Astronomy:2012 TC4

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2012 TC4
2012 TC4 radar animation before closest approach.gif
Radar movie of 2012 TC4[1]
Discovery[2][3]
Discovered byPan-STARRS 1
Discovery siteHaleakala Obs.
Discovery date4 October 2012
Designations
2012 TC4
Minor planet category
Orbital characteristics[2]
Epoch 1 October 2017 (JD 2458027.5)
Uncertainty parameter 1
Observation arc5.19 yr (1,897 d)
|{{{apsis}}}|helion}}1.8786 AU
|{{{apsis}}}|helion}}0.9335 AU
1.4061 AU
Eccentricity0.3361
Orbital period1.67 yr (609 d)
Mean anomaly332.79°
Mean motion0° 35m 27.96s / day
Inclination0.8572°
Longitude of ascending node198.23°
222.58°
Earth MOID0.000149 astronomical unit|AU (0.0580 LD)
Mars MOID0.03 AU[4]
Physical characteristics
Dimensions15 m × 8 m[5][6]
Mean diameter7–13 m[7][8]
15 m[8]
Rotation period
Geometric albedo
  • 0.35±0.1[7]
  • 0.30±0.01 (radiometric)
Apparent magnitude12.9–31[10]
Absolute magnitude (H)


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.[6][7][8] 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 astronomical unit|AU (22,300 km).[2] On 12 October 2017, it passed Earth at 0.00033524 astronomical unit|AU (50,151 km).[2] The asteroid was removed from the Sentry Risk Table on 16 October 2017[11] and with a 5-year observation arc has a well-known orbit.[2] For example, on the previously risk-listed date of 12 October 2022,[12] it is now known that the asteroid will be more than 3 astronomical unit|AU (450 million km) from Earth.[13]

Approaches to large bodies

Orbital modeling shows the asteroid nominally passed about 1 million km from Earth in October 1986, but the uncertainty region suggests it could have passed as close as 20 km.[2]

Date (UT) Object distance in km
(center–center) 		3-Σ
uncertainty
in km 		Speed-
relative
in km/s
13 October 1996 Earth 753 000 ± 7000 6.445
13 October 1996 Moon 530 000 ± 6300 7.144
12 October 2012 Earth 94 965 ± 0.32 7.123
12 October 2012 Moon 113 886 ± 0.64 6.773
12 October 2017 – 05:42 Earth 50 151 ± 0.14 7.647
12 October 2017 – 19:19 Moon 277 697 ± 0.34 6.101

Data from JPL 60 solution date 3 November 2017[2]

2012 Earth encounter

2012 TC4 appears as a dot of this composite of 37 individual 50-second exposures.[14]

2012 TC4 was discovered on 4 October 2012 at apparent i-band magnitude 20.1 while the asteroid was 0.03 AU (4,500,000 km; 2,800,000 mi) from Earth.[3] It came within 0.000634 AU (0.247 LD, 94,800 km, 58,900 mi) from Earth on 12 October 2012.[2]

During the 2012 close approach, the asteroid only had an observation arc of 7 days, between 4 and 11 October 2012, so the exact distance of the 2017 closest approach was poorly constrained. With the 7 day observation arc, the asteroid had a 3-sigma chance of passing between 0.00008818 and 0.002896 AU (0.034 to 1.127 LD, 13,200–433,200 km, 8,200–269,200 mi) from Earth on 12 October 2017.[15] Astronomers were certain that it would not pass closer than 6,800 km from the surface of Earth, ruling out any possibility that it could hit the Earth in 2017.[16]

2017 Earth encounter

Orbit in yellow among inner solar system planets before 2017 flyby
Orbit of 2012 TC4 deflected by Earth's gravity. Earth is blue. For reference, a geosynchronous satellite and the Moon are included in this animation. The green path of 2012 TC4 turns darker as it dips below the ecliptic plane (click for animation).
Orbits from pre-2012 to post-2017 encounters. The orbit of 2012 TC4 has changed twice since 2012.

