Journal articles: 'Meteoroid stream'

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 that there are now two less grains in it. Solar radiation has some effect, but this can be included in the equations of motion. Because of the large numbers of particles involved, meteoroid streams represent a laboratory where many of our dynamical concepts can be tested.At a basic level, meteoroid streams represent a collective dynamical phenomenon in which all members display roughly the same behavior. One of the fundamental questions which can be investigated is whether the behavior of the mean orbit of the whole stream represents the mean behavior of the stream members. Within the boundaries of some meteor streams lie regions where the orbits are in high order resonance with Jupiter. This also represents a phenomenon of interest. Finally, the possibility exists that some streams are in chaotic regions and it is interesting to investigate whether or not meteoroids in such regions do display chaotic behavior.

2

Kokhirova, G. I., and P. B. Babadzhanov. "Current Knowledge of Objects Approaching the Earth." Астрономический вестник 57, no. 5 (September 1, 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, it is necessary to study both their dynamic and physical parameters. Some of the known meteoroid streams are shown to contain, along with the countless small meteoroids, also large extinct fragments of cometary nuclei, which are classified as NEAs. A meteoroid stream and such bodies belonging to it form together an asteroid–meteoroid complex. Observational and theoretical data are presented to confirm the modern understanding of near-Earth objects.

3

Cukier, W. Z., and J. R. Szalay. "Formation, Structure, and Detectability of the Geminids Meteoroid Stream." Planetary Science Journal 4, no. 6 (June 1, 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 model of the Geminids meteoroid stream, calibrate its total density to Earth-based measurements, and compare this model to recent observations of the dust environment near the Sun by PSP. For the formation mechanisms considered, we find with the exception of very near perihelion the core of the meteoroid stream predominantly lies interior to the orbit of its parent body and we expect grains in the stream to be ≳10 μm in radius. Data–model comparisons of the location of the stream relative to Phaethon’s orbit near perihelion are more consistent with a catastrophic formation scenario, with the core stream residing near or outside the orbit of its parent body consistent with PSP observations. This is in contrast to a cometary formation mechanism, where even near the Sun the meteoroid stream is interior to the orbit of its parent body. Finally, while PSP transits very near the core of the stream, the impact rate expected from Geminids meteoroids is orders of magnitude below the impact rates observed by PSP, and hence undetectable in situ. We similarly expect the upcoming DESTINY+ mission to be unable to detect appreciable quantities of Geminids grains far from (3200) Phaethon.

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 (July 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.

5

Rudawska, Regina, and Tadeusz J. Jopek. "Study of meteoroid stream identification methods." Proceedings of the International Astronomical Union 5, S263 (August 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.

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 (March 17, 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 based on real measurements of meteor shower radiant dispersion.

7

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.

8

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.

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.

10

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 роев, найденных нами ранее [4]. Эти рои имеют важное значение с точки зрения потенциальной опасности при встрече их с Землей. В работе приводится краткая информация о таком редком явлении, которое названо А. Брезиной [5] «цепным падением» метеоритов. Based on the analysis of more than 500 orbits of meteoroid and reball streams according to published catalogs, we established the connection of the Križevci meteorite generated by the bolide on February 4, 2011 over Croatia [1] with a meteoroid stream Cancrid (No. 166 (a), [2, 3]). The well-known Southworth-Hawkins criterion gives a value of D SH = 0.128, which is quite acceptable for a fairly good agreement of the orbits of the meteorite and the stream. The dynamic parameter of Tisserand indicates the asteroid origin of the stream and the meteorite. Thus, this is yet another meteorite-forming stream that complements the list of 14 meteorite-forming streams that we found earlier [4]. These streams have an signi cance in terms of potential danger when they approach the Earth. The paper provides brief information about such a rare phenomenon, which is called the “chain fall” of meteorites by A. Brezina [5].

11

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 initial orbital semi-major axis.

