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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
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Three points:
• 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
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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 LL5 chondrite
Meteor plume over Chelyabinsk on Feb 15th, 2013
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View from North-WestT ~ 4 min after explosion
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
23.3 km
Mesospheric part of plume (>50 km)
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On February 15th, OMPS/LP detected the meteor cloud in stratosphere
NPP SUOMI
OMPS/LP
Meteor
Present talk: focus on meteor aftermath effect on atmosphere over ensuing 2 months: Feb 15th-Apr 15th
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First detection of plume,Orbit 6752
Second detection of plume,Orbit 6753
Chelyabinsk
On February 15th, OMPS/LP detected the meteor cloud in stratosphere on two orbits:1. 3 h 35 min after meteor impact: near Novosibirsk, about 1100 km east of
Chelyabinsk: eastward plume drift velocity of ~80 m/s2. 5 h 16 min meteor impact: near Chelyabinsk
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Mean Junge layer as measured by OMPS/LPFeb 8 – April 15, 2013
OMPS/LP observations above Junge layerWeek prior to meteor
Week 1 after meteor
Week 2
Scale x 35
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Week 3
Week 4
Week 5
Week 7
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Meteor day-by-day cloud evolution
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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)
Plume well above June layer Small Angstrom (Large particles) High plume above Junge small extinction relative to Junge
Meteor plume extinction is 10 times smaller than Junge layer but still detected by
limb viewing OMPS/LP
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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
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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
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February 20th
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February 21st
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February 22nd
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February 23rd
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February 25th
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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
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February 27th
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February 28th
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March 1st
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March 2nd
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March 4th
Larger Angstrom (Smaller particles) Lower plume above Junge small extinction relative to Junge
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March 5th
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March 6th
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March 7th
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March 8th
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March 9th
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March 10th
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March 18th
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March 19th
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March 20th
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March 21st
Larger Angstrom (Smaller particles) Lower plume above Junge small extinction relative to Junge
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March 22nd
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March 23rd
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March 25th
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March 26th
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March 27th
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March 28th
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March 29th
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March 30th
Larger Angstrom (Smaller particles) Lower plume above Junge small extinction relative to Junge
March 30, 2013
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Meteor plume simulation with Goddard Trajectory Model (GTM)
16th
20th
18th• 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
Chelyabinsk
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Meteor plume simulation with GEOS-5
• 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
Dust AOD on Feb 21, 12.00 UTC
Dust AOD on Feb 23, 21.00 UTC
AOD
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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.
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Time evolution of Meteor cloud (2)
88 meters/ day - Sedimentation - Diabatic cooling
Particle size slowly decreasing
from 0.2 to 0.05 μm
Plume optical depth slowly decreasing
Plume slowly drifting
Northwards
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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.