scholarly journals Dynamical Aspects of the Taurid Meteor Complex

1992 ◽  
Vol 152 ◽  
pp. 315-324 ◽  
Author(s):  
J. Štohl ◽  
V. Porubčan
Keyword(s):  
Data Center ◽  
Dynamical Evolution ◽  
Similarity Criteria ◽  
Orbital Elements ◽  
Meteor Streams ◽  
Photographic Meteor Orbits ◽  
Meteor Data

Unusually long activity of the Taurid meteor complex, extending over 3-5 months according to new estimations based on various orbital similarity criteria, has been evoking controversies about the possible origin and dynamical evolution of this unique complex of meteor streams. It even casts doubts on the reality of the extension of the complex. In the present paper orbital elements and the extension of the Taurid meteor complex are re-examined on the bases of the most precise photographic meteor orbits available from the IAU Meteor Data Center in Lund. The results are evaluated and discussed from the viewpoint of various proposals on the origin and dynamical evolution of the complex.

Statistical results on discovered near-Earth asteroids

1999 ◽  
Vol 173 ◽  
pp. 81-86
Author(s):  
S. Berinde
Keyword(s):  
Dynamical Evolution ◽  
Minor Planet ◽  
Orbital Elements ◽  
The Earth ◽  
Near Earth Asteroids ◽  
Statistical Results

AbstractThe first part of this paper gives a recent overview (until July 1st, 1998) of the Near-Earth Asteroids (NEAs) database stored at Minor Planet Center. Some statistical interpretations point out strong observational biases in the population of discovered NEAs, due to the preferential discoveries, depending on the objects’ distances and sizes. It is known that many newly discovered NEAs have no accurately determinated orbits because of the lack of observations. Consequently, it is hard to speak about future encounters and collisions with the Earth in terms of mutual distances between bodies. Because the dynamical evolution of asteroids’ orbits is less sensitive to the improvement of their orbital elements, we introduced a new subclass of NEAs named Earth-encounter asteroids in order to describe more reliably the potentially dangerous bodies as impactors with the Earth. So, we pay attention at those asteroids having an encounter between their orbits and that of the Earth within 100 years, trying to classify these encounters.

scholarly journals The orbital evolution of meteor streams at the 2/1 resonance with Jupiter

1985 ◽  
Vol 83 ◽  
pp. 179-180
Author(s):  
Cl. Froeschlé
Keyword(s):  
Major Axis ◽  
Orbital Evolution ◽  
The Sun ◽  
Orbital Elements ◽  
Meteor Stream ◽  
Semi Major Axis ◽  
Meteor Streams ◽  
Gravitational Forces ◽  
Resonant Effect

We investigated the orbital evolution of Quadrantid-like meteor streams situated in the vicinity of the 2/1 resonance with Jupiter. For the starting orbital elements we took the values of the orbital elements of the Quadrantid meteor stream except for the semi-major axis which was varied between a = 3.22 and a = 3.34 AU. We considered these meteor streams as a ring and we investigated the resonant effect on the dispersion of this ring over a period of 13 000 years. Only gravitational forces due to the Sun and due to Jupiter were taken into account.

scholarly journals Do comet groups exist?

1985 ◽  
Vol 83 ◽  
pp. 353-363
Author(s):  
B.A. Lindblad
Keyword(s):  
Computer Program ◽  
Confidence Level ◽  
Computer Search ◽  
Orbital Elements ◽  
Similarity Parameter ◽  
The Real ◽  
Meteor Streams ◽  
Long Period ◽  
Random Samples ◽  
Period Comet

AbstractThe phenomena of comet groups, i.e. sets of comets that exhibit similarity in their orbital elements, is investigated. A computer program based on the D-criterion of orbital similarity is used to search for comet pairs and groups. The reality of the groups is tested by making computer searches in random samples of comet orbits.The data base for the study is 599 long-period comet orbits. The degree of orbital similarity within a comet group was first assumed to be identical to that encountered in meteor streams. The computer search at this level produced five comet pairs plus two groups with four and seven members, respectively. The latter two represented the eleven known members of the Kreutz group of sun-grazing comets. A comparison with searches in random samples showed that the two Kreutz groups were significant. There is a probability of 0.2 that the five comet pairs found in the real sample could be accidental formations.In a second study the orbital similarity parameter Ds was varied and the number of comet groups found in the real and synthetic comet populations was compared at each level of Ds. Apart from the Kreutz group of comets, the number of groups detected in the real comet sample was for all levels of orbital similarity only slightly higher than the average found in the random samples. At the 2σ confidence level we conclude that comet groups exhibit similarity in their orbital elements, that is no greater than might be expected by chance.

scholarly journals The Iau Meteor Data Center in Lund

1991 ◽  
Vol 126 ◽  
pp. 311-314 ◽  
Author(s):  
B.A. Lindblad
Keyword(s):  
Data Center ◽  
Meteor Data

AbstractThe purpose of the IAU Meteor Data Center in Lund is to archive, document and disseminate information on meteoroid orbits. At present some 6 000 photographic double-station orbits and 60 000 radio determined orbits are archived.

scholarly journals IAU Meteor Data Center—the shower database: A status report

2017 ◽  
Vol 143 ◽  
pp. 3-6 ◽  
Author(s):  
Tadeusz Jan Jopek ◽  
Zuzana Kaňuchová
Keyword(s):  
Data Center ◽  
Status Report ◽  
Meteor Data

scholarly journals The past orbit of comet Halley and its meteor stream

1985 ◽  
Vol 83 ◽  
pp. 399-403
Author(s):  
A. Hajduk
Keyword(s):  
Structural Features ◽  
Orbital Elements ◽  
Meteor Stream ◽  
Meteor Streams ◽  
The Past ◽  
Maximum Lifetime ◽  
Check Points ◽  
History Of ◽  
Comet Halley ◽  
Comet Orbit