On 12 October 2017 at 5:42 UT, the asteroid passed 0.00033524 AU (50,151 km; 31,163 mi) from Earth.[2] Observations between July and October reduced the uncertainty region from several hundred thousand kilometers[15] to about ±140 meters.[17][2] The asteroid was removed from the Sentry Risk Table on 16 October 2017 using JPL solution #56.[11] Prior to the encounter, it was rated −4.11 on the Palermo scale, with a 1 in 1,000 chance of impact over the next hundred years.[12]

Paul Chodas of NASA's Center for near-Earth Object Studies, and Vishnu Reddy of the University of Arizona's Lunar and Planetary Laboratory, viewed the 2017 flyby (inside of the orbit of the Moon) as a way to test and refine the global asteroid detection and tracking network designed to give warning of objects heading toward Earth.[16] Reddy coordinated the effort, involving over a dozen institutions worldwide.[16][18][19] In addition to the observation campaign, NASA used this exercise to test communications between the many observers and also to test internal U.S. government messaging and communications up through the executive branch and across government agencies, as it would during an actual predicted impact emergency. Results of the campaign were published on 3 November 2017.[5]

The asteroid remained too faint to be recovered with automated astronomical surveys until early September,[20] but a more targeted observation with the Very Large Telescope recovered it on 27 July 2017 at apparent magnitude 26.8, while the asteroid was 0.4 AU (60,000,000 km; 37,000,000 mi) from Earth, making it one of the dimmest asteroid recoveries ever. As such, 2012 TC4 has become the first known asteroid ever to be observed passing less than 1 Lunar distance from Earth twice in a row.[21] At the time of recovery the asteroid was about 100 million times fainter than what can be seen with the naked eye[22] and 500 times fainter than when it was discovered in 2012. As a result of the 2017 recovery observations, it was known that on 12 October 2017 at 5:42 UT, the asteroid would pass 0.0003352 AU (50,150 km; 31,160 mi) from Earth.[2] Then at 19:19 UT, the asteroid would pass 0.001856 AU (277,700 km; 172,500 mi) from the Moon.[2] 2012 TC4 peaked at about apparent magnitude 12.9,[23] and was too faint to be seen without a telescope. The Earth approach of 2017 increased the asteroid's orbital period from 1.67 years to 2.06 years.[24]

2012 TC4 reached a maximum apparent magnitude of 12.9 just prior to its closest approach, soon after which it came too close to the Sun to be seen with telescopes.[23] It was last observed on 14 December 2017 at an apparent magnitude of 25,[4]

Physical properties

2012 TC4 size reference.png
Size reference of 2012 TC4, based on radar observations.

Fast rotator and tumbler

Studies of the asteroid's light curve in October 2012, found it to have a rotation period of 0.2038 hours (or 12 minutes and 14 seconds) with a brightness variation of 0.93 magnitude ({{{1}}}), which is indicative for a non-spherical shape.[9][lower-alpha 1] 2012 TC4 is a fast rotator, which is rather typical for its small size. The fastest rotator currently known is 2014 RC, a similarly sized NEO, with a period of only 16 seconds. Lightcurves obtained during the 2017 encounter confirmed that 2012 TC4 is in a non-principal axis rotation, commonly known as tumbling.[7][5] The spin axis varies on timescales of minutes, with a second period of 0.142 hours (or 8.5 minutes).[8] The lightcurve amplitude suggests a ratio of largest to smallest axis of at least 2.3.[7]

Radar observations

Radar images were taken from Goldstone Observatory and Green Bank Telescope on 12 October 2017. The delay-doppler images had a range resolution of 1.9 meters/pixel, the highest resolution ever obtained using Goldstone transmissions.[6][1] The images showed that 2012 TC4 was a very elongated object about 50 feet (15 meters) long and roughly 25 feet (8 meters) wide.[5] The high circular polarization ratio found for 2012 TC4 is consistent with results seen from E- and V-type NEAs previously.[6] Observations from Arecibo Observatory were planned, but had to be cancelled due to damage to the observatory as a result of Hurricane Maria.[25]

