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Articles de revues sur le sujet « Meteoroid stream »

Auteur : Grafiati

Publié le 8 juin 2024

Mis à jour le 31 juillet 2025

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1

Wiliams, I. P. "The Dynamics of Meteoroid Streams." Symposium - International Astronomical Union 152 (1992): 299–313. http://dx.doi.org/10.1017/s0074180900091312.

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Meteor showers are seen at regular and frequent intervals on Earth. They are caused by meteoroids (that is small dust grains) in a coherent stream, all moving on similar heliocentric orbits, burning up on encountering the atmosphere of the Earth. Such streams contain 1012 or more meteoroids, with the mass of the visible meteoroids ranging up to about 1 g. The main evolutionary effect on such streams is gravitational perturbations by the planets. Though grain-grain collision may be catastrophic for the two grains involved, it has no effect on the remainder of the stream, other than the fact tha

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2

Kokhirova, G. I., and P. B. Babadzhanov. "Current Knowledge of Objects Approaching the Earth." Астрономический вестник 57, no. 5 (2023): 458–78. http://dx.doi.org/10.31857/s0320930x23050031.

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Modern ideas about objects approaching the Earth are discussed. This population includes near-Earth asteroids (NEAs), including potentially hazardous asteroids, short-period comets, meteoroid streams, and large sporadic meteoroids. An overview is given of the currently available information on the dynamic and physical properties of NEAs and comets. Almost 5% of the currently known NEAs are extinct cometary nuclei or their fragments. Being outwardly similar with true asteroids, they differ markedly in their dynamic and physical properties. In order to distinguish between these groups of objects

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Cukier, W. Z., and J. R. Szalay. "Formation, Structure, and Detectability of the Geminids Meteoroid Stream." Planetary Science Journal 4, no. 6 (2023): 109. http://dx.doi.org/10.3847/psj/acd538.

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Abstract The Geminids meteoroid stream produces one of the most intense meteor showers at Earth. It is an unusual stream in that its parent body is understood to be an asteroid, (3200) Phaethon, unlike most streams, which are formed via ongoing cometary activity. Until recently, our primary understanding of this stream came from Earth-based measurements of the Geminids meteor shower. However, the Parker Solar Probe (PSP) spacecraft has transited near the core of the stream close to its perihelion and provides a new platform to better understand this unique stream. Here, we create a dynamical m

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4

Ryabova, Galina O. "Averaged changes in the orbital elements of meteoroids due to Yarkovsky-Radzievskij force." Proceedings of the International Astronomical Union 9, S310 (2014): 160–61. http://dx.doi.org/10.1017/s1743921314008114.

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AbstractYarkovsky-Radzievskij effect exceeds the Poynting-Robertson effect in the perturbing action on particles larger than 100 μm. We obtained formulae for averaged changes in a meteoroid's Keplerian orbital elements and used them to estimate dispersion in the Geminid meteoroid stream. It was found that dispersion in semi-major axis of the model shower increased nearly three times on condition that meteoroids rotation is fast, and the rotation axis is stable.

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Rudawska, Regina, and Tadeusz J. Jopek. "Study of meteoroid stream identification methods." Proceedings of the International Astronomical Union 5, S263 (2009): 253–56. http://dx.doi.org/10.1017/s1743921310001870.

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AbstractWe have tested the reliability of various meteoroid streams identification methods. We used a numerically generated set of meteoroid orbits (a stream component and a sporadic background) that were searched for streams using several methods.

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6

Moorhead, Althea V., Tiffany D. Clements, and Denis Vida. "Realistic gravitational focusing of meteoroid streams." Monthly Notices of the Royal Astronomical Society 494, no. 2 (2020): 2982–94. http://dx.doi.org/10.1093/mnras/staa719.

