Meteoroid-stream complex originating from comet 2P/Encke

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.

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When Might 2P/Encke Have Produced Meteor Storms?

International Astronomical Union Colloquium ◽

10.1017/s0252921100501407 ◽

1996 ◽

Vol 150 ◽

pp. 125-128

Author(s):

D.I. Steel ◽

D.J. Asher

Keyword(s):

Dynamical Evolution ◽

The Past ◽

Gravitational Forces ◽

The Earth ◽

Short Period Comet ◽

Short Period ◽

Meteor Storm ◽

Pass Through ◽

Better Than ◽

Period Comet

Abstract2P/Encke is the only Earth-crossing short-period comet to have a meteoroid/dust trail identified in the data collected by IRAS Such trails have been suggested by Kresák to be the cause of meteor storms, these occurring when the comet/trail node is near 1 AU and the Earth happens to pass through the trail. Here we present the results of integrations of variational orbits of 2P/Encke (the differences in the assumed initial semi-major axes representing the order of changes that could occur due to non-gravitational effects) from which we derive indications of when this comet may have produced meteor storms in the past. Pairs of sets of storms are expected about 300 yr apart, but the effects of chaotic dynamical evolution (and our ignorance of 2P/Encke's non-gravitational forces for any but the last two centuries) mean that we cannot define the epochs in which these may have occurred to better than 200 BC to AD 500 for the last pair, and 3600 to 1800 BC for the previous pair. Looking forwards in time, no meteor storm due to 2P/Encke will occur for at least 600 yr.

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Modeling of the meteoroid stream of comet C/1975 T2 and λ-Ursae Majorids

Astronomy and Astrophysics ◽

10.1051/0004-6361/201935630 ◽

2019 ◽

Vol 627 ◽

pp. A73 ◽

Cited By ~ 3

Author(s):

M. Hajduková ◽

L. Neslušan

Keyword(s):

Dynamical Evolution ◽

Parent Body ◽

Meteor Shower ◽

Evolutionary Time ◽

Meteoroid Stream ◽

Test Particles ◽

International Astronomical ◽

The Mean ◽

Almost All ◽

Meteor Data

Aims. We study the meteoroid stream of the long-period comet C/1975 T2 (Suzuki-Saigusa-Mori). This comet was suggested as the parent body of the established λ-Ursae Majorid meteor shower, No. 524. Methods. We modeled 32 parts of a theoretical meteoroid stream of the parent comet considered. Each of our models is characterized with a single value of the evolutionary time and a single value of the strength of Poynting-Robertson effect. The evolutionary time ranges from 10 000 to 80 000 yr. It is the period during which the evolution of the stream part is followed. In each model, the dynamical evolution of 10 000 test particles was then followed, via a numerical integration, from the time of the modeling up to the present. At the end of the integration, we analyzed the mean orbital characteristics of particles in the orbits that approach the Earth’s orbit, which thus enabled us to predict a shower related to the parent comet. The predicted shower was subsequently compared with its observed counterparts. We separated the latter from the databases of real meteors. As well, we attempted to identify the predicted shower to a shower recorded in the International Astronomical Union Meteor Data Center (IAU MDC) list of all showers. Results. Almost all modeled parts of the stream of comet C/1975 T2 are identified with the corresponding real shower in three video-meteor databases. No real counterpart is found in the IAU MDC photographic or radio-meteor data. In the IAU MDC list of showers and in our current study, this shower is identified with the established λ-Ursae Majorid shower, No. 524. Hence, our modeling confirms the results of previous authors. At the same time we exclude an existence of other meteor shower associated with C/1975 T2.

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Meteor showers of comet C/1964 N1 (Ikeya)

Astronomy and Astrophysics ◽

10.1051/0004-6361/201832829 ◽

2018 ◽

Vol 616 ◽

pp. A162 ◽

Cited By ~ 3

Author(s):

L. Neslušan ◽

M. Hajduková

Keyword(s):

Dynamical Evolution ◽

Parent Body ◽

Meteor Shower ◽

Earth Orbit ◽

Test Particles ◽

Numerous Data ◽

The Mean ◽

The Relationship ◽

Period Comet

Aims. We intend to map the meteor complex of the long-period comet C/1964 N1 (Ikeya), which is a proposed parent body of the July ξ-Arietids, the meteor shower 533 in the IAU MDC list. Methods. For five perihelion passages of the parent comet in the past, we modeled the associated theoretical stream, its parts, consisting of 10 000 test particles each, and followed the dynamical evolution of these parts up to the present. We performed several simulations of the evolution, with various strengths of the Poynting–Robertson effect. At the end of each simulation, we analyzed the mean orbital characteristics of the particles that approached Earth orbit and thus created one or several showers. The showers were compared with their observed counterparts as separated from photographic and several video databases when the separation was successful. Results. The modeled stream of C/1964 N1 typically approaches Earth orbit in four filaments that correspond to four showers. Their radiant areas are close to the apex of Earth’s motion around the Sun. We confirm the generic relationship between the studied parent comet and the July ξ-Arietids. The comet also seems to be the parent of the ϵ-Geminids, shower 23, and we suspect a relationship between the comet and the ξ-Geminids, shower 718, although the relationship is rather uncertain. The real counterparts of three of the predicted showers were selected in the CAMS and SonotaCo databases. However, these real showers are diffuse, with relatively few members, and determination of their characteristics is therefore uncertain; the showers were separated into more than one single “modification”. Confirmation of their existence will have to await considerably more numerous data.

