1996
DOI: 10.1016/0273-1177(95)00763-5
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Characteristics of the plasma from A 94 kms−1 micro-particle impact

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Cited by 26 publications
(19 citation statements)
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“…The range of ion energies required to fit peaks in the flight spectra is greater than previously reported in some laboratory experiments. For higher-velocity impacts, our results are in good agreement with both Ratcliff and Allahdadi (1996) and Hornung et al (1996), with ion energies of hundreds of eV. For the low-velocity impacts (o10 km s À1 ), which produce cluster ion spectra, we obtain good fits to the data using ion energies of up to $80 eV, contrasting with the results of Friichtenicht, quoted by Ratcliff and Allahdadi (1996), of 0.5 eV for metallic target ions (impact velocities of 17-47 km s À1 ).…”
Section: Discussionsupporting
confidence: 81%
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“…The range of ion energies required to fit peaks in the flight spectra is greater than previously reported in some laboratory experiments. For higher-velocity impacts, our results are in good agreement with both Ratcliff and Allahdadi (1996) and Hornung et al (1996), with ion energies of hundreds of eV. For the low-velocity impacts (o10 km s À1 ), which produce cluster ion spectra, we obtain good fits to the data using ion energies of up to $80 eV, contrasting with the results of Friichtenicht, quoted by Ratcliff and Allahdadi (1996), of 0.5 eV for metallic target ions (impact velocities of 17-47 km s À1 ).…”
Section: Discussionsupporting
confidence: 81%
“…For higher-velocity impacts, our results are in good agreement with both Ratcliff and Allahdadi (1996) and Hornung et al (1996), with ion energies of hundreds of eV. For the low-velocity impacts (o10 km s À1 ), which produce cluster ion spectra, we obtain good fits to the data using ion energies of up to $80 eV, contrasting with the results of Friichtenicht, quoted by Ratcliff and Allahdadi (1996), of 0.5 eV for metallic target ions (impact velocities of 17-47 km s À1 ). The ion energies we derived for low-velocity impacts do, however, agree with those found by Burchell et al (1996) of tens of eV and we remain unable to explain the discrepancy with Friichtenicht's results.…”
Section: Discussionsupporting
confidence: 81%
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“…1,2 In addition, chemical reactions, including dissociation and recombination, can take place within the resultant fluid phases, especially in gas-phase and ionized species. [3][4][5] Understanding the chemical changes associated with impacts is essential to understanding the impact accretion planetary formation process as it occurs on different lengths and timescales upon the initial differentiation and evolution of planets. Toward the end of the Earth's accretion, impacts from the increasingly larger planetesimals (which themselves accreted to masses within the planetary range) resulted in at least one giant collision that is hypothesized to have resulted in Moon formation.…”
Section: Introductionmentioning
confidence: 99%