Hostname: page-component-586b7cd67f-t7fkt Total loading time: 0 Render date: 2024-11-24T23:40:32.679Z Has data issue: false hasContentIssue false

The Chelyabinsk event

Published online by Cambridge University Press:  27 October 2016

Jiří Borovička*
Affiliation:
Astronomical Institute of the Czech Academy of Sciences, Fričova 298, CZ-25165 Ondřejov, Czech Republic email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

On February 15, 2013, 3:20 UT, an asteroid of the size of about 19 meters and mass of 12,000 metric tons entered the Earth's atmosphere unexpectedly near the border of Kazakhstan and Russia. It was the largest confirmed Earth impactor since the Tunguska event in 1908. The body moved approximately westwards with a speed of 19 km s−1, on a trajectory inclined 18 degrees to the surface, creating a fireball of steadily increasing brightness. Eleven seconds after the first sightings, the fireball reached its maximum brightness. At that point, it was located less than 40 km south from Chelyabinsk, a Russian city of population more than one million, at an altitude of 30 km. For people directly underneath, the fireball was 30 times brighter than the Sun. The cosmic body disrupted into fragments; the largest of them was visible for another five seconds before it disappeared at an altitude of 12.5 km, when it was decelerated to 3 km s−1. Fifty six second later, that ~600 kg fragment landed in Lake Chebarkul and created a 8 m wide hole in the ice. Small meteorites landed in an area 80 km long and several km wide and caused no damage. The meteorites were classified as LL ordinary chondrites and were interesting by the presence of two phases, light and dark. More material remained, however, in the atmosphere forming a dust trail up to 2 km wide and extending along the fireball trajectory from altitude 18 to 70 km. The dust then circled the Earth within few days and formed a ring around the northern hemisphere. In Chelyabinsk and its surroundings a very strong blast wave arrived 90 – 150 s after the fireball passage (depending on location). The wave was produced by the supersonic flight of the body and broke ~10% of windows in Chelyabinsk (~40% of buildings were affected). More than 1600 people were injured, mostly from broken glass. The whole event was well documented by video cameras, seismic and infrasonic records, and satellite observations. The total energy was 500 kT TNT (2 × 1015 J).

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2016 

References

Badyukov, D. D., Dudorov, A. E. & Khaibrakhmanov, S. A. 2014. Vestnik Chelyab. Gosudar. Univ., 1/2014, Fizika, Vyp. 19, p. 40 (in Russian)Google Scholar
Borovička, J., Spurný, P., Brown, P. et al. 2013. Nature, 503, 235 Google Scholar
Borovička, J., Shrbený, L., Kalenda, P. et al. 2015. Astron. Astrophys., in press, doi: 10.1051/0004-6361/201526680 Google Scholar
Brown, P. G., Assink, J. D., Astiz, L. et al. 2013. Nature, 503, 238 Google Scholar
Chesley, S. R., Farnocchia, D., Brown, P. G., & Chodas, P. W., 2015. In Aerospace Conference, 2015 IEEE, 8 pp., 7–14 March 2015, doi: 10.1109/AERO.2015.7119148 Google Scholar
Gorkavyi, N., Rault, D. F., Newman, P. A. et al. 2013. Geophys. Res. Lett. 40, 4728 Google Scholar
Harris, A. W. & D'Abramo, G. 2015. Icarus, 257, 302 Google Scholar
Jenniskens, P., Shaddad, M. H., Numan, D. et al. 2009. Nature, 458, 485 Google Scholar
Jones, R. L., Chesley, S. R., Connolly, A. J., et al. 2009, Earth Moon and Planets, 105, 101 Google Scholar
Kohout, T., Gritsevich, M., Grokhovsky, V. I. et al. 2014. Icarus, 228, 78 Google Scholar
McCord, T. B., Morris, J., Persing, D. et al. 1995. J. Geophys. Res. 100 (E2), 3245.CrossRefGoogle Scholar
Miller, S. D., Straka, W. C. III, Scott Bachmeier, A. et al. 2013. PNAS, 110, 18092 Google Scholar
Popova, O., Borovička, J., Hartmann, W. K. et al. 2011. Meteorit. Plan. Sci., 46, 1525 Google Scholar
Popova, O. P., Jenniskens, P., Emel'yanenko, V. et al. 2013. Science, 342, 1069 Google Scholar
Popova, O. P., Jenniskens, P., & Glazachev, D. O. 2014. In: Geofiz. effekty padeniya Chelyab. Meteorita (Moscow: IDG RAS), Dynam. Proc. Geospher. 5, 59 (In Russian)Google Scholar
Povinec, P. P., Laubenstein, M., Jull, A. J. T. et al. 2015. Meteorit. Plan. Sci., 50, 273 Google Scholar
Proud, S. R. 2013. Geophys. Res. Lett. 40, 3351 CrossRefGoogle Scholar
Reddy, V., Sanchez, J. A., Bottke, W. F. et al. 2014. Icarus, 237, 116 CrossRefGoogle Scholar
Reddy, V., Vokrouhlický, D., Bottke, W. F. et al. 2015. Icarus, 252, 129 CrossRefGoogle Scholar
Richter, K., Abell, P., Agresti, D. et al. 2015. Meteorit. Plan. Sci., 50, 1790 Google Scholar
Rieger, L. A., Bourassa, A. E., & Degenstein, D. A. 2014. Atmos. Meas. Tech., 7, 777 CrossRefGoogle Scholar
Silber, E. A., ReVelle, D. O., Brown, P. G. & Edwards, W. N. 2009. J. Geophys. Res. 114 E08006.Google Scholar
Silber, E. A., Le Pichon, A. & Brown, P. G. 2011. Geophys. Res. Lett. 38 L12201.Google Scholar
Tonry, J. L. 2011. Publ. Astron. Soc. Pacific, 123, 58 CrossRefGoogle Scholar
Vasilyev, N. V. 1998. Plan. Space Sci., 46, 129.CrossRefGoogle Scholar