12

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

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13

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, identify its parent object, and evaluate its link to the impacting asteroid 2019 MO. Methods. Our analysis is based on a sample of 22 JEO meteor orbits and four emission spectra observed by the AMOS network at the Canary Islands and in Chile. The meteoroid composition was studied by spectral classification based on relative intensity ratios of Na, Mg, and Fe. Heliocentric orbits, trajectory parameters, and material strengths were determined for each meteor and the mean orbit and radiant of the stream were calculated. The link to potential parent objects was evaluated using a combination of orbital-similarity D-criteria and backwards integration of the orbit of comet 300P and the JEO stream. Results. We confirm the reports of an unexpected swarm of meteoroids originating in the JEO stream. JEO meteoroids have low material strengths characteristic for fragile cometary bodies, and they exhibit signs of a porous structure. The emission spectra reveal slightly increased iron content compared to all other measured cometary streams, but they are generally consistent with a primitive chondritic composition. Further dynamical analysis suggests that the JEO stream is likely to originate from comet 300P/Catalina and that it was formed within the last 1000 yr. Over longer timescales, the meteoroids in the stream move to chaotic orbits due to the turbulent orbital evolution of the comet. Our results also suggest that the impact of the small asteroid 2019 MO on June 22 was not connected to the JEO activity.

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 (asteroids and comets) in the inner solar system; indeed it is now known that objects presently observed as Apollo-type asteroids may also be the progenitors of streams.Searches for showers associated with newly-discovered possible parent objects may be carried out either via the calculation of theoretical meteor radiants (which have hitherto been derived using an untenable method), or through searches of catalogues of individual meteor orbits. In order to accomplish the latter, about 68,000 radar, photographic and TV meteor orbits from various programmes in the U.S.A., the former Soviet Union, Canada and Australia are available from the IAU Meteor Data Center, and more than 350,000 orbits of very faint meteors have been determined over the past three years using a new facility in New Zealand.The discovery amongst IRAS data of dust trails lagging behind comets has opened up a new way in which meteoroid streams may be investigated, although the relationship between these trails and the streams observed as meteor showers at the Earth is by no means clear at this stage. Similarly radar, radio and spacecraft impact observations of meteoroids near cometary nuclei have added to our knowledge.In spite of the improvement in our understanding of meteoroid streams over the past few years it is clear that there is much still to be done. The words of W.F. Denning in 1923 are still pertinent: “Few astronomers occupy themselves with the observation and investigation of meteors, and yet it is an attractive field of work offering inviting prospects of new discoveries”.

15

Wu, Z., and I. P. Williams. "On the Quadrantid meteoroid stream complex." Monthly Notices of the Royal Astronomical Society 259, no. 4 (December 15, 1992): 617–28. http://dx.doi.org/10.1093/mnras/259.4.617.

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Williams, I. P., and Z. Wu. "The Quadrantid meteoroid stream and Comet 1491I." Monthly Notices of the Royal Astronomical Society 264, no. 3 (October 1, 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 (May 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 (February 11, 1998): 127–38. http://dx.doi.org/10.1046/j.1365-8711.1998.01168.x.

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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 (March 21, 2011): 1059–76. http://dx.doi.org/10.1111/j.1365-2966.2011.18442.x.

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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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Cevolani, G., G. Bortolotti, L. Foschini, C. Franceschi, G. Grassi, G. Trivellone, A. Hajduk, and V. Porubčan. "Radar observations of the Geminid meteoroid stream." Earth, Moon, and Planets 68, no. 1-3 (January 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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Ryabova, G. O. "Mathematical modelling of the Geminid meteoroid stream." Monthly Notices of the Royal Astronomical Society 375, no. 4 (February 5, 2007): 1371–80. http://dx.doi.org/10.1111/j.1365-2966.2007.11392.x.

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Moser, Danielle E., and William J. Cooke. "Updates to the MSFC Meteoroid Stream Model." Earth, Moon, and Planets 102, no. 1-4 (October 23, 2007): 285–91. http://dx.doi.org/10.1007/s11038-007-9159-1.

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Li, Guangyu, and Haibin Zhao. "Dynamical simulation of the motion of Leonid Meteoric Stream." International Journal of Modern Physics D 11, no. 07 (August 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. Secondly, the orbit of Comet Tempel-Tuttle is determined by using the observation data of this apparition. Finally, assuming an isotropic ejection model of comet, the authors simulate the motion of the meteoric stream and discover that the particles aged 2-revolutions erupted with velocity 50m/s can befall Earth at 20h37m UT of Nov. 17, 1998, which form the main part of the second peak of Leonids 1998.

