Szablon:Bland (2006) - Historia wersji

Wiki woreczko o 19:59, 9 cze 2026

2026-06-09T19:59:14Z

← poprzednia wersja		Wersja z 19:59, 9 cze 2026
Linia 1:		Linia 1:
-	Bland Philip A., Artemieva Natalya A., (2006), '''The rate of small impacts on Earth''', ''Meteoritics & Planetary Science'', vol. 41(4), 2006, s. 607–631 ({{!abs-ilink\|:Szablon:Bland (2006)}}). Plik {{!doi\|10.1111/j.1945-5100.2006.tb00485.x}}; plik {{!ADS\|a=2006M&PS...41..607B}}.<noinclude>	+	Bland Philip A., Artemieva Natalya A., (2006), '''The rate of small impacts on Earth''', ''Meteoritics & Planetary Science'', vol. 41(4), 2006, s. 607–631 ({{!abs-ilink\|:Szablon:Bland (2006)}}). Plik {{!doi\|10.1111/j.1945-5100.2006.tb00485.x}}; plik {{Link-ADS\|a=2006M&PS...41..607B}}.<noinclude>

Wiki woreczko o 22:55, 4 lut 2022

2022-02-04T22:55:08Z

← poprzednia wersja		Wersja z 22:55, 4 lut 2022
Linia 1:		Linia 1:
-	Bland Philip A., Artemieva Natalya A., (2006), '''The rate of small impacts on Earth''', ''Meteoritics & Planetary Science'', vol. 41(4), 2006, s. 607–631. Plik {{!doi\|10.1111/j.1945-5100.2006.tb00485.x}}; plik {{!ADS\|a=2006M&PS...41..607B}} ~~({{!abs-ilink\|:Szablon:Bland (2006)}})~~.<noinclude>	+	Bland Philip A., Artemieva Natalya A., (2006), '''The rate of small impacts on Earth''', ''Meteoritics & Planetary Science'', vol. 41(4), 2006, s. 607–631 ({{!abs-ilink\|:Szablon:Bland (2006)}}). Plik {{!doi\|10.1111/j.1945-5100.2006.tb00485.x}}; plik {{!ADS\|a=2006M&PS...41..607B}}.<noinclude>
		+

	----		----

Wiki woreczko o 09:49, 15 maj 2018

2018-05-15T09:49:28Z

← poprzednia wersja		Wersja z 09:49, 15 maj 2018
Linia 4:		Linia 4:
	'''Abstract:''' Asteroids tens to hundreds of meters in diameter constitute the most immediate impact hazard to human populations, yet the rate at which they arrive at Earth's surface is poorly known. Astronomic observations are still incomplete in this size range; impactors are subjected to disruption in Earth's atmosphere, and unlike the Moon, small craters on Earth are rapidly eroded. In this paper, we first model the atmospheric behavior of iron and stony bodies over the mass range 1–10<sup>12</sup> kg (size range 6 cm – 1 km) taking into account deceleration, ablation, and fragmentation. Previous models in meteoritics deal with rather small masses (<10<sup>5</sup>–10<sup>6</sup> kg) with the aim of interpreting registered fireballs in atmosphere, or with substantially larger objects without taking into account asteroid disruption to model cratering processes. A few earlier attempts to model terrestrial crater strewn fields did not take into account possible cascade fragmentation. We have performed large numbers of simulations in a wide mass range, using both the earlier “pancake” models and also the separated fragments model to develop a statistical picture of atmosphere-bolide interaction for both iron and stony impactors with initial diameters up to ~1 km. Second, using a compilation of data for the flux at the upper atmosphere, we have derived a cumulative size-frequency distribution (SFD) for upper atmosphere impactors. This curve is a close fit to virtually all of the upper atmosphere data over 16 orders of magnitude. Third, we have applied our model results to scale the upper atmosphere curve to a flux at the Earth's surface, elucidating the impact rate of objects <1 km diameter on Earth.		'''Abstract:''' Asteroids tens to hundreds of meters in diameter constitute the most immediate impact hazard to human populations, yet the rate at which they arrive at Earth's surface is poorly known. Astronomic observations are still incomplete in this size range; impactors are subjected to disruption in Earth's atmosphere, and unlike the Moon, small craters on Earth are rapidly eroded. In this paper, we first model the atmospheric behavior of iron and stony bodies over the mass range 1–10<sup>12</sup> kg (size range 6 cm – 1 km) taking into account deceleration, ablation, and fragmentation. Previous models in meteoritics deal with rather small masses (<10<sup>5</sup>–10<sup>6</sup> kg) with the aim of interpreting registered fireballs in atmosphere, or with substantially larger objects without taking into account asteroid disruption to model cratering processes. A few earlier attempts to model terrestrial crater strewn fields did not take into account possible cascade fragmentation. We have performed large numbers of simulations in a wide mass range, using both the earlier “pancake” models and also the separated fragments model to develop a statistical picture of atmosphere-bolide interaction for both iron and stony impactors with initial diameters up to ~1 km. Second, using a compilation of data for the flux at the upper atmosphere, we have derived a cumulative size-frequency distribution (SFD) for upper atmosphere impactors. This curve is a close fit to virtually all of the upper atmosphere data over 16 orders of magnitude. Third, we have applied our model results to scale the upper atmosphere curve to a flux at the Earth's surface, elucidating the impact rate of objects <1 km diameter on Earth.

