WikiJournal of Science/Earth-grazing meteoroid of 13 October 1990
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Visual observations were reported by three independent Czech observers: astronomer Petr Pravec, Pavel Klásek, and Lucie Bulíčková. According to their report, the event started at 03:27:16±3 UT[note 1] and the observed bright meteor (fireball) moved from south to north. It left a track that was visible for 10 seconds.
Most data about the encounter was acquired using photographic observations by cameras of the European Fireball Network. It was the first event of this type recorded by cameras from two distant locations, at Červená hora and Svratouch (both in the present-day Czech Republic), which enabled the calculation of the meteoroid's orbital characteristics by geometrical methods. Both were equipped with all-sky objectives.
The Červená hora image was especially valuable. It recorded the fireball's trajectory over approximately 110°, starting 51° above the southern horizon, passing the zenith just 1° westward and disappearing only 19° above the northern horizon (thus crossing about 60% of the sky). Its camera was also equipped with a rotating shutter that interrupted the exposure 12.5 times per second and divided the captured track of the fireball, allowing the determination of its speed. Over the last 4°, the fireball's angular velocity was lower than the resolution of the instrument. The Svratouch image recorded the trajectory only for about 15°, beginning at 30° above the northwest horizon, and the pictured fireball was quite weak. Despite this, the data was sufficient for the calculations.
The meteoroid grazed Earth's atmosphere quite gently (in comparison to, for example, the 1972 Great Daylight Fireball above the United States and Canada). It became visible north of Uherský Brod, Czechoslovakia, at a height of 103.7 km, approaching the Earth's surface to 98.67 km[note 2] northeast of Wrocław, Poland, and disappearing from sight at a height of 100.4 km north of Poznań, Poland. It would probably still have been visible until it reached a height of 110 km above the southern Baltic Sea.
The meteoroid's absolute magnitude (the apparent magnitude it would have at an altitude of 100 km at the observer's zenith) was approximately −6 and did not vary significantly during the few seconds of observation. It traveled a distance of 409 km in 9.8 seconds during the time it was observed. It moved at a speed of 41.74 km per second,[note 3] which did not change measurably during the flight. Jiří Borovička and Zdeněk Ceplecha from the Ondřejov Observatory in Czechoslovakia estimated that the deceleration caused by the friction of the atmosphere reached only 1.7 m/s2 at the fireball's perigee (closest approach to Earth), and its velocity was reduced by only 0.012 km per second (less than 0.03%). This corresponds well with computer simulations provided by D. W. Olson, R. L. Doescher and K. M. Watson at the Southwest Texas State University, who concluded that the deceleration was less than 0.5 m/s2 except for a few seconds near perigee. This small loss of speed, 12 m per second, corresponded to a loss of kinetic specific energy (in the earth's frame of reference) of 0.5 MJ/kg, which was converted to heat (and perhaps sound). The change in the object's velocity vector due to Earth's gravity during the hours it was in the earth's vicinity was on the order of kilometres per second (see Orbit section).
The software also calculated the fireball's instantaneous apparent magnitude at the ground. The computation started and ended with heights of approximately 250 km, long before and after the cameras of the European Fireball Network could observe it. Its apparent magnitude started at a value of +5.7 and it became brighter quite quickly. The program gave an apparent magnitude of −5.7 when it was seen by one camera and −6.3 at perigee. The fireball subsequently dimmed, with an apparent magnitude of −5.4 when it was last seen by the cameras and a final calculated value of +6.0 at a height of 257 km. These values are not entirely certain, because the program worked with the simplified assumption that the luminous efficacy of the fireball did not change along the track. The starting apparent magnitude is not far from the naked eye visibility limits. For example, faint stars of the magnitude +6 can be observed only in dark rural areas approximately 150 km away from large cities. This magnitude corresponds to the apparent magnitude of Uranus. At its brightest, it was several times as bright as the maximum brightness of Venus.
