 meters or about 400 m (1,300 feet) in diameter. It was discovered on 28 December 2005 by Robert S. McMillan at Steward Observatory, Kitt Peak. On 8 November 2011 it passed 0.85 lunar distances (324,900 kilometers; 201,900 miles) from Earth.

    <span class="nowrap">(192642) 1999 RD<sub>32</sub></span> Asteroid and suspected contact binary

    (192642) 1999 RD32, provisional designation: 1999 RD32, is an asteroid and suspected contact binary on an eccentric orbit, classified as a large near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 5 kilometers (3 miles) in diameter. It was discovered on 8 September 1999, at a magnitude of 18, by astronomers of the LINEAR program using its 1-meter telescope at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, United States. The asteroid is likely of carbonaceous composition and has a rotation period of 17.08 hours.

    <span class="nowrap">2014 HQ<sub>124</sub></span>

    2014 HQ124 is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Aten group, approximately 400 meters (1,300 feet) in diameter. It passed 3.25 lunar distances (LD) from Earth on 8 June 2014. It was discovered on 23 April 2014 by NEOWISE. It is estimated that an impact event would have had the energy equivalent of 2,000 megatons of TNT and would have created a 5 km (3 mi) impact crater. The news media misleadingly nicknamed it The Beast. 2014 HQ124 previously passed this close to Earth in 1952 and will not again until at least 2307. Radar imaging suggests it may be a contact binary.

    <span class="nowrap">2012 TC<sub>4</sub></span>

    2012 TC4 is a tumbling micro-asteroid classified as a bright near-Earth object of the Apollo group, approximately 10 meters (30 feet) in diameter. It was first observed by Pan-STARRS at Haleakala Observatory on the Hawaiian island of Maui, in the United States. As of 1 October 2017, it had a small Earth minimum orbital intersection distance of 0.000149 AU (22,300 km). On 12 October 2017, it passed Earth at 0.00033524 AU (50,151 km). The asteroid was removed from the Sentry Risk Table on 16 October 2017 and with a 5-year observation arc has a well-known orbit. For example, on the previously risk-listed date of 12 October 2022, it is now known that the asteroid will be more than 3 AU (450 million km) from Earth.

    <span class="nowrap">(85989) 1999 JD<sub>6</sub></span>

    (85989) 1999 JD6 is an Aten asteroid, near-Earth object, and potentially hazardous object in the inner Solar System that makes frequent close approaches to Earth and Venus. On the Earth approach in 2015, it was observed by the Goldstone Solar System Radar and found to be a contact binary with the largest axis approximately 2 kilometers wide, and each lobe about 200–300 meters large. Although 1999 JD6 in its current orbit never passes closer than 0.047 AU to Earth, it is listed as a potentially hazardous object because it is large and might pose a threat in the future.

    <span class="nowrap">(153201) 2000 WO<sub>107</sub></span>

    (153201) 2000 WO107 is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Aten group with a very well determined orbit. It was discovered on 29 November 2000, by astronomers of the Lincoln Near-Earth Asteroid Research (LINEAR) at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. It is a contact binary.

    <span class="nowrap">2015 TB<sub>145</sub></span> Asteroid

    2015 TB145 is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 650 meters (2,000 feet) in diameter. It safely passed 1.27 lunar distances from Earth on 31 October 2015 at 17:01 UTC, and passed by Earth again in November 2018.

    <span class="mw-page-title-main">460P/PanSTARRS</span> Near-Earth object and periodic comet of the Jupiter family

    460P/PanSTARRS (also known with the provisional designation P/2016 BA14) is a near-Earth object and periodic comet of the Jupiter family, with an orbital period of 5.25 years. In March 2016 it passed at distance of 2.2 million miles (3.5 million km, or 9 lunar distances) from Earth. It was the closest approach by a comet since 1770 and 3rd closest recorded comet to Earth. The close flyby enabled the size of the nucleus to be calculated at about 1 km (0.62 mi) in diameter, which was much bigger than expected. The comet is very dark, reflecting about 2-3 percent of the visible light, about the same as a charcoal briquette. It has a very similar orbit as numbered comet 252P/LINEAR, and may be related to it (e.g. split off of).