-	We find that iron meteorites >5 times 10<sup>4</sup> kg (2.5 m) arrive at the Earth's surface approximately once every 50 years. Iron bodies a few meters in diameter (10<sup>5</sup>–10<sup>6</sup> kg), which form craters ~100 m in diameter, will strike the Earth's land area every 500 years. Larger bodies will form craters 0.5 km in diameter every 20,000 years, and craters 1 km in diameter will be formed on the Earth's land area every 50,000 years. Tunguska events (low-level atmospheric disruption of stony bolides >10<sup>8</sup> kg) may occur every 500 years. Bodies capable of producing hazardous tsunami (~200 m diameter projectiles) should strike the Earth's surface every ~100,000 years. This data also allows us to assess the completeness of the terrestrial crater record for a given area over a given time interval.	+	We find that iron meteorites >5 times 10<sup>4</sup> kg (2.5 m) arrive at the Earth's surface approximately once every 50 years. Iron bodies a few meters in diameter (10<sup>5</sup>–10<sup>6</sup> kg), which form craters ~100 m in diameter, will strike the Earth's land area every 500 years. Larger bodies will form craters 0.5 km in diameter every 20,000 years, and craters 1 km in diameter will be formed on the Earth's land area every 50,000 years. Tunguska events{{MBD-record\|name=Tunguska}} (low-level atmospheric disruption of stony bolides >10<sup>8</sup> kg) may occur every 500 years. Bodies capable of producing hazardous tsunami (~200 m diameter projectiles) should strike the Earth's surface every ~100,000 years. This data also allows us to assess the completeness of the terrestrial crater record for a given area over a given time interval.
	{{Przypisy \|ncol=1}}		{{Przypisy \|ncol=1}}
	[[Category:Bibliografia (szablony)\|{{PAGENAME}}]]		[[Category:Bibliografia (szablony)\|{{PAGENAME}}]]
	</noinclude>		</noinclude>

Wiki woreczko o 15:17, 21 lut 2018

2018-02-21T15:17:07Z

← poprzednia wersja		Wersja z 15:17, 21 lut 2018
Linia 2:		Linia 2:

