Sporadic meteor radiant distributions: orbital survey results

Jones, J.; Brown, Peter

doi:10.1093/mnras/265.3.524

Cited by 120 publications

(156 citation statements)

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“…(1) particles associated with streams concentrated in interplanetary space (e.g., Jenniskens 2006Jenniskens , 2008aJenniskens , 2008bBrown et al 2008Brown et al , 2010, thus impacting the Earth at discrete and welldefined time windows lasting typically days, and (2) particles belonging to a sporadic background (e.g., Jones & Brown 1993) for an excellent data compilation and a historic perspective). It is believed that the sporadic component is actually composed of particles which originated in streams, which over the course of time have dispersed and become interwoven so much with other sources that they cannot be individually distinguished anymore.…”

Section: Introductionmentioning

confidence: 99%

Dynamical Model for the Toroidal Sporadic Meteors

Pokorný

Vokrouhlický

Nesvorný

et al. 2014

ApJ

115

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More than a decade of radar operations by the Canadian Meteor Orbit Radar have allowed both young and moderately old streams to be distinguished from the dispersed sporadic background component. The latter has been categorized according to broad radiant regions visible to Earth-based observers into three broad classes: the helion and anti-helion source, the north and south apex sources, and the north and south toroidal sources (and a related arc structure). The first two are populated mainly by dust released from Jupiter-family comets and new comets. Proper modeling of the toroidal sources has not to date been accomplished. Here, we develop a steady-state model for the toroidal source of the sporadic meteoroid complex, compare our model with the available radar measurements, and investigate a contribution of dust particles from our model to the whole population of sporadic meteoroids. We find that the long-term stable part of the toroidal particles is mainly fed by dust released by Halley type (long period) comets (HTCs). Our synthetic model reproduces most of the observed features of the toroidal particles, including the most troublesome low-eccentricity component, which is due to a combination of two effects: particles' ability to decouple from Jupiter and circularize by the Poynting-Robertson effect, and large collision probability for orbits similar to that of the Earth. Our calibrated model also allows us to estimate the total mass of the HTC-released dust in space and check the flux necessary to maintain the cloud in a steady state.

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Section: Introductionmentioning

confidence: 99%

Dynamical Model for the Toroidal Sporadic Meteors

Pokorný

Vokrouhlický

Nesvorný

et al. 2014

ApJ

115

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show abstract

“…The first three sources associated with the ecliptic plane were discovered by Hawkins (1957). According to the latest papers (Jones & Brown 1993;Brown & Jones 1995;Poole 1997) we now identify six such sources. They are antihelion, helion, northern and southern toroidal centers and also the northern and southern apex.…”

Section: Distribution Of Sporadic Meteors Over the Celestial Spherementioning

confidence: 92%

“…These radiants in July at Polish geographical coordinates are always either very close to the Sun or below the horizon. The remaining three sources were included into the database and their properties taken from Jones & Brown (1993) are summarized in Table 4. According to the work of Jones & Brown (1993) and Poole (1997) all sources seem to have similar activity.…”

Section: Distribution Of Sporadic Meteors Over the Celestial Spherementioning

confidence: 99%

“…The remaining three sources were included into the database and their properties taken from Jones & Brown (1993) are summarized in Table 4. According to the work of Jones & Brown (1993) and Poole (1997) all sources seem to have similar activity. Thus we assumed that the number of the sporadic events radiating from each center is proportional only to the sine function of the center altitude.…”

Section: Distribution Of Sporadic Meteors Over the Celestial Spherementioning

confidence: 99%

“…Thus for each sporadic source we used the entry velocity distributions given by Jones & Brown (1993) (see their Figs. 7-9).…”

Section: Distribution Of Sporadic Meteors Over the Celestial Spherementioning

confidence: 99%

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An artificial meteor database as a test for the presence of weak showers

Olech¹,

Wiśniewski²

2002

A&A

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Abstract.We have constructed an artificial meteor database resembling in all details the real sample collected by the observers of the Comets and Meteors Workshop in the years 1996-1999. The artificial database includes the sporadic meteors and also events from the following showers: Perseids, Aquarid complex, α-Capricornids, July Pegasids and Sagittarids. This database was searched for the presence of the radiants of two weak showers: α-Cygnids and Delphinids. The lack of these radiants in the artificial database and their existence in the real observations suggests that α-Cygnids and Delphinids are real showers and their radiants could not be formed as an effect of intersections of back prolongated paths of meteors belonging to other showers.

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Interferometric meteor head echo observations using the Southern Argentina Agile Meteor Radar

et al. 2014

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A radar meteor echo is the radar scattering signature from the free electrons generated by the entry of extraterrestrial particles into the atmosphere. Three categories of scattering mechanisms exist: specular, nonspecular trails, and head echoes. Generally, there are two types of radars utilized to detect meteors. Traditional VHF all‐sky meteor radars primarily detect the specular trails, while high‐power, large‐aperture (HPLA) radars efficiently detect meteor head echoes and, in some cases, nonspecular trails. The fact that head echo measurements can be performed only with HPLA radars limits these studies in several ways. HPLA radars are sensitive instruments constraining the studies to the lower masses, and these observations cannot be performed continuously because they take place at national observatories with limited allocated observing time. These drawbacks can be addressed by developing head echo observing techniques with modified all‐sky meteor radars. Such systems would also permit simultaneous detection of all different scattering mechanisms using the same instrument, rather than requiring assorted different classes of radars, which can help clarify observed differences between the different methodologies. In this study, we demonstrate that such concurrent observations are now possible, enabled by the enhanced design of the Southern Argentina Agile Meteor Radar (SAAMER). The results presented here are derived from observations performed over a period of 12 days in August 2011 and include meteoroid dynamical parameter distributions, radiants, and estimated masses. Overall, the SAAMER's head echo detections appear to be produced by larger particles than those which have been studied thus far using this technique.

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Sporadic meteor radiant distributions: orbital survey results

Cited by 120 publications

References 0 publications

Dynamical Model for the Toroidal Sporadic Meteors

Dynamical Model for the Toroidal Sporadic Meteors

An artificial meteor database as a test for the presence of weak showers

Interferometric meteor head echo observations using the Southern Argentina Agile Meteor Radar

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