Measuring the Antarctic Ozone Hole with the new Ozone Mapping and Profiler Suite (OMPS)

Measuring the Antarctic Ozone Hole with the new Ozone Mapping

and Profiler Suite (OMPS)

Natalya Kramarova, Paul Newman, Eric Nash, PK Bhartia, Richard McPeters, Didier Rault, Colin Seftor, Gordon Labow

OMPS meeting, June 6, 2013

Objectives• Can OMPS reasonably represent the Antarctic

ozone hole?

• Do the metrics derived from OMPS match OMI and MLS?

• Is OMPS an improvement?


Outline:

I. Introduction

II. The Ozone Mapping and Profiler Suite (OMPS)

III. Validation of OMPS measurements

IV. OMPS ozone hole first results

V. Conclusions


OMPS NP vs OMPS LP

Coincidence criteria: +/-0.5 hour, +/-1° latitude, +/-4° longitude.

September –November 2012



Biases increase for higher latitudes

SBUV vs OMPS NPSeptember –November 2012

Coincidence criteria: +/-4 hour, +/-1° latitude, +/-5° longitude.



OMPS NP overestimates ozone compared to SBUV

OMPS LP vs Aura MLSSeptember –November 2012

Coincidence criteria: +/-1 hour, +/-1° latitude, +/-4° longitude.



OMPS LP and Aura MLS vs Neumayer Sonde (70.6S, 8W)September –November 2012, 36 balloon measurements

Coincidence criteria: 1000-km distance from the station (dist. weight. average); same day.



Aura MLS/OMPS LP vs Neumayer SondeIII. Validation of OMPS measurements


OMPS LPAura MLS

SONDESONDE

OMPS TC vs OMPS NP57.5S 62.5S 67.5S 72.5S 77.5S

Bias, % -0.6 -0.1 -0.1 -0.5 -0.5

Std dev % 1.2 2.1 2.1 2.3 2.4

57.5S 62.5S 67.5S 72.5S 77.5S

Bias, % -0.9 -0.5 0.3 0.7 1

Std dev % 3.6 4.3 4.7 4.3 3.5

OMPS NP vs SBUV NOAA18

OMPS NP vs SBUV NOAA1957.5S 62.5S 67.5S 72.5S 77.5S

Bias, % -0.8 -0.7 -0.4 -0.2 -0.6

Std dev % 3.4 3.8 3.9 3.7 3.3

Total ozone column comparisonsIII. Validation of OMPS measurements


•Biases < 1%• Standard deviation is 3-4%



Total ozone, October 2012



Total ozone, October 2012Low values generally found

inside ozone hole

Higher values found outside ozone hole everywhere



Area of the Antarctic ozone hole based on TOMS and OMI measurements. Red bar shows an estimate from OMPS TC.

2012 Antarctic ozone hole was 2nd smallest observed in the last twenty-

three years — only the major warming 2002 ozone hole was smaller

OMPS compares quite well with OMI, but slightly smaller because of the high bias



Evolution of 2012

Antarctic ozone hole

“Normal” development up to mid-September

Area

Minimum

More rapid disappearance after mid-September

IV. OMPS ozone hole first resultsO

MPS m

eeting, June 6, 2013

Location of the ozone hole center for September,

October, and November


MPS m


Total ozone values following the ozone hole


MPS m


Ozone profile following the ozone hole’s center


MPS m


Strong depletion of ozone in the

14-24 km region


MPS m


Lowest total ozone value

reached about Oct. 1


MPS m


Lowest profile value reached about Oct. 11


MPS m


Strong build-up of ozone in the

middle stratosphere

leads to overall ozone increase


MPS m


Large ozone loss sharpens the vertical gradient. The gradient’s

altitude is related to the Cl levels. As Cl declines, the gradient should

move to lower altitudes.


MPS m



MPS m


+

+

+

=



High ozone concentration in the lowermost stratosphere

Clear signs of ozone depletion in the upper layer



The 3 layers show depletions by mid-September

Deep ozone hole



Area of the hole decreases

Deep ozone hole

Total ozone min ~ 1 Oct.



Notable decrease of the hole area in middle and upper stratosphere

Min ozone at mid Oct

Signs of ozone recovery



Ozone hole splits



• Ozone increasing in all 3 layers• Total ozone shows a rapid

increase by late-November

V. Conclusions (1)

• OMPS suite began routine operations in 2012. – OMPS is derived from the strong heritage of UV-Vis satellite

instruments that extend from the 1970s;– Will become the standard ozone monitoring instrument

aboard the US polar orbiting satellites. • OMPS performs quite reasonably.

– direct comparisons of OMPS TC to the OMI column observations show differences of <1%;

– comparisons of the ozone profiles obtained from OMPS LP and NP with the profiles from the Aura MLS, SBUV, and ozone sondes show good agreement (biases <5-8% and std dev <5-10%) in the vertical range 20-45 km;

– good agreements between OMPS TC and OMI on estimates of the average minimum ozone and ozone hole area.


V. Conclusions (2)

• 2012 ozone hole – 2nd smallest since 1988 - weakest ozone hole was 2002 – driven

by the first observed major SSW observed in the SH;– Early development (Aug. to mid-Sep.) was normal – still plenty

of Cl and Br for ozone loss. In the lower stratosphere, large losses seen in the LP from early Sep. to about 11 Oct. Ozone near zero at 16 km altitude by Oct. 11. Lowest column seen about Oct.1. Very strong vertical gradient develops by early October;

– Extremely high values of ozone seen in upper stratosphere by Mid-October as ozone is advected over Antarctica;

– Ozone hole disappeared (late-Sep to Nov) quite rapidly in comparison to the ozone holes in the last 20-year period, because of the strong wave dynamics, faster warming during Austral spring, and stronger advection.


Measuring the Antarctic Ozone Hole with the new Ozone Mapping and Profiler Suite (OMPS)

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