High resolution radiant distribution and orbits of sporadic radar meteoroids

Campbell-Brown, M.

doi:10.1016/j.icarus.2008.02.022

Cited by 91 publications

(113 citation statements)

References 22 publications

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“…They may thus be measuring only recent contributions to the stream, while we are also sampling older trails, the orbits of which may have altered over time. CMOR measurements of the psi Cassiopeids (Brown et al 2008) give a = 2.2 AU (slightly higher than the peak in the distribution here, around 1 AU), e = 0.57, in the middle of our broad distribution, i = 83.1°( within the uncertainty of our distribution) and v g = 44.2 km s -1 , very close to our peak. Similar measurements of the alpha Lacertids have a = 1.1 AU (in good agreement), e = 0.1 (close to our peak, though we show a long tail to higher eccentricities), i = 81.8° (good agreement) and v g = 39.0 km s -1 , slightly lower than our peak.…”

Section: Orbital Distributions Of the Radiantssupporting

confidence: 79%

“…Orbital elements of Bootid/Corona Borealid complex showers, as measured with CMOR data (Brown et al 2008 …”

Section: Discussionmentioning

confidence: 99%

“…The south toroidal source was confirmed in a study of meteor orbit surveys by Jones and Brown (1993), who found it in data from the Adelaide meteor radar; they also characterized the orbital distribution of the north toroidal source, for which more data existed. Campbell-Brown (2008) determined from a study of the Canadian Meteor Orbit Radar (CMOR) data that 18% of observed sporadic meteors were north toroidal; the fraction dropped to 10% when corrected for observing biases, since high latitude radiants are better observed from the northern hemisphere than radiants on the ecliptic. Brown and Jones (1995) determined from Springhill and Christchurch radar data that approximately 6% of sporadic meteors originated in the north toroidal source, and 6% in the south toroidal source, a slightly lower fraction than the most recent results.…”

Section: Introductionmentioning

confidence: 99%

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Seasonal variations in the north toroidal sporadic meteor source

Campbell-Brown

Wiegert

2009

Meteorit & Planetary Scien

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Abstract-Determining the origins of the sporadic meteoroid sources helps determine their current properties. We have analyzed four years of orbital radar data, looking at how the rates, radiants, and orbits of meteoroids in the north toroidal sporadic source change throughout the year. Twelve broad radiant concentrations, separated in either time or radiant location, are identified. Six are broad distributions associated with more focused shower activity, and six are not associated with major showers. Four of the six concentrations not associated with showers have been named Toroidal, Toroidal A, Toroidal B, and Toroidal C, because of their constant location at the north toroidal centre. The other two, which appear close to the north toroidal source and drift toward the helion and antihelion sources respectively, have been named the Helion Arc and the Antihelion Arc. The twelve radiant concentrations generally last for more than ten degrees solar longitude, and those which may have a single parent are likely composed of orbitally evolved material.

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Section: Orbital Distributions Of the Radiantssupporting

confidence: 79%

“…Orbital elements of Bootid/Corona Borealid complex showers, as measured with CMOR data (Brown et al 2008 …”

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Seasonal variations in the north toroidal sporadic meteor source

Campbell-Brown

Wiegert

2009

Meteorit & Planetary Scien

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“…A more detailed understanding of the zodiacal dust cloud at 1 AU, including both its ultimate origin(s) and its contribution to the cosmic dust flux to the Earth, has come from a recent series of dynamical models (e.g., Wiegert et al 2009;Nesvorný et al 2010Nesvorný et al , 2011aPokorny et al 2014). By comparison with remote observations from the Infrared Astronomical Satellite (IRAS), the Cosmic Background Explorer (COBE), and the Spitzer Space Telescope Kelsall et al 1998), and observations from terrestrial-based meteor surveys including the Canadian Meteor Orbit Radar (CMOR) (Campbell-Brown 2008), the Advanced Meteor Orbit Radar (AMOR) Baggaley 2004, 2005), and High Performance Large Aperture (HPLA) radars (e.g., Janches and Chau 2005;Janches and ReVelle 2005;Janches et al 2006Janches et al , 2014, the Nesvorný et al (2010Nesvorný et al ( , 2011a dynamical models have concluded that a majority (∼85-95%) of the zodiacal dust cloud near 1 AU originates from JFCs (e.g., Levison and Duncan 1997). AST, HTC, and OCC dust sources contribute the remaining 5-15%.…”

Section: Astronomical Dust Modelsmentioning

confidence: 99%

Impacts of Cosmic Dust on Planetary Atmospheres and Surfaces

et al. 2017

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Recent advances in interplanetary dust modelling provide much improved estimates of the fluxes of cosmic dust particles into planetary (and lunar) atmospheres throughout the solar system. Combining the dust particle size and velocity distributions with new chemical ablation models enables the injection rates of individual elements to be predicted as a function of location and time. This information is essential for understanding a variety of atmospheric impacts, including: the formation of layers of metal atoms and ions; meteoric smoke particles and ice cloud nucleation; perturbations to atmospheric gas-phase chemistry; and the effects of the surface deposition of micrometeorites and cosmic spherules. There is discussion of impacts on all the planets, as well as on Pluto, Triton and Titan.

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“…Eventually the goal is to produce a map in Sun-centered ecliptical coordinates of the distribution of meteor radiants and to compare it to similar ones obtained by optical or radar means (e.g. [4]). …”

Section: The Brams Networkmentioning

confidence: 99%

BRAMS: The Belgian RAdio Meteor Stations

Lamy

Ranvier

Keyser

et al. 2011

2011 XXXth URSI General Assembly and Scientific Symposium

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In the last months, the Belgian Institute for Space Aeronomy has been developing a Belgian network for observing radio meteors using forward scattering technique. This network is called BRAMS for Belgian RAdio Meteor Stations. Two beacons emitting a circularly polarized pure sine wave toward the zenith act as the transmitters at frequencies of 49.97 and 49.99 MHz. The first one located in Dourbes (Southern Belgium) emits a constant power of 150 Watts while the one located in Ieper (Western Belgium) emits a constant power of 50 Watts. The receiving network consists of about 20 stations hosted mainly by radio amateurs. Two stations have crossed-Yagi antennas measuring horizontal and vertical polarizations of the waves reflected off meteor trails. This will enable a detailed analysis of the meteor power profiles from which physical parameters of the meteoroids can be obtained. An interferometer consisting of 5 Yagi-antennas will be installed at the site of Humain in order to determine the angular detection of one reflection point, allowing us to determine meteoroid trajectories. We describe this new meteor observing facility and present the goals we expect to achieve with the network.

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High resolution radiant distribution and orbits of sporadic radar meteoroids

Cited by 91 publications

References 22 publications

Seasonal variations in the north toroidal sporadic meteor source

Seasonal variations in the north toroidal sporadic meteor source

Impacts of Cosmic Dust on Planetary Atmospheres and Surfaces

BRAMS: The Belgian RAdio Meteor Stations

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