Dynamics and Spatial Shape of Short-Period Meteoroid Streams

Бабаджанов, П. Б.; Obrubov, Yu. V.

doi:10.1007/978-94-009-0977-9_44

Cited by 16 publications

(6 citation statements)

References 4 publications

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“…This is close to the value calculated by Babadzhanov and Obrubov (1980) based on P-R drag and secular perturbations for a particle density of 1 g/cm . Olsson-Steel (1987b) In their more recent study, Babadzhanov and Obrubov (1989) state that secular perturbations are constrained by two relations:…”

Section: Closest Approach To Jupitermentioning

confidence: 99%

“…where C 1 and C 2 are constants. The first is a modified version of the Tisserand criterion; the second is stated to be an integral of the motion developed by authors referenced by Babadzhanov and Obrubov (1989).…”

Section: Closest Approach To Jupitermentioning

confidence: 99%

“…Mcintosh (1990) shows that two comets, P/Machholz 1986 VIII and 1491-1, and several meteor streams, all form a complex associated with the Quadrantids. Babadzhanov and Obrubov (1989) note that, for Quadrantid-like orbits, their equations (see Section 3.2.2.2) have eight possible solutions. A number of major showers correspond to the solutions: the daytime Arietids; the northern and southern 6 Aquarids; and the Ursids.…”

Section: Sextantidsmentioning

confidence: 99%

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Debris from Comets: The Evolution of Meteor Streams

McIntosh¹

1989

International Astronomical Union Colloquium

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The evolution of meteor streams is controlled basically by: (a) the initial velocities with which the particles were ejected from the parent body; (b) gravitational perturbations by the planets; (c) radiation forces; and (d) collisions. This review focuses mainly on recent numerical modelling dealing with (b) and (a).Ejection velocities spread the particles around the orbit, closing the ring in a few tens of revolutions. The greater ejection velocities of smaller particles cause more rapid dispersion both around the orbit and in the cross section.A determination of the effects of gravitational perturbations must take into account the distributed properties of the stream. The stream’s evolution is dependent on the short-term impulse nature of planetary perturbations, as well as on long-term secular effects. The combined effects produce complex stream cross-sections as in the ribbon-like form of the Halley stream (Orionid and η Aquarid showers) or as in the changes in the annual position of peak shower activity shown by the Quadrantids. Perturbations may cause the orbit of a parent body to sweep rapidly across the orbit of the Earth. But the associated particle stream may not be lost as a meteor shower because it tends to become dispersed in a manner that ensures a continuing supply of particles in Earth-crossing orbits. The nodes of the observed meteoroid orbits may show very little motion compared with the rapid motion of the nodes of the orbit of the parent object.Radiation effects contribute to size separation of particles. Very small particles are blown out of the stream or spiral in toward the sun because of Poynting–Robertson drag. Older meteor streams usually show a predominance of large particles.

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Section: Closest Approach To Jupitermentioning

confidence: 99%

Section: Closest Approach To Jupitermentioning

confidence: 99%

Section: Sextantidsmentioning

confidence: 99%

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Debris from Comets: The Evolution of Meteor Streams

McIntosh¹

1989

International Astronomical Union Colloquium

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“…On the other hand, the broader background stream implies larger ages of perhaps ∼3500 years or more (Ohtsuka et al 1995;Wiegert & Brown 2005;Kanuchová & Nesluśan 2007;. Comet 96P/Machholz is also suspected to form part of the "Quadrantid complex," possibly releasing meteoroids between 2000-5000 years ago (McIntosh 1990;Babadzhanov & Obrubov 1991;Gonczi et al 1992;Jones & Jones 1993;Wiegert & Brown 2005). Comet 96P/Machholz currently has a small perihelion orbit (a = 3.034 AU, e = 0.959, i = 58°.312 and q = 0.124 AU from NASA/JPL HORIZON) substantially different from that of 2003 EH1.…”

