Volume 617, September 2018
|Number of page(s)||6|
|Section||Letters to the Editor|
|Published online||21 September 2018|
Letter to the Editor
Interplanetary dust delivery of water to the atmospheres of Pluto and Triton⋆
Space Sciences Laboratory, University of California at Berkeley, 7 Gauss Way, Berkeley, CA, USA
2 Dept. of Physics, University of Colorado at Boulder, Boulder, CO, USA
3 Laboratory for Atmospheric and Space Physics, University of Colorado at Boulder, Boulder, CO, USA
Accepted: 19 August 2018
Context. Both Pluto and Triton possess thin, N2-dominated atmospheres controlled by sublimation of surface ices.
Aims. We aim to constrain the influx and ablation of interplanetary dust grains into the atmospheres of both Pluto and Triton in order to estimate the rate at which oxygen-bearing species are introduced into both atmospheres.
Methods. We use (i) an interplanetary dust dynamics model to calculate the flux and velocity distributions of interplanetary dust grains relevant for both Pluto and Triton and (ii) a model for the ablation of interplanetary dust grains in the atmospheres of both Pluto and Triton. We sum the individual ablation profiles over the incoming mass and velocity distributions of interplanetary dust grains in order to determine the vertical structure and net deposition of water to both atmospheres.
Results. Our results show that <2% of silicate grains ablate at either Pluto or Triton while approximately 75% and >99% of water ice grains ablate at Pluto and Triton, respectively. From ice grains, we calculate net water influxes to Pluto and Triton of ~3.8 kg day−1 (8.5 × 103 H2O cm−2 s−1) and ~370 kg day−1 (6.2 × 105 H2O cm−2 s−1), respectively. The significant difference in total water deposition between Pluto and Triton is due to the presence of Triton within Neptune’s gravity well, which both enhances interplanetary dust particle (IDP) fluxes due to gravitational focusing and accelerates grains before entry into Triton’s atmosphere, thereby causing more efficient ablation.
Conclusions. We conclude that water deposition from dust ablation plays only a minor role at Pluto due to its relatively low flux. At Triton, water deposition from IDPs is more significant and may play a role in the alteration of atmospheric and ionospheric chemistry. We also suggest that meteoric smoke and smaller, unablated grains may serve as condensation nuclei for the formation of hazes at both worlds.
Key words: meteorites, meteors, meteoroids / Kuiper belt objects: individual: Pluto / planets and satellites: individual: Triton / planets and satellites: atmospheres / zodiacal dust
Data for Figs. 4 and 5 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/617/L5
© ESO 2018
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