    References

    1. 1 2 3 "4179 Toutatis (1989 AC)". Minor Planet Center. Retrieved 2 November 2017.
    2. 1 2 Schmadel, Lutz D. (2007). "(4179) Toutatis". Dictionary of Minor Planet Names – (4179) Toutatis. Springer Berlin Heidelberg. pp. 357–358. doi:10.1007/978-3-540-29925-7_4150. ISBN   978-3-540-00238-3.
    3. 1 2 3 4 5 6 7 8 "JPL Small-Body Database Browser: 4179 Toutatis (1989 AC)" (2017-05-27 last obs.). Jet Propulsion Laboratory. Retrieved 2 November 2017.
    4. ↑ Hudson, "Gravitational Isopotentials on Toutatis"
    5. 1 2 3 Huang, Jiangchuan; Ji, Jianghui; Ye, Peijian; Wang, Xiaolei; Yan, Jun; Meng, Linzhi; Wang, Su; Li, Chunlai; Li, Yuan; Qiao, Dong; Zhao, Wei; Zhao, Yuhui; Zhang, Tingxin; Liu, Peng; Jiang, Yun; Rao, Wei; Li, Sheng; Huang, Changning; Ip, Wing-Huen; Hu, Shoucun; Zhu, Menghua; Yu, Liangliang; Zou, Yongliao; Tang, Xianglong; Li, Jianyang; Zhao, Haibin; Huang, Hao; Jiang, Xiaojun; Bai, Jinming (2013). "The Ginger-shaped Asteroid 4179 Toutatis: New Observations from a Successful Flyby of Chang'e-2 : Scientific Reports : Nature Publishing Group". Scientific Reports. 3: 3411. Bibcode:2013NatSR...3E3411H. doi:10.1038/srep03411. PMC   3860288 . PMID   24336501.
    6. 1 2 Hudson, R. S.; Ostro, S. J.; Scheeres, D. J. (February 2003). "High-resolution model of Asteroid 4179 Toutatis". Icarus. 161 (2): 346–355. Bibcode:2003Icar..161..346H. CiteSeerX   10.1.1.494.7779 . doi:10.1016/S0019-1035(02)00042-8.
    7. 1 2 Scheeres, D. J.; Ostro, S. J.; Hudson, R. S. (March 1998). "Dynamics of Orbits Close to Asteroid 4179 Toutatis". Icarus. 132 (1): 53–79. doi:10.1006/icar.1997.5870.
    8. ↑ "LCDB Data for (4179) Toutatis". Asteroid Lightcurve Database (LCDB). Retrieved 2 November 2017.
    9. 1 2 "AstDys (4179) Toutatis Ephemerides for 2004". Department of Mathematics, University of Pisa, Italy. Retrieved 27 June 2010.
    10. ↑ "AstDys (4179) Toutatis Ephemerides 2059". Department of Mathematics, University of Pisa, Italy. Retrieved 27 June 2010.
    11. ↑ "Asteroid 4179 Toutasis". NASA. Retrieved 24 May 2022.
    12. 1 2 "Trick or Treat: It's Toutatis!". Science@Nasa. 31 October 2000. Archived from the original on 29 January 2009. Retrieved 27 January 2009.
    13. 1 2 Lakdawalla, Emily (14 December 2012). "Chang'E 2 imaging of Toutatis succeeded beyond my expectations!". The Planetary Society . Retrieved 15 December 2012.
    14. 1 2 3 4 5 6 7 8 9 "JPL Close-Approach Data: 4179 Toutatis (1989 AC)" (2011-05-22 last obs (arc=77.28 years)). Retrieved 13 November 2011.
    15. ↑ "(4179) Toutatis = 1934 CT = 1989 AC". IAU Minor Planet Center. Retrieved 18 April 2013.
    16. ↑ "By Toutatis! France unveils statue to Asterix creator". France 24. 23 January 2020. Retrieved 24 March 2022.
