ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5
Eugene Rozanov
PMOD/WRC, Davos and IAC ETH, Zurich, Switzerland [email protected]
Simulation of the NOy production by auroral electrons and solar protons and their effects on
ozone with the CCM SOCOL v3.0
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5New SPARC Chemistry-Climate Models inter comparison project (CCMI) started more than a year ago;
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5
First time ever EP are included in the forcing set of CCMI
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5
Solar variability. The solar radiative forcing data are provided at
http://sparcsolaris. gfz-potsdam.de/input_data. php. Daily,
spectrally-resolved solar irradiance data from the NRLSSI model
(Lean et al., 2005), which have been used in previous CCMVal and
CMIP5 experiments, are recommended.
In addition, the inclusion of atmospheric ionization by solar protons
(and related HOx and NOx production) are strongly encouraged by
using the GOES-based ionization rate data set and a methodology
to derive HOx and NOx production rates from Jackman et al.(2009).
Models capable of considering indirect particle effects by the
inclusion of an Ap-parameterized auroral source or upper boundary
condition are encouraged to do so.
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5AO CCM SOCOL/MPI-OM
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5
Recommended Ap index for CCMI runs
REF–C1,C2
REF–C2ST
2000
2008
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5
Applied SPE IR (annual mean: 50 km, polar cap)
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5Ion and neutral chemsitry:Treatment in the models
Below 90 km:
Complete ion chemsitry (50+ species) - SOCOLi Computationally expensive
Parameterizations of NOx and HOx production
• Porter et al., 1976; Solomon et al., 19810.7 N*, 0.55 N(4S) and 2 HOx per ion pair;widely applied below 90 km (WACCM, HAMMONIA, EMAC, SOCOL...)
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5NOx and HOx production
Widely used parameterization(0.7 N* + 0.55 N(4S) + up to 2 HOx per Ion Pair)
against
complete ion chemistryCCM SOCOL (Egorova et al., 2011)
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5Ion and neutral chemsitry:Treatment in the models
Below 90 km:
• Verronen and Lehman, 2013LUT, includes HNO3 production
• Nieder et al., 2014 (LUT)LUT
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5
Applied annual mean Ap index
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5Ion and neutral chemsitry:Treatment in the models
Above 90 km: 5-ion scheme – WACCM, HAMMONIA
NOx (ppbv) from MIPAS. HEPPA-2, Courtesy of B. Funke
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5
Baumgartner et al, 2009
Treatment of the auroral electrons in SOCOL
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5Time evolution of VMR CO 70oS-90oS
Simulated CO (ppbv)
MIPAS CO (ppmv), Funke et al., 2014a
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5Time evolution of VMR CH4 70oS-90oS
Simulated CH4 (ppbv)
MIPAS CH4 (ppmv), Funke et al., 2014a
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5Time evolution of VMR NOy 70oS-90oS
Simulated NOy (ppbv)
MIPAS NOy (ppmv), Funke et al., 2014a
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5Time evolution of VMR NOy 70oS-90oS
Simulated NOy (ppbv)
MIPAS NOy (ppmv), Funke et al., 2014a
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5Time evolution of VMR NOy 70oN-90oN
Simulated NOy (ppbv)
MIPAS NOy (ppmv), Funke et al., 2014a
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5Time evolution of VMR NOy 70oN-90oN
Simulated NOy (ppbv)
MIPAS NOy (ppmv), Funke et al., 2014a
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5How to extract EPP-NOy
1. By comparison with the reference model runsPro: clear approach.Contra: not compatible with observations. 2. Using correlations with other tracer (e.g., CH4, CO)Pro: comparable to observation.Contra: Not always clear what we are getting. 3. Multiple linear regression analysisPro: potentially comparable to observation.Contra: Not so easy to introduce time lag.
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5Time evolution of VMR NOy 70oS-90oS
Simulated NOy (ppbv) w/o EPP
Simulated NOy (ppbv) with EPP
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5NOy (ppbv) produced by EPP(70oS-90oS, 1960-2006 mean)
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5NOy produced by EPP relative to background
(70oS-90oS, 1960-2006 mean)
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5NOy produced by EPP relative to background
(70oS-90oS, 1960-2006 mean)
EPP contribution to NOy column 20-70 km (Funke et al., 2014a)
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5How to extract EPP-NOy
1. By comparison with the reference model runsPro: clear approach.Contra: not compatible with observations. 2. Using correlations with other tracer (e.g., CH4, CO)Pro: comparable to observation.Contra: Not always clear what we are getting. 3. Multiple linear regression analysisPro: potentially comparable to observation.Contra: Not so easy to introduce time lag.
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5EPP-NOx from NOx-CH4 correlations
From Randall et al., 2007)
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5EPP-NOx from NOx-CH4 correlations
From Randall et al., 2007)
ISS
I te
am
work
sh
op
, B
ern
, 1
9-2
3
Jan
uary
, 2
01
5
Conclusions
SPE and auroral electrons influence on the atmosphere were
simulated with CCM SOCOL in the framework of CCMI project
using SPR induced ionization and parameterized NOx influx;
The influence of EPP on NOy is visible in the model output
The response of NOy is in qualitative agreement with satellite
data
The influence of both SPE and auroral electrons is visible
The work on the evaluation of quantitative agreement between
model and satellite data is in progress