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ABSTRACT The number density and flux of a meteoroid stream is enhanced near a massive body due to the phenomenon known as gravitational focusing. The greatest enhancement occurs directly opposite the massive body from the stream radiant: as an observer approaches this location, the degree of focusing is unbound for a perfectly collimated stream. However, real meteoroid streams exhibit some dispersion in radiant and speed that will act to eliminate this singularity. In this paper, we derive an analytic approximation for this smoothing that can be used in meteoroid environment models and is base

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Babadzhanov, P. B., and Yu V. Obrubov. "Dynamics and Spatial Shape of Short-Period Meteoroid Streams." Highlights of Astronomy 8 (1989): 287–93. http://dx.doi.org/10.1017/s1539299600007905.

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AbstractAt the early stage of evolution the meteoroid streams may be considered as elliptical rings of relatively small thickness. The influence of planetary perturbations can essentially increase the stream width and its thickness. As a result one stream may produce several couples of meteor showers active in different seasons of the year. 22 short-period meteoroid streams under review may theoretically produce 104 meteor showers. The existence of 67 is confirmed by observations.

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8

Wu, Zidian, and Iwan P. Williams. "The Quadrantid Stream, Chaos or Not?" Symposium - International Astronomical Union 152 (1992): 329–32. http://dx.doi.org/10.1017/s0074180900091348.

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The Quadrantid stream covers a region of space which contains many strong resonances and commensurabilities with the Jovian orbit. We have numerically integrated the orbital evolution of over one hundred actual meteoroids backwards to BC 5000. The evolution is quit complex, but most of the meteoroids are quite well behaved with rapid but smooth changes in the orbital elements. One meteoroid however shows sharp sudden changes in its orbital parameters and these changes are generally indicative of the presence of chaos.

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9

Froeschlé, CL, T. J. Jopek, and G. B. Valsecchi. "The Use of Geocentric Variables to Search for Meteoroid Streams and Their Parents." International Astronomical Union Colloquium 172 (1999): 55–64. http://dx.doi.org/10.1017/s0252921100072419.

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AbstractA set of geocentric variables suitable for the identification of meteoroid streams has been recently proposed and successfully applied to photographic meteor orbits. We describe these variables and the secular invariance of some of them, and discuss their use to improve the search for meteoroid stream parents.

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10

Harris, Nathan W. "The Formation and Evolution of the Perseid Meteoroid Stream." International Astronomical Union Colloquium 150 (1996): 101–4. http://dx.doi.org/10.1017/s0252921100501341.

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AbstractThe orbital evolution of two modelled ‘Perseid’ meteoroid streams is investigated using direct numerical integration techniques. We conclude that, in the absence of significant meteoroid velocity determination errors, the observed meteoroid orbital semi-major axis distribution is a direct consequence of the cometary ejection process and not due to subsequent orbital evolution. A high ejection-velocity (~ 0.6 km s-1) model stream succeeds in reproducing the observations. Conclusions are made concerning how the orbital stability of Earth-orbit-intersecting Perseid metecroids varies with

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11

А.К., Терентьева,, and Барабанов, С.И. "Meteorite Križevci (Croatia) and meteoroid stream Cancrid." Научные труды Института астрономии РАН, no. 4 (December 16, 2022): 241–43. http://dx.doi.org/10.51194/inasan.2022.7.4.004.

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На основании анализа более 500 орбит метеороидных и болидных роев по опубликованным каталогам нами была установлена связь метеорита Križevci, порожденного болидом 4 февраля 2011 г. над Хорватией [1] с метеороидным роем Канкрид (No. 166 (а), [2, 3]). Известный критерий Саутворта-Хокинса дает величину D SH = 0.128, которая является вполне приемлемой для достаточно хорошего согласия орбит метеорита и роя. Динамический параметр Тиссерана указывает на астероидное происхождение роя и метеорита. Таким образом, выявлен еще один метеоритообразующий рой, который дополняет список 14 метеоритообразующих р

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12

Matlovič, Pavol, Leonard Kornoš, Martina Kováčová, Juraj Tóth, and Javier Licandro. "Characterization of the June epsilon Ophiuchids meteoroid stream and the comet 300P/Catalina." Astronomy & Astrophysics 636 (April 2020): A122. http://dx.doi.org/10.1051/0004-6361/202037727.