	----		----
-	'''Abstract:''' Asteroids tens to hundreds of meters in diameter constitute the most immediate impact hazard to human populations, yet the rate at which they arrive at Earth's surface is poorly known. Astronomic observations are still incomplete in this size range; impactors are subjected to disruption in Earth's atmosphere, and unlike the Moon, small craters on Earth are rapidly eroded. In this paper, we first model the atmospheric behavior of iron and stony bodies over the mass range 1–10<sup>12</sup> kg (size range 6 cm~~<sup>-~~1~~</sup>~~ km) taking into account deceleration, ablation, and fragmentation. Previous models in meteoritics deal with rather small masses (<10<sup>5</sup>–10<sup>6</sup> kg) with the aim of interpreting registered fireballs in atmosphere, or with substantially larger objects without taking into account asteroid disruption to model cratering processes. A few earlier attempts to model terrestrial crater strewn fields did not take into account possible cascade fragmentation. We have performed large numbers of simulations in a wide mass range, using both the earlier “pancake” models and also the separated fragments model to develop a statistical picture of atmosphere-bolide interaction for both iron and stony impactors with initial diameters up to ~1 km. Second, using a compilation of data for the flux at the upper atmosphere, we have derived a cumulative size-frequency distribution (SFD) for upper atmosphere impactors. This curve is a close fit to virtually all of the upper atmosphere data over 16 orders of magnitude. Third, we have applied our model results to scale the upper atmosphere curve to a flux at the Earth's surface, elucidating the impact rate of objects <1 km diameter on Earth.	+	'''Abstract:''' Asteroids tens to hundreds of meters in diameter constitute the most immediate impact hazard to human populations, yet the rate at which they arrive at Earth's surface is poorly known. Astronomic observations are still incomplete in this size range; impactors are subjected to disruption in Earth's atmosphere, and unlike the Moon, small craters on Earth are rapidly eroded. In this paper, we first model the atmospheric behavior of iron and stony bodies over the mass range 1–10<sup>12</sup> kg (size range 6 cm – 1 km) taking into account deceleration, ablation, and fragmentation. Previous models in meteoritics deal with rather small masses (<10<sup>5</sup>–10<sup>6</sup> kg) with the aim of interpreting registered fireballs in atmosphere, or with substantially larger objects without taking into account asteroid disruption to model cratering processes. A few earlier attempts to model terrestrial crater strewn fields did not take into account possible cascade fragmentation. We have performed large numbers of simulations in a wide mass range, using both the earlier “pancake” models and also the separated fragments model to develop a statistical picture of atmosphere-bolide interaction for both iron and stony impactors with initial diameters up to ~1 km. Second, using a compilation of data for the flux at the upper atmosphere, we have derived a cumulative size-frequency distribution (SFD) for upper atmosphere impactors. This curve is a close fit to virtually all of the upper atmosphere data over 16 orders of magnitude. Third, we have applied our model results to scale the upper atmosphere curve to a flux at the Earth's surface, elucidating the impact rate of objects <1 km diameter on Earth.

	We find that iron meteorites >5 times 10<sup>4</sup> kg (2.5 m) arrive at the Earth's surface approximately once every 50 years. Iron bodies a few meters in diameter (10<sup>5</sup>–10<sup>6</sup> kg), which form craters ~100 m in diameter, will strike the Earth's land area every 500 years. Larger bodies will form craters 0.5 km in diameter every 20,000 years, and craters 1 km in diameter will be formed on the Earth's land area every 50,000 years. Tunguska events (low-level atmospheric disruption of stony bolides >10<sup>8</sup> kg) may occur every 500 years. Bodies capable of producing hazardous tsunami (~200 m diameter projectiles) should strike the Earth's surface every ~100,000 years. This data also allows us to assess the completeness of the terrestrial crater record for a given area over a given time interval.		We find that iron meteorites >5 times 10<sup>4</sup> kg (2.5 m) arrive at the Earth's surface approximately once every 50 years. Iron bodies a few meters in diameter (10<sup>5</sup>–10<sup>6</sup> kg), which form craters ~100 m in diameter, will strike the Earth's land area every 500 years. Larger bodies will form craters 0.5 km in diameter every 20,000 years, and craters 1 km in diameter will be formed on the Earth's land area every 50,000 years. Tunguska events (low-level atmospheric disruption of stony bolides >10<sup>8</sup> kg) may occur every 500 years. Bodies capable of producing hazardous tsunami (~200 m diameter projectiles) should strike the Earth's surface every ~100,000 years. This data also allows us to assess the completeness of the terrestrial crater record for a given area over a given time interval.