Composition

The spectrum of 2012 TC4 is that of an E- or Xe-type asteroid.[7][6] E-type asteroids tend to have a high albedo (>0.30). This agrees with the albedo of 0.35 found for 2012 TC4.[1] This type of asteroids is commonly found in the inner Main Belt.[26]

2012 TC4 is composed of igneous material.[5] The short rotation period of 2012 TC4 implies that it is not a rubble pile but rather a monolithic object of non-negligible strength, which is typical for very small asteroids.[7]

Orbit change

As a result of 2012 TC4's frequent approaches to Earth, its orbit changes significantly over short periods of only decades. Its two observed close approaches and their effects are shown below:

Date Event Semimajor axis (AU) Perihelion (AU) Aphelion (AU) Eccentricity Inclination (°) Argument of perihelion (°) Ascending node (°)
2012-10-01 pre-2012 approach 1.2744 0.9015 1.6472 0.2926 1.4097 234.7282 198.5560
2012-10-12 2012 approach 1.3837 0.9115 1.8559 0.3413 1.2320 228.5354 198.4622
2012-10-30 post-2012 approach 1.3893 0.9305 1.8480 0.3302 0.8582 223.1271 198.1033
2017-10-01 pre-2017 approach 1.4155 0.9410 1.8901 0.3353 0.8566 221.8553 198.0054
2017-10-12 2017 approach 1.7076 0.9522 2.4630 0.4424 0.1693 218.4570 193.6520
2017-10-30 post-2017 approach 1.6492 0.9711 2.3273 0.4112 0.5327 248.6359 208.5051
2050-01-01 pre-2050 approach 1.6226 0.9688 2.2765 0.4030 0.5266 266.6192 197.8009

Between 2012 and 2017, 2012 TC4's average distance from the Sun increased by almost 0.4 AU, with the time it takes to orbit the sun increasing by 250 days. Its closest approach to the Sun also increased significantly, from 90% of the Earth's distance to the Sun to 97%, and its inclination lowered slightly, going from 1.4 degrees to less than 0.5 degrees relative to Earth's orbit.

As a result of non-gravitational forces such as the Yarkovsky effect on small bodies, it is difficult to constrain its orbit more than a few decades into the past or future.

See also

Notes

  1. ↑ 1.0 1.1 Lightcurve plot of 2012 TC4 at the Palmer Divide Observatory by Brian D. Warner (2012). Rotation period 0.2038±0.0002 hours with a brightness amplitude of 0.93±0.05 mag. Summary figures for 2012 TC4 at the LCDB