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

Astronomy and Astrophysics ◽

10.1051/0004-6361/201936407 ◽

2019 ◽

Vol 631 ◽

pp. A112 ◽

Cited By ~ 1

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.

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Covering of cometary nucleus by refractory crust and its evolution into asteroid-like body

International Astronomical Union Colloquium ◽

10.1017/s0252921100031675 ◽

1999 ◽

Vol 173 ◽

pp. 365-370

Author(s):

Kh.I. Ibadinov

Keyword(s):

Laboratory Experiments ◽

Cometary Nucleus ◽

Sublimation Rate ◽

Cometary Nuclei ◽

Short Period Comet ◽

Short Period ◽

Brightness Decrease ◽

Crust Thickness ◽

Ice Sublimation ◽

Period Comet

AbstractFrom the established dependence of the brightness decrease of a short-period comet dependence on the perihelion distance of its orbit it follows that part of the surface of these cometary nuclei gradually covers by a refractory crust. The results of cometary nucleus simulation show that at constant insolation energy the crust thickness is proportional to the square root of the insolation time and the ice sublimation rate is inversely proportional to the crust thickness. From laboratory experiments resulted the thermal regime, the gas productivity of the nucleus, covering of the nucleus by the crust, and the tempo of evolution of a short-period comet into the asteroid-like body studied.

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Some comments about observations and image processing of comet 29P/Schwassmann-Wachmann 1

International Astronomical Union Colloquium ◽

10.1017/s0252921100031493 ◽

1999 ◽

Vol 173 ◽

pp. 243-248

Author(s):

D. Kubáček ◽

A. Galád ◽

A. Pravda

Keyword(s):

Image Processing ◽

Large Scale ◽

Harvard College ◽

Oak Ridge ◽

Large Scale Structures ◽

Short Period Comet ◽

Short Period ◽

Scale Structures ◽

Harvard College Observatory ◽

Period Comet

AbstractUnusual short-period comet 29P/Schwassmann-Wachmann 1 inspired many observers to explain its unpredictable outbursts. In this paper large scale structures and features from the inner part of the coma in time periods around outbursts are studied. CCD images were taken at Whipple Observatory, Mt. Hopkins, in 1989 and at Astronomical Observatory, Modra, from 1995 to 1998. Photographic plates of the comet were taken at Harvard College Observatory, Oak Ridge, from 1974 to 1982. The latter were digitized at first to apply the same techniques of image processing for optimizing the visibility of features in the coma during outbursts. Outbursts and coma structures show various shapes.

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Physical Observations of the Short-Period Comet 1969 IV

Symposium - International Astronomical Union ◽

10.1017/s0074180900006215 ◽

1972 ◽

Vol 45 ◽

pp. 27-34

Author(s):

K. I. Churyumov ◽

S. I. Gerasimenko

Keyword(s):

Spectral Region ◽

Sunspot Area ◽

Radius Vector ◽

Short Period Comet ◽

Short Period ◽

Single Emission ◽

The Continuum ◽

Period Comet

The new short-period comet Churyumov-Gerasimenko, discovered by the authors on plates taken by the Kiev University cometary expedition to Alma-Ata in September 1969, was systematically photographed with fast telescopes at Byurakan and Alma-Ata until March 1970. Measurements were made of the photographic magnitude of the photometric nucleus, as well as of the photographic and photovisual integral magnitudes. The variations in nuclear magnitude were found to be well correlated with changes in the total sunspot area. The integral photometric parameters are Hy = 11.91±0m.54 and n=4.0±0.8 (in the photographic spectral region). Deviations of the tail axis from the prolonged radius vector were considerable. A spectrogram shows the continuum and emission of CN, C2 and C3 in the head, the continuum and a single emission (perhaps CO+) in the tail.

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The Kuiper Belt

Symposium - International Astronomical Union ◽

10.1017/s007418090004643x ◽

1994 ◽

Vol 160 ◽

pp. 31-44

Author(s):

Jane Luu

Keyword(s):

Solar System ◽

Kuiper Belt ◽

Cometary Nucleus ◽

Outer Solar System ◽

Short Period Comet ◽

Short Period ◽

Lower Limits ◽

Period Comet

The existence of a belt of comets in the outer solar system (the “Kuiper belt”) has been postulated for a variety of reasons, including the need for a source for the short-period comets. The existence of the belt seems supported by the discoveries of the trans-Neptunian objects 1992 QB1, 1993 FW, 1993 RO, 1993 RP, 1993 SB, and 1993 SC. If these objects are members of the Kuiper belt, crude lower limits on the belt population can be established from the discoveries. The Kuiper belt comets are likely to be primordial remnants of the disk from which the solar system accreted. According to the current theories of cometary nucleus evolution, these objects are expected to possess mantles (“irradiation mantles”) which are different from mantles of comets which have been heated to the point of sublimation (“rubble mantles”). Kuiper belt comets on their way to short-period comet orbits may exist among the Centaur objects.

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