Atmospheric Chemistry of Meteoric Metals

Plane, J. M. C.

doi:10.1021/cr0205309

Cited by 328 publications

(448 citation statements)

References 171 publications

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“…25,26 Si atoms were generated in a slow flow reactor by LIF was collected through an interference filter ( max = 250 nm, FWHM = 10 nm) using a photomultiplier tube (Electron Tubes, model 9816QB) placed orthogonal to both the photolysis and probe beams. Si( 3 P J ) was detected resonantly in the J = 0, 1 and 2 spin-orbit states by exciting the transitions 3p 2 The concentrations of O 2 , CO 2 and organo-silicon vapour were calculated from the mass flow rates and absolute pressure in the reactor. Diluted mixtures of these species were prepared in a glass vacuum line by making them up to a known ratio in about 800 Torr of bath gas (N 2 or He) in 10 dm 3 glass bulbs.…”

Section: Experimental Setup Apparatusmentioning

confidence: 99%

Kinetic studies of atmospherically relevant silicon chemistry : Part I: Silicon atom reactions

Martı́n

Blitz

Plane

2009

Phys. Chem. Chem. Phys.

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Section: Experimental Setup Apparatusmentioning

confidence: 99%

Kinetic studies of atmospherically relevant silicon chemistry : Part I: Silicon atom reactions

Martı́n

Blitz

Plane

2009

Phys. Chem. Chem. Phys.

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“…Upon impact, the large dust particle was assumed to fragment into many small subparticles each containing one or more meteoric smoke particle. While most of the water ice on the fragments would sublimate during the impact, the meteoric smoke particles made of metals and silicate compounds (Plane, 2003) should survive and a considerable fraction of them would carry away a negative charge.…”

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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“…[2] The source of the layer of sodium (Na) atoms between 80 and 105 km in the mesosphere/lower thermosphere (MLT) is the ablation of approximately 10-100 tons of interplanetary dust that enter the atmosphere each day [Plane, 2003]. Since its development in the 1970s, the Na resonance lidar technique has enabled the Na layer to be observed with excellent spatial and temporal resolution [Clemesha et al, 1981;von Zahn et al, 1988;She et al, 1990].…”

Section: Introductionmentioning

confidence: 99%

Retrieval of global mesospheric sodium densities from the Odin satellite

Gumbel¹,

Fan²,

Waldemarsson³

et al. 2007

Geophysical Research Letters

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[1] Satellite observations of the Na D dayglow at 589 nm provide a global database for the climatology of the mesospheric sodium layer. More than five years of Na D limb observations are available from the Optical Spectrograph and InfraRed Imager System onboard the Odin satellite. We describe a robust retrieval method that provides individual sodium density profiles with a typical accuracy of 20% and altitude resolution of 2 km. Retrieved column abundances and density profiles are validated against sodium resonance lidar measurements at mid-latitudes. Examples of the seasonal and latitudinal variation of the sodium layer illustrate Odin's potential for climatological studies of mesospheric metals. Citation:

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Atmospheric Chemistry of Meteoric Metals

Cited by 328 publications

References 171 publications

Kinetic studies of atmospherically relevant silicon chemistry : Part I: Silicon atom reactions

Kinetic studies of atmospherically relevant silicon chemistry : Part I: Silicon atom reactions

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

Retrieval of global mesospheric sodium densities from the Odin satellite

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