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Aims. Prior to 2019, the June epsilon Ophiuchids (JEO) were known as a minor unconfirmed meteor shower with activity that was considered typically moderate for bright fireballs. An unexpected bout of enhanced activity was observed in June 2019, which even raised the possibility that it was linked to the impact of the small asteroid 2019 MO near Puerto Rico. Early reports also point out the similarity of the shower to the orbit of the comet 300P/Catalina. We aim to analyze the orbits, emission spectra, and material strengths of JEO meteoroids to provide a characterization of this stream, identi

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13

Hughes, D. W. "The Grigg-Skjellerupid meteoroid stream." Monthly Notices of the Royal Astronomical Society 257, no. 1 (1992): 25P—28P. http://dx.doi.org/10.1093/mnras/257.1.25p.

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14

Steel, Duncan. "Meteoroid Streams." Symposium - International Astronomical Union 160 (1994): 111–26. http://dx.doi.org/10.1017/s0074180900046490.

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Meteoroid streams, producing meteor showers if some part of the stream has a node near 1 AU, have complex structures which are only just beginning to be understood. The old simplistic idea of a narrow loop being formed about the orbit of a parent comet with one, or possibly two, terrestrial intersection(s) is now being replaced by the recognition that their dynamical evolution may render convoluted and distorted ribbon shapes with eight or more distinct showers being generated. As such the streams are excellent tracers of the sorts of orbital evolution which may be undergone by larger objects

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15

Wu, Z., and I. P. Williams. "On the Quadrantid meteoroid stream complex." Monthly Notices of the Royal Astronomical Society 259, no. 4 (1992): 617–28. http://dx.doi.org/10.1093/mnras/259.4.617.

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16

Williams, I. P., and Z. Wu. "The Quadrantid meteoroid stream and Comet 1491I." Monthly Notices of the Royal Astronomical Society 264, no. 3 (1993): 659–64. http://dx.doi.org/10.1093/mnras/264.3.659.

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17

Jones, J., B. A. McIntosh, and R. L. Hawkes. "The age of the Orionid meteoroid stream." Monthly Notices of the Royal Astronomical Society 238, no. 1 (1989): 179–91. http://dx.doi.org/10.1093/mnras/238.1.179.

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18

Williams, I. P., and S. J. Collander-Brown. "The parent of the Quadrantid meteoroid stream." Monthly Notices of the Royal Astronomical Society 294, no. 1 (1998): 127–38. http://dx.doi.org/10.1046/j.1365-8711.1998.01168.x.

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19

Soja, R. H., W. J. Baggaley, P. Brown, and D. P. Hamilton. "Dynamical resonant structures in meteoroid stream orbits." Monthly Notices of the Royal Astronomical Society 414, no. 2 (2011): 1059–76. http://dx.doi.org/10.1111/j.1365-2966.2011.18442.x.

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20

Ryabova, G. O. "The mass of the Geminid meteoroid stream." Planetary and Space Science 143 (September 2017): 125–31. http://dx.doi.org/10.1016/j.pss.2017.02.005.

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21

Cevolani, G., G. Bortolotti, L. Foschini, et al. "Radar observations of the Geminid meteoroid stream." Earth, Moon, and Planets 68, no. 1-3 (1995): 247–55. http://dx.doi.org/10.1007/bf00671513.

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22

Obrubov, Yu V. "A new octuple Earth-crossing meteoroid stream." Earth, Moon, and Planets 68, no. 1-3 (1995): 443–49. http://dx.doi.org/10.1007/bf00671538.

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23

Ryabova, G. O. "Mathematical modelling of the Geminid meteoroid stream." Monthly Notices of the Royal Astronomical Society 375, no. 4 (2007): 1371–80. http://dx.doi.org/10.1111/j.1365-2966.2007.11392.x.

