Smoke and Dust Particles of Meteoric Origin in the Mesosphere and Stratosphere

Hunten, D. M.; Turco, R. P.; Toon, O. B.

doi:10.1175/1520-0469(1980)037<1342:sadpom>2.0.co;2

Cited by 570 publications

(575 citation statements)

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“…Hence, we have tried to assess the interpretation of our retrieved radii assuming that the actual MSP size distribution is of the same form as described by Hunten et al [1980]. Their results can be closely described by a distribution of the form…”

Section: Resultsmentioning

confidence: 99%

“…Radii show a near constant value of $0.8 nm, while number densities show a relatively steep gradient with only $10 cm À3 at an altitude of 85 km and maximum values of $1000 cm À3 at an altitude of 90 km. Importantly, these retrieved values are all well within the range of values suggested by MSP models and the available data from in situ observations [Hunten et al, 1980;Rapp et al, 2007].…”

Section: Resultsmentioning

confidence: 99%

“…[2] It is now common belief that meteor smoke particles (MSPs) form as a secondary product of meteoroid ablation in the altitude range between 70-110 km with average number densities of up to several 1000 cm À3 and particle radii in the low nanometer-range [Rosinski and Snow, 1961;Hunten et al, 1980]. Despite their tiny dimensions, it has been suggested that MSPs play a significant role in a host of atmospheric phenomena such as the nucleation of noctilucent clouds, the mesospheric metal atom chemistry, the transport of meteoric material to the ground, and the formation of nitric acid trihydrate-particles in polar stratospheric clouds [e.g., Plane, 2003;Gabrielli et al, 2004;Voigt et al, 2005].…”

Section: Introductionmentioning

confidence: 99%

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Meteor smoke particle properties derived from Arecibo incoherent scatter radar observations

Strelnikova

Rapp

Raizada

et al. 2007

Geophysical Research Letters

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[1] We present a new algorithm to infer information on the properties of charged meteoric smoke particles (MSPs) from the shape of incoherent scatter radar spectra. We show that in the presence of charged MSPs the spectrum can be approximated as the sum of two Lorentzians. These two distinct spectral lines correspond to two diffusion modes in the D-region plasma, i.e., one due the presence of positive ions and one because of heavy charged MSPs. The widths and amplitudes of these two spectral lines yield information on the radius and number density (the latter only for positively charged particles) of the charged MSPs. We apply this new algorithm to measurements obtained with the 430 MHz ISR at Arecibo and demonstrate that the observed spectra indeed bear the features anticipated in the presence of charged MSPs. Resulting values of retrieved MSP number densities and radii fall well within the range of values expected from models and independent in situ observations. Citation: Strelnikova, I., M. Rapp, S. Raizada, and M. Sulzer (2007), Meteor smoke particle properties derived from Arecibo incoherent scatter radar observations, Geophys. Res. Lett., 34, L15815,

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Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Meteor smoke particle properties derived from Arecibo incoherent scatter radar observations

Strelnikova

Rapp

Raizada

et al. 2007

Geophysical Research Letters

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“…The reason for the comparatively high value of the impact angles found in the experiments, compared to those required for mesospheric dust particles, is most likely that the pure ice particles in the experiments will totally sublimate at lower impact angles (Tomsic, 2001). On the other hand, mesospheric ice particles may contain many small meteoric particles (Rosinski and Snow, 1961;Hunten et al, 1980;Megner et al, 2006) which probably do not sublimate. Havnes and Naesheim (2007) suggested that mesospheric dust particles fragment during impact and that much or all of the ice within which the meteoric smoke particles are embedded, sublimates, while the meteoric smoke particles carry away charge from the surface where the impact takes place.…”

Section: Secondary Charge Production In the Nlc/pmse And Pmse Layermentioning

confidence: 98%

“…The required effectivity for the secondary charge production of the mesospheric dust is much larger than what is observed for pure water-ice particles in experiments. This, combined with a modelling of the impacts on the dust probe grids as a function of payload spin rotation angle, led Havnes and Naesheim (2007) to conclude that a model for the mesospheric dust could be a fairly loosely bound ice particle in which a considerable number of small meteoric particles (Rosinski and Snow, 1961;Hunten et al, 1980;Megner et al, 2006) of radius 1 nm are embedded. Upon impact, the large dust particle was assumed to fragment into many small subparticles each containing one or more meteoric smoke particle.…”

Section: Introductionmentioning

confidence: 99%

Mesospheric dust and its secondary effects as observed by the ESPRIT payload

Havnes

Surdal²,

Philbrick

2009

Ann. Geophys.

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Abstract. The dust detector on the ESPRIT rocket detected two extended dust/aerosol layers during the launch on 1 July 2006. The lower layer at height ∼81.5-83 km coincided with a strong NLC and PMSE layer. The maximum dust charge density was ∼−3.5×10 9 e m −3 and the dust layer was characterized by a few strong dust layers where the dust charge density at the upper edges changed by factors 2-3 over a distance of 10 m, while the same change at their lower edges were much more gradual. The upper edge of this layer is also sharp, with a change in the probe current from zero to I DC =−10 −11 A over ∼10 m, while the same change at the low edge occurs over ∼500 m. The second dust layer at ∼85-92 km was in the height range of a comparatively weak PMSE layer and the maximum dust charge density was ∼−10 8 e m −3 . This demonstrates that PMSE can be formed even if the ratio of the dust charge density to the electron density P =N d Z d /n e 0.01.In spite of the dust detector being constructed to reduce possible secondary charging effects from dust impacts, it was found that they were clearly present during the passage through both layers. The measured secondary charging effects confirm recent results that dust in the NLC and PMSE layers can be very effective in producing secondary charges with up to ∼50 to 100 electron charges being rubbed off by one impacting large dust particle, if the impact angle is θ i 20-35 • . This again lends support to the suggested model for NLC and PMSE dust particles (Havnes and Naesheim, 2007) as a loosely bound water-ice clump interspersed with a considerable number of sub-nanometer-sized meteoric smoke particles, possibly also contaminated with meteoric atomic species.

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Airborne mass spectrometers: four decades of atmospheric and space research at the Air Force Research Laboratory

Viggiano¹,

Hunton²

1999

J. Mass Spectrom.

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Smoke and Dust Particles of Meteoric Origin in the Mesosphere and Stratosphere

Cited by 570 publications

References 0 publications

Meteor smoke particle properties derived from Arecibo incoherent scatter radar observations

Meteor smoke particle properties derived from Arecibo incoherent scatter radar observations

Mesospheric dust and its secondary effects as observed by the ESPRIT payload

Airborne mass spectrometers: four decades of atmospheric and space research at the Air Force Research Laboratory

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