|Velocity[note 3]||41.74 km/s||41.74 km/s||41.74 km/s|
|Height||103.7 km||98.67 km||100.4 km|
The meteoroid was a type I fireball, i.e. an ordinary chondrite. When it entered Earth's atmosphere its mass was about 44 kg, which was estimated on the basis of the measured values of its absolute magnitude and velocity. From the known bulk densities of ordinary chondrites (3.40 ± 0.15 g/cm³ for H group ordinary chondrites, 3.40 ± 0.15 g/cm³ for L group and 3.29 ± 0.17 g/cm³ for LL group) we get the approximate diameter of the meteoroid between 28.5 and 30 cm. During the encounter it lost approximately 350 g. Computer simulations showed that it started losing mass approximately at the moment it became visible to the cameras of the European Fireball Network, at a height of 100.6 km. Losing of mass lasted 35 seconds, until it reached a height of 215.7 km. Its surface melted and solidified again after leaving, which means its surface became a typical meteoritic fusion crust.
The meteoroid was not dangerous to life on Earth. Even if it had headed towards lower parts of the atmosphere it would have heated so much that it would have exploded high above the ground and only some small particles (meteorites) eventually might have made it to Earth's surface.
Because the fireball was recorded by two cameras of the European Fireball Network, it was possible to calculate the trajectory of its flight through the atmosphere, and afterward also the characteristics of both its pre- and post-encounter orbit in the Solar System. The calculations were published by Czech astronomers Pavel Spurný, Zdeněk Ceplecha, and Jiří Borovička of the Ondřejov Observatory, who specialize in meteor observations. They demonstrated that the swing by the earth significantly altered the meteoroid's orbit. Its aphelion (the farthest it travels from the Sun) and orbital period were lowered to almost half of their original values. The object was initially in a highly inclined orbit (71°) and ended in an orbit with a slightly higher inclination (74°).
|Orbital characteristics||Before encounter||After encounter|
|Semi-major axis||2.72 ± 0.08 AU||1.87 ± 0.03 AU|
|Orbital eccentricity||0.64 ± 0.01||0.473 ± 0.009|
|Perihelion||0.9923 ± 0.0001 AU||0.9844 ± 0.0002 AU|
|Aphelion||4.45 ± 0.15 AU||2.76 ± 0.07 AU|
|Argument of periapsis||9.6 ± 0.1°||16.6 ± 0.2°|
|Longitude of the ascending node||19.671°||19.671°|
|Orbital inclination||71.4 ± 0.2°||74.4 ± 0.2°|
|Orbital period||4.5 ± 0.2 years||2.56 ± 0.06 years|
Approximately every 2.5 or 2.6 years, the object comes back to the point in the solar system where the 1990 encounter occurred, and the earth comes back to the same point every year. The period is not known precisely enough to predict when the next encounter between the two will occur.
Although entries of meteoroids into Earth's atmosphere are very common, recording a similar flight through the upper layers of the atmosphere is quite rare. Probably the first one reliably verified happened on 20 July 1860 above the American state of New York. The Czechoslovak–Polish fireball is sometimes compared to the 1972 Great Daylight Fireball above Utah, the United States, and Alberta, Canada, which is the first scientifically observed and studied event of this type. The 1972 fireball was more than a thousand times as massive and it got 40 km closer to Earth's surface. Observational data from both of them helped to develop a method for computing the grazing trajectories of such bodies, which was later used when calculating the trajectory of another Earth-grazing meteoroid, observed on 29 March 2006 above Japan.
- The record is in Universal Time (UT), local Central European Time (CET) was 1 hour later.
- That is just below the Kármán line, lying at the height of 100 km and considered to be the boundary of Earth's atmosphere.
- This is the observed velocity. Geocentric velocity (i.e. velocity relative to the Earth, whose orbital velocity is about 30 km per second) was 40.22 km per second.
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