    17. ↑ Mueller, Béatrice E. A.; Samarasinha, Nalin H.; Belton, Michael J. S. (August 2002). "The Diagnosis of Complex Rotation in the Lightcurve of 4179 Toutatis and Potential Applications to Other Asteroids and Bare Cometary Nuclei". Icarus. 158 (2): 305–311. Bibcode:2002Icar..158..305M. doi:10.1006/icar.2002.6892.
    18. ↑ Bottke, William Jr. (October 2007). "Implications of the YORP Effect for Our Understanding of Asteroid Evolution". Bulletin of the American Astronomical Society. 39: 416. Bibcode:2007DPS....39.0507B.
    19. ↑ "Toutatis is in a 3:1 mean-motion resonance with Jupiter (rotating frame)". Gravity Simulator. Retrieved 27 January 2009.
    20. 1 2 3 4 Whipple, L.; Shelus, Peter J. (1993). "Long-Term Dynamical Evolution of the Minor Planet (4179) Toutatis". Icarus. 105 (2): 408–419. Bibcode:1993Icar..105..408W. doi:10.1006/icar.1993.1137.
    21. ↑ "The Minor Planet Bulletin" (PDF). Association of Lunar and Planetary Onservers. 1994. Archived from the original (PDF) on 19 June 2013. Retrieved 25 June 2014.
    22. ↑ "Solex by Aldo Vitagliano". Archived from the original on 20 December 2008. Retrieved 3 March 2009.
    23. 1 2 3 "NEODys (4179) Toutatis Close Approaches". Department of Mathematics, University of Pisa, Italy. Retrieved 20 March 2009.
    24. ↑ "NEODys (4179) Toutatis Ephemerides for December 2012". Department of Mathematics, University of Pisa, Italy. Retrieved 27 June 2010.
    25. ↑ "(4179) Toutatis = 1934 CT = 1989 AC". IAU Minor Planet Center. Retrieved 19 October 2012.
    26. ↑ Ostro, S. J.; Hudson, R. S.; Rosema, K. D.; Giorgini, J. D.; et al. (1998). "Asteroid 4179 Toutatis: 1996 Radar Observations" (PDF). Icarus. 137 (1): 122–139. Bibcode:1999Icar..137..122O. doi:10.1006/icar.1998.6031. hdl:2014/19433. Archived (PDF) from the original on 22 September 2017.
    27. ↑ "Close call for earth ahead? – possible collision with asteroid Toutatis". USA Today (Society for the Advancement of Education). 1993. Archived from the original on 28 June 2012.
    28. ↑ David Morrison (27 September 2004). "Close Flyby This Week from Asteroid Toutatis". Asteroid and Comet Impact Hazards (NASA). Archived from the original on 14 February 2013. Retrieved 18 June 2015.
    29. ↑ "2012 Goldstone Radar Observations of (4179) Toutatis" . Retrieved 15 November 2012.
    30. ↑ "Big Asteroid Tumbles Harmlessly Past Earth". NASA . Retrieved 6 April 2018.
    31. ↑ Lakdawalla, Emily (14 June 2012). "Chang'E 2 has departed Earth's neighborhood for.....asteroid Toutatis!?". The Planetary Society . Retrieved 15 November 2012.
    32. ↑ ""Pseudo-MPEC" for 2010-050A = SM999CF = Chang'e 2 probe" . Retrieved 15 November 2012.
    33. ↑ "[视频]"嫦娥二号"飞越探测小行星_新闻台_中国网络电视台". News.cntv.cn. Retrieved 25 June 2014.
    This page is based on this Wikipedia article
    Text is available under the CC BY-SA 4.0 license; additional terms may apply.
    Images, videos and audio are available under their respective licenses.