References

  1. ↑ 1.0 1.1 1.2 "The 2012 TC4 Observing Campaign -- Radar animations". University of Maryland. http://2012tc4.astro.umd.edu/References/radar_movies.shtml. 
  2. ↑ 2.00 2.01 2.02 2.03 2.04 2.05 2.06 2.07 2.08 2.09 2.10 2.11 2.12 2.13 "JPL Small-Body Database Browser: (2012 TC4)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/?sstr=2012TC4&view=OPC. 
  3. ↑ 3.0 3.1 "MPEC 2012-T18 : 2012 TC4". IAU Minor Planet Center. 2012-10-07. http://www.minorplanetcenter.net/mpec/K12/K12T18.html.  (K12T04C)
  4. ↑ 4.0 4.1 4.2 4.3 "2012 TC4". Minor Planet Center. https://minorplanetcenter.net/db_search/show_object?utf8=%E2%9C%93&object_id=2012+TC4. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 "Astronomers Complete First International Asteroid Tracking Exercise". JPL. 3 November 2017. https://www.jpl.nasa.gov/news/news.php?release=2017-289. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 "The 2012 TC4 Observing Campaign – Radar observations UPDATE October 12, 2017". University of Maryland. http://2012tc4.astro.umd.edu/References/TC4RadarUpdate.txt. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 7.7 7.8 Ryan, William H.; Ryan, Eileen V. (2017). "Physical Characterization of NEA 2012 TC4". University of Maryland. http://2012tc4.astro.umd.edu/References/ryan_pdc2017.pdf. 
  8. ↑ 8.0 8.1 8.2 8.3 8.4 8.5 "NEA 2012 TC4 -- Physical Properties". University of Maryland. http://2012tc4.astro.umd.edu/2012TC4_properties.shtml. 
  9. ↑ 9.0 9.1 9.2 9.3 "LCDB Data for 2012 TC4". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=0%7C2012+TC4. 
  10. ↑ 10.0 10.1 "NEODyS-2 2012TC4". Department of Mathematics, University of Pisa, Italy. https://newton.spacedys.com/neodys/index.php?pc=1.1.0&n=2012+TC4. 
  11. ↑ 11.0 11.1 "Date/Time Removed". NASA/JPL Near-Earth Object Program Office. https://cneos.jpl.nasa.gov/sentry/removed.html. 
  12. ↑ 12.0 12.1 "Archive: Earth Impact Risk Summary: 2012 TC4 (7 day observation arc)". NASA/JPL Near-Earth Object Program Office. https://cneos.jpl.nasa.gov/sentry/details.html#?des=2012%20TC4. 
  13. ↑ "Horizons Batch for 2022-10-12". JPL Horizons. https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND=%272012+TC4%27&START_TIME=%272022-10-12%27&STOP_TIME=%272022-10-13%27&STEP_SIZE=%272%20day%27&QUANTITIES=%2720,39%27. Retrieved 2022-10-04. 
  14. ↑ "A Very Close Encounter". http://www.eso.org/public/announcements/ann17052/. 
  15. ↑ 15.0 15.1 "Archive: Close Approach table for 2012 TC4 (using 7 day obs arc)". NASA. http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2012TC4;cad=1. 
  16. ↑ 16.0 16.1 16.2 "Asteroid Flyby Will Benefit NASA Detection and Tracking Network". NASA. 28 July 2017. https://www.jpl.nasa.gov/news/news.php?feature=6906. 
  17. ↑ "TC4: HOW NASA PLANS TO TEST ITS PLANETARY DEFENSE SYSTEMS ON CLOSE-APPROACH ASTEROID". 6 October 2017. http://www.newsweek.com/asteroid-tc4-nasa-planetary-defense-exercise-paul-chodas-679660. 
  18. ↑ Coleman, Nancy (1 August 2017). "NASA's planetary defense system will be put to the test in October". CNN. http://www.cnn.com/2017/08/01/us/nasa-asteroid-flyby-planetary-defense-trnd/index.html. 
  19. ↑ "The 2012 TC4 Observing Campaign". University of Maryland. http://2012tc4.astro.umd.edu/. 
  20. ↑ "NEODyS-2 Possible recovery list". Department of Mathematics, University of Pisa, Italy. https://newton.spacedys.com/neodys/index.php?pc=4.1&ots=r. 
  21. ↑ "MPEC 2017-P26 : 2012 TC4". IAU Minor Planet Center. 2017-08-06. http://www.minorplanetcenter.net/mpec/K17/K17P26.html.  (K12T04C)
  22. ↑ Math: [math]\displaystyle{ (\sqrt[5]{100})^{26.8-6.5}\approx 131800000 }[/math]
  23. ↑ 23.0 23.1 "2012TC4 Ephemerides for 12 October 2017". NEODyS (Near Earth Objects – Dynamic Site). https://newton.spacedys.com/neodys/index.php?pc=1.1.3.1&n=2012TC4&oc=500&y0=2017&m0=10&d0=11&h0=0&mi0=0&y1=2017&m1=10&d1=13&h1=0&mi1=0&ti=1.0&tiu=hours. 
  24. ↑ "Orbit of NEA 2012 TC4". http://2012tc4.astro.umd.edu/2012TC4_orbit.shtml. 
  25. ↑ "Goldstone Radar Observations Planning: 2012 TC4". JPL. https://echo.jpl.nasa.gov/asteroids/2012TC4/tc4_planning.2017.html. 
  26. ↑ Fornasier, S.; Clark, B. E.; Dotto, E. (July 2011). "Spectroscopic survey of X-type asteroids". Icarus 214 (1): 131–146. doi:10.1016/j.icarus.2011.04.022. Bibcode: 2011Icar..214..131F. 

External links



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