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OMPS/LP observations of Russian meteor aftermath effect on Earth’s atmosphere

OMPS/LP observations of Russian meteor aftermath effect on Earth’s atmosphere. Nick Gorkavyi, Science Systems and Applications, Inc D.F. Rault, GESTAR, Morgan State University P.A . Newman, A.M. da Silva, NASA/GSFC. OMPS Science Team Meeting, June 6, 2013. Three points:

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OMPS/LP observations of Russian meteor aftermath effect on Earth’s atmosphere

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  1. OMPS/LP observations of Russian meteor aftermath effect on Earth’s atmosphere Nick Gorkavyi, Science Systems and Applications, Inc D.F. Rault, GESTAR, Morgan State University P.A. Newman, A.M. da Silva, NASA/GSFC OMPS Science Team Meeting, June 6, 2013

  2. Threepoints: • Suomi satellite detected new stratospheric “skybelt” from meteor dust around the planet in the mid-stratosphere • We can clearly see the Chelyabinsk bolide aftermath effect in OMPS/LP aerosol product (> 2 months). Observations corroborated with back trajectory analyses • We can evaluate meteor cloud parameters: particle size, rate of descent, total mass of particulates within cloud

  3. Meteor plume over Chelyabinsk on Feb 15th, 2013 • Meteor physical characteristics: • 60 feet in diameter, 10,000 metric tons, Velocity of 18.6 km/s • Exploded at 03:20 UTC (just after local sunrise), at altitude of 23.3 km with energy release equivalent to more than 30 Hiroshima atomic weapons • On the ground, meteoritic debris scattered over large area, and recovered fragments were found to be very small (typically sub-cm), bearing witness to intensity of air-burst explosion which pulverized the bolide during the 10 s duration atmospheric entry • The recovered meteoritic material consists of ordinary LL5chondrite

  4. View from North-West T ~ 4 min after explosion Mesospheric part of plume (>50 km) 23.3 km Large fraction of meteor dust transported upwards in air-burst mushroom cloud which rose quickly (~100 s) up to 33-35 km, above Earth’s Junge layer

  5. Meteor NPP SUOMI OMPS/LP On February 15th, OMPS/LP detected the meteor cloud in stratosphere Present talk: focus on meteor aftermath effect on atmosphere over ensuing 2 months: Feb 15th-Apr 15th

  6. Second detection of plume, Orbit 6753 First detection of plume, Orbit 6752 Chelyabinsk On February 15th, OMPS/LP detected the meteor cloud in stratosphere on two orbits: 3 h 35 min after meteor impact: near Novosibirsk, about 1100 km east of Chelyabinsk: eastward plume drift velocity of ~80 m/s 5 h 16 min meteor impact: near Chelyabinsk

  7. Mean Junge layer as measured by OMPS/LP Feb 8 – April 15, 2013 OMPS/LP observations above Junge layer Week prior to meteor Week 1 after meteor Week 2 Scale x 35

  8. Week 3 Week 4 Week 5 Week 7

  9. Meteor day-by-day cloud evolution

  10. February 16th • Plume detected several times on succeeding orbits and observed to stretch over 150° of longitude • Mean eastward velocity of ~35 m/s. • The vertical wind shear (from meteorological data) at these levels is consistent with the observed plume stretching • high altitude dust (40 km) • moving much faster (>60m/s) • low altitude dust (30 km) • moving much slower (~ 20 m/s) Meteor plume extinction is 10 times smaller than Junge layer but still detected by limb viewing OMPS/LP  Plume well above June layer Small Angstrom (Large particles) High plume above Junge  small extinction relative to Junge

  11. February 18th • Plume was observed from North America to the middle of the Atlantic ocean • Maximum plume density registered along the US/Canada border at altitudes of 36-37 km

  12. February 19th • 4 days after meteor impact the upper part of the meteor plume has circumnavigated the globe and returned over Chelyabinsk, 20000 km in 4 days: 200 km/h, 60 m/sec

  13. February 20th

  14. February 21st

  15. February 22nd

  16. February 23rd

  17. February 25th

  18. February 26th • Meteoric dust plume has formed a quasi-continuous mid-latitude “skybelt” located a few kilometers above the Junge layer. Skybelt settled on inside edge of polar vortex, as confirmed by the GEOS-5 model simulations

  19. February 27th

  20. February 28th

  21. March 1st

  22. March 2nd

  23. March 4th Larger Angstrom (Smaller particles) Lower plume above Junge  small extinction relative to Junge

  24. March 5th

  25. March 6th

  26. March 7th

  27. March 8th

  28. March 9th

  29. March 10th

  30. March 18th

  31. March 19th

  32. March 20th

  33. March 21st Larger Angstrom (Smaller particles) Lower plume above Junge  small extinction relative to Junge

  34. March 22nd

  35. March 23rd

  36. March 25th

  37. March 26th

  38. March 27th

  39. March 28th

  40. March 29th

  41. March 30th March 30, 2013 Larger Angstrom (Smaller particles) Lower plume above Junge  small extinction relative to Junge

  42. Meteor plume simulation with Goddard Trajectory Model (GTM) • The advection of sample parcels is traced using the wind / temperatures dataset from NASA’s MERRA reanalysis • Simulations initialized on Feb 15th at Chelyabinsk in a 150 km cylinder extending from 33.5 to 43.5 km • For each day, • - Red for 43.5 km • - Blue for 33.5 km 18th 16th 20th Chelyabinsk

  43. Meteor plume simulation with GEOS-5 Dust AOD on Feb 21, 12.00 UTC • 5 dust bins with radius at • 0.06, 0.11, 0.22, 0.44, 0.89 μm • Standard GEOS-5 processes: advection, diffusion, convection, dry/wet deposition, sedimentation • Initial dust distribution: 100 tons between 30 and 40 km centered at Chelyabinsk • A movie depicting time evolution of modeled plume • Figure shows snapshots of modeled plume about a week after initialization AOD Dust AOD on Feb 23, 21.00 UTC

  44. Time evolution of Meteor cloud (1) Meteor skybelt has a vertical depth of about 5 km, a width of about 300-400 km, a density of about 1 particle per cc. Total particulate mass within skybelt is estimated to be 40-50 metric tons.

  45. Time evolution of Meteor cloud (2) Plume optical depth slowly decreasing Particle size slowly decreasing from 0.2 to 0.05 μm 88 meters/ day - Sedimentation - Diabatic cooling Plume slowly drifting Northwards

  46. Conclusion • The Chelyabinsk meteor event was ideal for assessing OMPS/LP potentials: • - Large (60 feet diameter, 10000 tons) • - Highly observed (landed over a city, highly photographed) • - Easy to analyze composition (most of mass deposited onto snow) • - ideal for OMPS/LP •  high Northern latitudes: low SSA, confined within polar vortex •  entry during daylight • OMPS/LP was proven valuable to track the meteor plume in time / space • The models and stratospheric meteorological data assimilation allowed one to predict the evolution of meteoric dust plumes, suggesting a great potential for the assimilation OMPS/LP aerosol retrievals in near real-time. • The Earth is constantly impacted by meteors, and meteoric debris are known to contribute to high altitude atmospheric physics (such as condensation nuclei for stratospheric and mesospheric clouds). Further observations by OMPS/LP over its 5-year design lifetime will help in better understanding these effects. • The Chelyabinsk meteor plume can be used as test case for study of variability of spectra, TH problem and upgrading retrieval algorithm for local events.

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