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24

Moser, Danielle E., and William J. Cooke. "Updates to the MSFC Meteoroid Stream Model." Earth, Moon, and Planets 102, no. 1-4 (2007): 285–91. http://dx.doi.org/10.1007/s11038-007-9159-1.

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25

Li, Guangyu, and Haibin Zhao. "Dynamical simulation of the motion of Leonid Meteoric Stream." International Journal of Modern Physics D 11, no. 07 (2002): 1021–34. http://dx.doi.org/10.1142/s0218271802002530.

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The Leonid meteoric shower has been the most famous meteoric shower. The main characteristics of the stream are well known, being very spectacular displays in recent years. In this paper, the authors aim at searching the dynamic origin of the second peak of Leonids 1998. Firstly a dynamic model of the solar system is constructed, considering the perturbations of the nine major planets and the Moon, Post-Newtonian effects and the figure effect of the Earth. For the motions of cornet and meteoroid, the non-gravitational effect and radiation pressure effect are taken into account separately. Seco

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26

Hughes, David W. "The mass distribution of comets and meteoroid streams and the shower/sporadic ratio in the incident visual meteoroid flux." Monthly Notices of the Royal Astronomical Society 245, no. 2 (1990): 198. http://dx.doi.org/10.1093/mnras/245.2.198.

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Summary The large dust particles that comets emit as they decay produce meteoroid streams. If the Earth passes close to the centre of a meteoroid stream, a shower of meteors is produced in the atmosphere and the intensity of this shower can be quantified by the maximum zenithal hour rate (ZHR) of the meteors that are observed. If, as seems reasonable, the dust/snow mass ratio and the mass distribution of the dust particles are similar in all comets, then comets and meteoroid streams are expected to have similar mass distribution indices. This expectation has been confirmed for the more massive

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27

Baggaley, Jack W., and R. G. T. Bennett. "The Meteoroid Orbit Facility AMOR: Recent Developments." International Astronomical Union Colloquium 150 (1996): 65–70. http://dx.doi.org/10.1017/s0252921100501286.

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AbstractSome 3 x 105radar meteoroid orbits have been secured to date by the AMOR, project since its inception in 1990. For many types of study it is important to realize a high angular resolution; for example to probe more incisively meteoroid stream orbital structure in order better to determine the rôle of the various processes controlling stream dynamics. The orbital precision of AMOR has been enhanced by developing a new dual spacing interferometer using single channel phase detection. In addition, a Doppler-sensing facility has been incorporated to record simultaneously data concerning mi

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Williams, I. P., and D. C. Jones. "How useful is the 'mean stream' in discussing meteoroid stream evolution?" Monthly Notices of the Royal Astronomical Society 375, no. 2 (2007): 595–603. http://dx.doi.org/10.1111/j.1365-2966.2006.11297.x.

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29

Margonis, A., A. Christou, and J. Oberst. "Characterisation of the Perseid meteoroid stream through SPOSH observations between 2010–2016." Astronomy & Astrophysics 626 (June 2019): A25. http://dx.doi.org/10.1051/0004-6361/201834867.

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We have characterised the Perseid meteoroid stream from data acquired in a series of observing campaigns between 2010 and 2016. The data presented in this work were obtained by the Smart Panoramic Optical Sensor Head (SPOSH), an all-sky camera system designed to image faint transient noctilucent phenomena on dark planetary hemispheres. For the data reduction, a sophisticated software package was developed that utilises the high geometric and photometric quality of images obtained by the camera system. We identify 934 meteors as Perseids, observed over a long period between late July (~124°) an

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30

Galligan, D. P. "Radar meteoroid orbit stream searches using cluster analysis." Monthly Notices of the Royal Astronomical Society 340, no. 3 (2003): 899–907. http://dx.doi.org/10.1046/j.1365-8711.2003.06348.x.

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Tomko, D., and L. Neslušan. "Meteoroid-stream complex originating from comet 2P/Encke." Astronomy & Astrophysics 623 (February 25, 2019): A13. http://dx.doi.org/10.1051/0004-6361/201833868.