Section: Introductionmentioning

confidence: 99%

Physical Observations of (196256) 2003 Eh1, Presumed Parent of the Quadrantid Meteoroid Stream

Kasuga

Jewitt

2015

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The near-Earth asteroid (196256) 2003 EH1 has been suggested to have a dynamical association with the Quadrantid meteoroid stream. We present photometric observations taken to investigate the physical character of this body and to explore its possible relation to the stream. We find no evidence for ongoing mass loss. A model fitted to the point-like surface brightness profile at 2.1 AU limits the fractional contribution to the integrated brightness by the near-nucleus coma to 2.5%. Assuming an albedo equal to those typical of cometary nuclei (p R = 0.04), we find that the effective nucleus radius is r e = 2.0 ± 0.2 km. Time-resolved R-band photometry can be fitted by a two-peaked light curve having a rotational period of 12.650 ± 0.033 hr. The range of the light curve, Δm R = 0.44 ± 0.01 mag, is indicative of an elongated shape having an axis ratio of ∼1.5 projected into the plane of the sky. The asteroid shows colors slightly redder than the Sun, being comparable with those of C-type asteroids. The limit to the mass loss rate set by the absence of the resolved coma is 2.5 × 10 −2 kg s −1 , corresponding to an upper limit on the fraction of the surface that could be sublimating water ice f A  10 −4 . Even if sustained over the 200-500 year dynamical age of the Quadrantid stream, the total mass loss from 2003 EH1 would be too small to supply the reported stream mass (10 13 kg), implying either that the stream has another parent or that mass loss from 2003 EH1 is episodic.

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“…However sometimes, the importance of the mean parameters is quite high. In Babadzhanov & Obrubov (1980, 1982), Williams, Murray & Hughes (1979), Murray, Hughes & Williams (1980) and Fox, Williams & Hughes (1982), the mean orbital elements have been used to investigate the long‐term evolution of meteor streams. Also, the mean orbit is compared with the orbit of the possible parent of the stream, as in Fox, Williams & Hughes (1984) and Lindblad (1990).…”

Section: Introductionmentioning

confidence: 99%

Calculation of the mean orbit of a meteoroid stream

Jopek¹,

Rudawska²,

Prętka-Ziomek³

2006

Monthly Notices of the Royal Astronomical Society

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The traditional approach used for averaging the parameters of a meteoroid gives results that are biased by several conceptual defects: among others things, the mean orbital elements do not satisfy the laws of celestial mechanics. The Voloshchuk & Kashcheev method in the domain of geocentric parameters removes all of these defects except one: the epoch corresponding to the mean geocentric values, which is critical for the calculation of the mean heliocentric orbital elements from the mean geocentric radiant coordinates and velocity. We propose a new approach: our solution gives the mean orbital elements and the geocentric radiant parameters of the meteor stream, free from all conceptual faults. Instead of the Keplerian orbital elements, we average the heliocentric vectorial elements, and the solution is obtained by the least‐squares method completed by placing two constraints on the mean vectorial elements. One may calculate the corresponding geocentric parameters using the theoretical radiant approach. However, to obtain mutually numerically consistent helioparameters and geoparameters, all members of the stream should be pre‐integrated into a common epoch of time. Our approach, due to simultaneous averaging of seven variables, is limited to the streams of seven or more members only. We give the results of the numerical example, which shows that the mean values obtained by our approach differ slightly from those obtained by the traditional averaging. However, for some streams and for some particular orbital elements, the differences can exceeds 2 au in the semimajor axes or in the angular orbital elements.

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Dynamics and Spatial Shape of Short-Period Meteoroid Streams

Cited by 16 publications

References 4 publications

Debris from Comets: The Evolution of Meteor Streams

Debris from Comets: The Evolution of Meteor Streams

Physical Observations of (196256) 2003 Eh1, Presumed Parent of the Quadrantid Meteoroid Stream

Calculation of the mean orbit of a meteoroid stream

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