26

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 (February 21, 2007): 595–603. http://dx.doi.org/10.1111/j.1365-2966.2006.11297.x.

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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°) and mid-to-late August (~147°). The maximum meteor activity contributing to the annual shower was found at λ⊙ = 140°.08 ± 0°.07. The radiant of the shower was estimated at RA = 47°.2 and Dec = 57°.5 with a median error of 0°.6 and 0°.2, respectively. The mean population index of the shower between solar longitudes of 120°.68 and 145°.19 was r = 2.36 ± 0.05, showing strong temporal variation. A predicted outburst in shower activity for the night of August 11–12, 2016 was confirmed, with a peak observed 12.75 hr before the annual maximum at 23:30 ± 15′ UT. We measure a peak flux of 6.1 × 10−4 km−2 hr−1 for meteoroids of mass 1.6 × 10−2 g or more, appearing in the time period between 23:00 and 00:00 UT. We estimate the measured flux of the outburst meteoroids to be approximately twice as high as the annual meteoroid flux of the same mass. The population index of r = 2.19 ± 0.08, computed from the outburst Perseids in 2016, is higher than the value of r = 1.92 ± 0.06 derived from meteors observed in 2015 belonging to the annual Perseid shower which was active near the time of the outburst. A dust trail with an unusually high population index of r = 3.58 ± 0.24 was encountered in 2013 between solar longitudes 136°.261 and 137°.442. The relatively high r-value implies an encounter with a dust trail rich in low-mass particles.

28

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 (July 15, 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 comets and streams by comparing the distribution of shower ZHRs with the distribution of cometary masses. The later distribution is also used to predict the expected numbers of minor meteor showers, with low ZHRs, that are present in what was previously referred to as the sporadic background. It is concluded that on a typical ‘non-shower’ night, (20 ±3) per cent of the observed visual meteors belong to minor showers, and the remaining percentage are truly sporadic. Statistical variations in the numbers of massive short-period comets and thus massive meteoroid streams will lead to significant variations in the decay products of these objects. It is thus expected that this effect will cause the sporadic meteor flux and the brightness of the zodiacal cloud to vary by around 30-40 per cent over time periods of the order of 103-105 yr.

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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 middle atmospheric dynamics allowing better interpretation of the individual echo signals.

30

Galligan, D. P. "Radar meteoroid orbit stream searches using cluster analysis." Monthly Notices of the Royal Astronomical Society 340, no. 3 (April 11, 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 from the comet’s nucleus up to the present. At the end of the integration, we analyzed the mean orbital characteristics of those particles that approached the Earth’s orbit, and thus created a meteor shower or showers. Using the mean characteristics of the predicted shower, we attempted to select its real counterpart from each of five considered databases (one photographic, three video, and one radio-meteor). If at least one attempt was successful, the quality of the prediction was evaluated. Results. The modeled stream of 2P approaches the Earth’s orbit in several filaments with the radiant areas grouped in four cardinal directions of ecliptical showers. These groups of radiant areas are situated symmetrically with respect to the apex of the Earth’s motion around the Sun. Specifically, we found that showers #2, #17, #156, #172, #173, #215, #485, #624, #626, #628, #629, #632, #634, #635, #636, and #726 in the IAU-MDC list of all showers are dynamically related to 2P. In addition, we found five new 2P-related showers in the meteor databases considered.

32

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 (April 16, 1999): 743–50. http://dx.doi.org/10.1046/j.1365-8711.1999.02264.x.

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33

Kaňuchová, Z., and L. Neslušan. "The parent bodies of the Quadrantid meteoroid stream." Astronomy & Astrophysics 470, no. 3 (May 30, 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 (November 20, 2007): 249–55. http://dx.doi.org/10.1051/0004-6361:20078185.