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Aims. We present a study of the meteor complex of the short-period comet 2P/Encke. Methods. For five perihelion passages of the parent comet in the past, we modeled the associated theoretical stream. Specifically, each of our models corresponds to a part of the stream characterized with a single value of the evolutionary time and a single value of the strength of the Poynting–Robertson effect. In each model, we follow the dynamical evolution of 10 000 test particles via a numerical integration. The integration was performed from the time when the set of test particles was assumed to be ejected

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Valsecchi, G. B., T. J. Jopek, and C. Froeschle. "Meteoroid stream identification: a new approach -- I. Theory." Monthly Notices of the Royal Astronomical Society 304, no. 4 (1999): 743–50. http://dx.doi.org/10.1046/j.1365-8711.1999.02264.x.

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Kaňuchová, Z., and L. Neslušan. "The parent bodies of the Quadrantid meteoroid stream." Astronomy & Astrophysics 470, no. 3 (2007): 1123–36. http://dx.doi.org/10.1051/0004-6361:20077329.

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Babadzhanov, P. B., I. P. Williams, and G. I. Kokhirova. "Near-Earth asteroids among the Piscids meteoroid stream." Astronomy & Astrophysics 479, no. 1 (2007): 249–55. http://dx.doi.org/10.1051/0004-6361:20078185.

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35

Svoreň, Ján, Luboš Neslušan, Zuzana Kaňuchová, and Vladimír Porubčan. "A Fine Structure of the Perseid Meteoroid Stream." Earth, Moon, and Planets 95, no. 1-4 (2005): 69–74. http://dx.doi.org/10.1007/s11038-005-2875-5.

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36

Ryabova, Galina O. "On mean motion resonances in the Geminid meteoroid stream." Planetary and Space Science 210 (January 2022): 105378. http://dx.doi.org/10.1016/j.pss.2021.105378.

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37

Babadzhanov, P. B., Zidian Wu, I. P. Williams, and D. W. Hughes. "The Leonids, Comet Biela and Biela's associated meteoroid stream." Monthly Notices of the Royal Astronomical Society 253, no. 1 (1991): 69–74. http://dx.doi.org/10.1093/mnras/253.1.69.

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Ryabova, G. O. "The comet Halley meteoroid stream: just one more model." Monthly Notices of the Royal Astronomical Society 341, no. 3 (2003): 739–46. http://dx.doi.org/10.1046/j.1365-8711.2003.06472.x.

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Brown, P., and J. Jones. "Dynamics of the Leonid Meteoroid Stream: a Numerical Approach." International Astronomical Union Colloquium 150 (1996): 113–16. http://dx.doi.org/10.1017/s0252921100501377.

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AbstractWe have simulated the evolution of the Leonid stream via numerical integration of 3 million test particles ejected from 55P/Tempel-Tuttle during five perihelion passages of that comet. Using the Whipple ejection velocity formula and a random ejection spread in true anomaly about the parent comet orbit inside 2.3 AU, we have followed the subsequent evolution of Leonid meteoroids differing by over 5 orders of magnitude in mass under the influence of radiation pressure and planetary perturbations. By comparing the model predictions of Leonid activity on a year by year basis with the avail

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Kornoš, Leonard, Juraj Tóth, Vladimír Porubčan, Jozef Klačka, Roman Nagy, and Regina Rudawska. "On the orbital evolution of the Lyrid meteoroid stream." Planetary and Space Science 118 (December 2015): 48–53. http://dx.doi.org/10.1016/j.pss.2015.05.001.

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Ryabova, G. O., V. A. Avdyushev, and I. P. Williams. "Asteroid (3200) Phaethon and the Geminid meteoroid stream complex." Monthly Notices of the Royal Astronomical Society 485, no. 3 (2019): 3378–85. http://dx.doi.org/10.1093/mnras/stz658.

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Ryabova, G. O. "A preliminary numerical model of the Geminid meteoroid stream." Monthly Notices of the Royal Astronomical Society 456, no. 1 (2015): 78–84. http://dx.doi.org/10.1093/mnras/stv2626.

