22
N. G. Syzranova and V. A. Andrushchenko
angle to the horizon (θ e < 9
◦
), it could be a flyby. This did not exclude its fragmentation with explosions of some of its fragments in the atmosphere, leading to the
collapse of the forest, but the main part of sufficiently large fragments could either
fall far from the epicenter of the explosion or go into outer space. This assumption
is also confirmed by the estimates given in [9]. The hypothesis we have considered
allows us to explain the results of studying the proposed fall site of the Tunguska
body by many expeditions: the absence of a crater and any material remnants of
the meteoritic substance of this body. The results also show that the implementation
of flight paths of meteoroids depends on a number of defining parameters of the
phenomenon in the aggregate: speed, angle of entry of the body into the atmosphere,
ballistic coefficient, and coefficient of aerodynamic quality. In addition, it is also
important to take into account the fragmentation and destruction of the meteoroid
under the influence of power and heat loads.
2.4 Conclusions
We simulate numerically the flight of large bodies in the Earth’s atmosphere. Based
on the model of a single body (no fragmentation), we determine the kinematic and
physical characteristics necessary for a meteoroid to ascend in the atmosphere after
its initial descend. We find that the key parameter for the possibility of such ascend is
the angle of entry into the atmosphere. We compute the critical angles for a range of
control parameters, i.e. the ballistic coefficient and the lift-to-drag ratio. Our results
explain certain effects of the Tunguska event that took place in 1908.
References
1. Gordon, E., Bartky, C.D., Li, F. Wager, J.F.: Dynamics of a large meteor. In: 13th Aerospace
Sciences Meeting, Pasadena, CA, U.S.A., AIAA Paper 75–14 (1975)
2. Ceplecha, Z.: Earth-grazing daylight fireball of August 10, 1972. Astron. Astrophys. 283, 287–
288 (1994)
3. Hartman, W.K.: The smaller bodies of the solar system. Sci. Am. 233(3), 142–159 (1975)
4. Syzranova, N.G., Andrushchenko, V.A.: Simulation of the motion and destruction of bolides in
the Earth’s atmosphere. High Temp. 54(3), 308–315 (2016)
5. Khokhryakov, V.A.: On the interaction of cosmic bodies with the atmospheres of planets. Space
Res. 15(2), 203–207 (1977) (in Russian)
6. Melosh, H.J.: Impact cratering: a geologic process. In: Oxford Monographs on Geology and
Geophysics Series, 11 (1989)
7. Schultz, P.H., Zarate, M., Hames, W., Camilion, C. King, J.: A 3.3-Ma impact in Argentina and
possible consequences. Science 282, 2061–2063 (1998)
N. G. Syzranova and V. A. Andrushchenko
angle to the horizon (θ e < 9
◦
), it could be a flyby. This did not exclude its fragmentation with explosions of some of its fragments in the atmosphere, leading to the
collapse of the forest, but the main part of sufficiently large fragments could either
fall far from the epicenter of the explosion or go into outer space. This assumption
is also confirmed by the estimates given in [9]. The hypothesis we have considered
allows us to explain the results of studying the proposed fall site of the Tunguska
body by many expeditions: the absence of a crater and any material remnants of
the meteoritic substance of this body. The results also show that the implementation
of flight paths of meteoroids depends on a number of defining parameters of the
phenomenon in the aggregate: speed, angle of entry of the body into the atmosphere,
ballistic coefficient, and coefficient of aerodynamic quality. In addition, it is also
important to take into account the fragmentation and destruction of the meteoroid
under the influence of power and heat loads.
2.4 Conclusions
We simulate numerically the flight of large bodies in the Earth’s atmosphere. Based
on the model of a single body (no fragmentation), we determine the kinematic and
physical characteristics necessary for a meteoroid to ascend in the atmosphere after
its initial descend. We find that the key parameter for the possibility of such ascend is
the angle of entry into the atmosphere. We compute the critical angles for a range of
control parameters, i.e. the ballistic coefficient and the lift-to-drag ratio. Our results
explain certain effects of the Tunguska event that took place in 1908.
References
1. Gordon, E., Bartky, C.D., Li, F. Wager, J.F.: Dynamics of a large meteor. In: 13th Aerospace
Sciences Meeting, Pasadena, CA, U.S.A., AIAA Paper 75–14 (1975)
2. Ceplecha, Z.: Earth-grazing daylight fireball of August 10, 1972. Astron. Astrophys. 283, 287–
288 (1994)
3. Hartman, W.K.: The smaller bodies of the solar system. Sci. Am. 233(3), 142–159 (1975)
4. Syzranova, N.G., Andrushchenko, V.A.: Simulation of the motion and destruction of bolides in
the Earth’s atmosphere. High Temp. 54(3), 308–315 (2016)
5. Khokhryakov, V.A.: On the interaction of cosmic bodies with the atmospheres of planets. Space
Res. 15(2), 203–207 (1977) (in Russian)
6. Melosh, H.J.: Impact cratering: a geologic process. In: Oxford Monographs on Geology and
Geophysics Series, 11 (1989)
7. Schultz, P.H., Zarate, M., Hames, W., Camilion, C. King, J.: A 3.3-Ma impact in Argentina and
possible consequences. Science 282, 2061–2063 (1998)