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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 (September 14, 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 (November 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 (May 21, 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 available observations we have attempted to determine roughly the time of ejection associated with each Leonid storm occurrence and model the observed mass distribution. On the basis of the demonstrated accuracy of the model we make predictions regarding times of peak activity and relative strengths for the Leonid returns for each year during the latter part of the 1990s.

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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 (March 7, 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 (December 11, 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 (September 21, 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 (September 24, 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 (December 25, 2007): 73–78. http://dx.doi.org/10.1007/s11038-007-9197-8.

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Maslov, Mikhail. "Gravitational Shifts and the Core of Perseid Meteoroid Stream." Earth, Moon, and Planets 117, no. 2-3 (February 8, 2016): 93–100. http://dx.doi.org/10.1007/s11038-016-9483-4.

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

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Drolshagen, E., T. Ott, D. Koschny, G. Drolshagen, J. Vaubaillon, F. Colas, B. Zanda, 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 Network (FRIPON) are studied. The luminous efficiencies of the events are computed using an ablation-based model. The relations of τ as a function of the pre-atmospheric meteoroid velocity, ve, and mass, Me, are studied. Various aspects that could render the method less valid, cause inaccuracies, or bias the results are investigated. On this basis, the best suitable meteors were selected for luminous efficiency computations. Results. The presented analysis shows the limits of the used method. The most influential characteristics that are necessary for reliable results for the τ computation were identified. We study the dependence of τ on the assumed meteoroid’s density, ρ, and include improved ρ-values for objects with identified meteoroid stream association. Based on the discovered individual biases and constraints we create a pre-debiased subset of 54 well-recorded events with a relative velocity change >80%, a final height <70 km, and a Knudsen number Kn < 0.01; this last value indicates that the events were observed in the continuum-flow regime. We find τ-values in the range between 0.012% and 1.1% for this pre-debiased subset and relations of τ to ve and Me of: τ=7.33⋅ve−1.10 and τ=0.28⋅Me−0.33. Conclusions. The derived luminous efficiency of meteoroids depends on the assumed material density. Our results indicate that the applied debiasing method improves the analysis of τ from decelerated meteoroids. The underlying method is only valid for meteors in the continuum-flow regime. These events tend to have low end heights, large masses, and high deceleration.

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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 роям, найденных нами. Выявлена астероидная ассоциация (три астероида), возможно, связанная с метеоритом Гланербруг и его болидным роем η-Ursa-Majorids. Это приводит к возможности существования в астероидно-метеороидной системе малых тел. Значения величины константы Тиссерана, вычисленные для всех пяти объектов данной системы, показывают, что все эти объекты, включая болидный рой с метеоритом Гланербруг, не имеют связи ни с кометами, ни с кометоидами, но могут иметь связь с астероидами. Все пять объектов имеют очень похожие значения константы Тиссерана. Мы также можем сделать предположение, что в прошлом все эти тела имели одну орбиту. The bright fireball of -12. m 5, that produced the Glanerbrug meteorite, was observed over Netherlands on April 7, 1990, at 18 h 32 m 38 s UT. The first orbit determinations were very approximate and naturally required revision. M. Langbroek, having analyzed basic data, obtained new revised orbital elements of the Glanerbrug meteorite. We apply this system of elements in our research. Having analyzed catalogues of fireball and meteoroid streams, we found fireball stream of the η-Ursa-Majorids. Its orbital elements are consistent with those of the Glanerbrug meteorite. The η-Ursa-Majorids fireball stream belongs to the 14 meteorite-producing fireball streams, found by us. The orbital elements of those streams are presented. We revealed asteroid association (three asteroids) possibly related with Glanerbrug meteorite and its fireball stream of η-Ursa-Majorids. This leads to a possible existence of an asteroid-meteoroid system of minor bodies. Value of Tisserand’s constant calculated for all five objects of this system reveals that all these objects including the fireball stream and Glanerbrug meteorite are not related with comets or cometoids but they may be related with asteroids. All five objects have very similar values of Tisserand’s constant. On the base of this Tisserand’s criterion does not contradict to the assumption that in the past all these bodies could have shared the same orbit.

Journal articles on the topic 'Meteoroid stream'

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