AbstractThe present paper studies the structural features of the meteor streams associated with Comet Halley deduced from the observations of its meteor showers, as check points of orbital elements in a deeper history of the comet orbit. Libration of the argument of perihelion of the comet and the corresponding displacement of the nodes, as recognized in the distribution of condensations within the stream, allows to estimate the maximum lifetime of the comet in the inner Solar System at about 2 × 105 years.

scholarly journals Dynamical Evolution of Interplanetary Dust due to Gravitational Scattering by Jupiter and the Inner Planets

1996 ◽  
Vol 150 ◽  
pp. 43-46 ◽  
Author(s):  
Nikolai N. Gor'kavyi ◽  
Leonid M. Ozernoy ◽  
John C. Mather
Keyword(s):  
Continuity Equation ◽  
Dynamical Evolution ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Coordinate Space ◽  
Gradual Change ◽  
Orbital Elements ◽  
Interplanetary Dust Particles ◽  
Zodiacal Cloud ◽  
Gravitational Scattering

AbstractWe introduce the continuity equation written in the coordinate space of the orbital elements (e.g. large semi-axis a vs. eccentricity e, etc.) to explore the density evolution of the zodiacal cloud. Emphasis is on those terms of the continuity equation which describe ‘jumps’ of particles in the (a, e)-space due to gravitational scattering of the interplanetary dust particles by planets, which represents one of the leading factors in the dynamical evolution of the zodiacal cloud. In the remainder (div-terms of the continuity equation), one can incorporate the known analytical expressions for the rates of gradual change of orbital elements due to the Poynting-Robertson and solar wind drags (Liou et al. 1995).

scholarly journals Long-period comet C/1963 A1 (Ikeya), the probable parent body of π-Hydrids, δ-Corvids, November α-Sextantids, and ϑ-Leonids

2019 ◽  
Vol 631 ◽  
pp. A112 ◽  
Author(s):  
L. Neslušan ◽  
M. Hajduková
Keyword(s):  
Dynamical Evolution ◽  
Parent Body ◽  
Video Data ◽  
Surveillance Video ◽  
Evolutionary Time ◽  
Meteoroid Stream ◽  
Long Period ◽  
The Mean ◽  
Meteor Data ◽  
Period Comet

Aims. We study the meteoroid stream of the long-period comet C/1963 A1 (Ikeya) to predict the meteor showers originating in this comet. We also aim to identify the predicted showers with their real counterparts. Methods. We modeled 23 parts of a theoretical meteoroid stream of the parent comet considered. Each of our models is characterized by a single value of the evolutionary time and a single value of the strength of the Poynting–Robertson effect. The evolutionary time is defined as the time before the present when the stream is modeled and when we start to follow its dynamical evolution. This period ranges from 10 000 to 80 000 yr. In each model, we considered a stream consisting of 10 000 test particles that dynamically evolve, and their dynamics is followed via a numerical integration up to the present. At the end of the integration, we analyzed the mean orbital characteristics of particles in the orbits approaching Earth’s orbit, which thus enabled us to predict a shower related to the parent comet. We attempted to identify each predicted shower with a shower recorded in the International Astronomical Union Meteor Data Center list of all showers. In addition, we tried to separate, often successfully, a real counterpart of each predicted shower from the databases of real meteors. Results. Many modeled parts of the stream of comet C/1963 A1 are identified with the corresponding real showers in three video-meteor databases. No real counterpart is found in the IAU MDC photographic or radio-meteor data. Specifically, we predict five showers related to C/1963 A1. Two predicted showers are identified with π-Hydrids #101 and δ-Corvids #729. The third predicted shower is only vaguely similar to November α-Sextantids #483, when its mean orbit is compared with the mean orbit of the November α-Sextantids in the IAU MDC list of all showers. However, the prediction is very consistent with the corresponding showers newly separated from three video databases. Another predicted shower has no counterpart in the IAU MDC list, but there is a good match of the prediction and a shower that we separated from the Cameras for Allsky Meteor Surveillance video data. We name this new shower ϑ-Leonids. The last of the predicted showers should be relatively low in number and, hence, no real counterparts were either found in the IAU MDC list or separated from any considered database.

The structure of meteor streams associated with Comet Halley: Eta Aquarids and Orionids

1974 ◽  
Vol 22 ◽  
pp. 309-311
Author(s):  
Anton Hajduk
Keyword(s):  
Density Distribution ◽  
Meteor Shower ◽  
Point Of View ◽  
Orbital Elements ◽  
Statistical Point ◽  
Radar Observations ◽  
Meteor Streams ◽  
Stream Structure ◽  
Comet Halley ◽  
Radar Meteor

The association of Comet Halley with the Orionid and Eta Aquarid meteor streams is not commonly accepted at present. Southworth (1961) has determined the differences in the orbital elements of the Orionid stream and Comet Halley on the basis of 19 photographic meteors and found them to be rather large.Extensive observational material obtained since the beginning of this century, including a homogeneous series of the radar observations, carried out at the Springhill Meteor Observatory during the periods of the Orionid meteor shower activity in 1957–1967 has been used by the author (Hajduk 1971) to study the stream structure and its association with Comet Halley from a statistical point of view.The present analysis is an extension of the paper mentioned, based mainly on the radar observations of the Eta Aquarid meteor shower carried out at the Springhill Observatory during the period 1958–67. The total number of 240,000 radar meteor echoes observed in 670 hours between May 1 and May 10 during each of the years previously cited was used in this investigation. The observed variations in the hourly rates of echoes of different duration enable us to study the density distribution and size distribution of meteoric particles along and across the stream.

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