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Jopek, T. J., R. Rudawska, and H. Pretka-Ziomek. "Calculation of the mean orbit of a meteoroid stream." Monthly Notices of the Royal Astronomical Society 371, no. 3 (2006): 1367–72. http://dx.doi.org/10.1111/j.1365-2966.2006.10770.x.

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Babadzhanov, P. B., I. P. Williams, and G. I. Kokhirova. "Near-Earth asteroids among the Iota Aquariids meteoroid stream." Astronomy & Astrophysics 507, no. 2 (2009): 1067–72. http://dx.doi.org/10.1051/0004-6361/200912936.

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Jopek, Tadeusz J., Regina Rudawska, and Przemysław Bartczak. "Meteoroid Stream Searching: The Use of the Vectorial Elements." Earth, Moon, and Planets 102, no. 1-4 (2007): 73–78. http://dx.doi.org/10.1007/s11038-007-9197-8.

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46

Maslov, Mikhail. "Gravitational Shifts and the Core of Perseid Meteoroid Stream." Earth, Moon, and Planets 117, no. 2-3 (2016): 93–100. http://dx.doi.org/10.1007/s11038-016-9483-4.

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47

Foschini, L., G. Cevolani, and G. Trivellone. "Radar observations of the Leonid meteoroid stream in 1994." Il Nuovo Cimento C 18, no. 3 (1995): 343–49. http://dx.doi.org/10.1007/bf02508565.

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Drolshagen, E., T. Ott, D. Koschny, et al. "Luminous efficiency of meteors derived from ablation model after assessment of its range of validity." Astronomy & Astrophysics 652 (August 2021): A84. http://dx.doi.org/10.1051/0004-6361/202140917.

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Context. The luminous efficiency, τ, can be used to compute the pre-atmospheric masses of meteoroids from corresponding recorded meteor brightnesses. The derivation of the luminous efficiency is non-trivial and is subject to biases and model assumptions. This has led to greatly varying results in the last decades of studies. Aims. The present paper aims to investigate how a reduction in various observational biases can be achieved to derive (more) reliable values for the luminous efficiency. Methods. A total of 281 meteors observed by the Fireball Recovery and InterPlanetary Observation Networ

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Williams, I. P. "JD23 The Leonid Meteor Storms:- Historical Significance and Upcoming Opportunities." Highlights of Astronomy 11, no. 2 (1998): 1003–4. http://dx.doi.org/10.1017/s1539299600019420.

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Without doubt, the Leonid stream is the most famous of all the known meteoroid streams. The reason for this is not hard to find, the display of meteors that it produces at times far surpassess anything that any other shower can produce. The showers of 1799, 1833 and 1966 all have numerous engravings or photographs recording the splendidness of the displays. The recorded history of the appearances of spectacular Leonid displays dates back for two millenia. Though the associated parent comet, 55/P Tempel-Tuttle, was only discovered in 1861.

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Терентьева, А. К., and С. И. Барабанов. "Fireball stream of the Glanerbrug meteorite. List of the 14 meteorite-producing fireball and meteoroid streams." Научные труды Института астрономии РАН, no. 3 (December 31, 2021): 69–73. http://dx.doi.org/10.51194/inasan.2021.6.3.001.

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Яркий болид -12. m 5, произведший метеорит Гланербруг, наблюдался над Нидерландами 7 апреля 1990 г. в 18 h 32 m 38 s UT. Первые определения орбит были очень приблизительными и требовали уточнения. М. Лангброк, проанализировав основные данные, получил новые уточненные элементы орбиты метеорита Гланербруг. Мы применили эту систему элементов в нашем исследовании. Проанализировав каталоги метеорных и болидных роев, мы нашли болидный рой η-Ursa-Majorids. Его орбитальные элементы соответствуют орбитальным элементам метеорита Гланербруг. Болидный рой η-Ursa-Majorids принадлежит 14 метеоритообразующим

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