Wiki woreczko o 15:10, 21 lut 2018

2018-02-21T15:10:55Z

← poprzednia wersja		Wersja z 15:10, 21 lut 2018
Linia 1:		Linia 1:
-	Bland Philip A., Artemieva Natalya A., (2006), '''The rate of small impacts on Earth''', ''Meteoritics & Planetary Science'', vol. 41(4), 2006, s. 607–631. Plik {{!doi\|10.1111/j.1945-5100.2006.tb00485.x}}; plik {{!ADS\|a=2006M&PS...41..607B}}.<noinclude>	+	Bland Philip A., Artemieva Natalya A., (2006), '''The rate of small impacts on Earth''', ''Meteoritics & Planetary Science'', vol. 41(4), 2006, s. 607–631. Plik {{!doi\|10.1111/j.1945-5100.2006.tb00485.x}}; plik {{!ADS\|a=2006M&PS...41..607B}} ({{!abs-ilink\|:Szablon:Bland (2006)}}).<noinclude>
		+
		+	----
		+	'''Abstract:''' Asteroids tens to hundreds of meters in diameter constitute the most immediate impact hazard to human populations, yet the rate at which they arrive at Earth's surface is poorly known. Astronomic observations are still incomplete in this size range; impactors are subjected to disruption in Earth's atmosphere, and unlike the Moon, small craters on Earth are rapidly eroded. In this paper, we first model the atmospheric behavior of iron and stony bodies over the mass range 1–10<sup>12</sup> kg (size range 6 cm<sup>-1</sup> km) taking into account deceleration, ablation, and fragmentation. Previous models in meteoritics deal with rather small masses (<10<sup>5</sup>–10<sup>6</sup> kg) with the aim of interpreting registered fireballs in atmosphere, or with substantially larger objects without taking into account asteroid disruption to model cratering processes. A few earlier attempts to model terrestrial crater strewn fields did not take into account possible cascade fragmentation. We have performed large numbers of simulations in a wide mass range, using both the earlier “pancake” models and also the separated fragments model to develop a statistical picture of atmosphere-bolide interaction for both iron and stony impactors with initial diameters up to ~1 km. Second, using a compilation of data for the flux at the upper atmosphere, we have derived a cumulative size-frequency distribution (SFD) for upper atmosphere impactors. This curve is a close fit to virtually all of the upper atmosphere data over 16 orders of magnitude. Third, we have applied our model results to scale the upper atmosphere curve to a flux at the Earth's surface, elucidating the impact rate of objects <1 km diameter on Earth.
		+
		+	We find that iron meteorites >5 times 10<sup>4</sup> kg (2.5 m) arrive at the Earth's surface approximately once every 50 years. Iron bodies a few meters in diameter (10<sup>5</sup>–10<sup>6</sup> kg), which form craters ~100 m in diameter, will strike the Earth's land area every 500 years. Larger bodies will form craters 0.5 km in diameter every 20,000 years, and craters 1 km in diameter will be formed on the Earth's land area every 50,000 years. Tunguska events (low-level atmospheric disruption of stony bolides >10<sup>8</sup> kg) may occur every 500 years. Bodies capable of producing hazardous tsunami (~200 m diameter projectiles) should strike the Earth's surface every ~100,000 years. This data also allows us to assess the completeness of the terrestrial crater record for a given area over a given time interval.
	{{Przypisy \|ncol=1}}		{{Przypisy \|ncol=1}}
	[[Category:Bibliografia (szablony)\|{{PAGENAME}}]]		[[Category:Bibliografia (szablony)\|{{PAGENAME}}]]
	</noinclude>		</noinclude>

Wiki woreczko: Utworzył nową stronę „Bland Philip A., Artemieva Natalya A., (2006), '''The rate of small impacts on Earth''', ''Meteoritics & Planetary Science'', vol. 41(4), 2006, s. 607–631. Plik {{!do...”

2018-02-21T09:38:44Z

Utworzył nową stronę „Bland Philip A., Artemieva Natalya A., (2006), '''The rate of small impacts on Earth''', ''Meteoritics & Planetary Science'', vol. 41(4), 2006, s. 607–631. Plik {{!do...”

Nowa strona

Bland Philip A., Artemieva Natalya A., (2006), '''The rate of small impacts on Earth''', ''Meteoritics & Planetary Science'', vol. 41(4), 2006, s. 607–631. Plik {{!doi|10.1111/j.1945-5100.2006.tb00485.x}}; plik {{!ADS|a=2006M&PS...41..607B}}.<noinclude>
{{Przypisy |ncol=1}}
[[Category:Bibliografia (szablony)|{{PAGENAME}}]]
</noinclude>