Japan-France planetary atmospheric modeling workshop,
2015/05/11, Kobe Univ.

Development of the Japanese-German
Mars GCMs: Toward the coupling
between lower and upper atmosphere
Takeshi Kuroda
Tohoku University

A.S. Medvedev, P. Hartogh
Max Planck Institute for
Solar System Researsh
And more collaborators…

Our brief history----

Kuroda started to develop a MGCM based on CCSR/NIES (Center for
Climate System Research, Univ. of Tokyo / National Institute forEnvironmental Studies) AGCM as a student of CCSR (get master in 2001,and Ph.D. in 2006).
Also Kuroda started to work at the Max Planck Institute for Solar System
Research since 2004, and engaged in the development of a MGCM there(MAOAM). Medvedev also started to work there in the same year.
We have produced publications about atmospheric dynamics mainly;
baroclinic waves [Kuroda et al., 2007], semi-annual oscillations [Kuroda etal., 2008], winter polar warming [Medvedev and Hartogh, 2007; Kuroda etal., 2009], etc…
We published a review paper about the effects of dust on the martian
meteorology [Medvedev et al., 2011, Aeolian Research].
Our recent main topics are gravity waves, CO2 snowfall, etc… (shown later)
Now the collaborations between Tohoku Univ. and MPS with the “Promotionof the strategic research program for overseas assignment of young
scientists and international collaborations” of JSPS is ongoing (October
2013 – March 2016), and Kuroda stays in MPS for about a year in total
during this period (actually I just came back from Germany last Saturday!).

Review paper from Aeolian Research

Refractive index of dust

Dust storm changes circulation

http://c.gp.tohoku.ac.jp/~promotion/index-en.html

DRAMATIC MGCM (Japanese)
Developments up to now
Dynamical core
CCSR/NIES(/FRCGC) AGCM 5.4.02 (Kuroda’s master thesis,2001) →5.4g (Kuroda’s first paper, 2005 and Ph.D. thesis,2006)→5.6→5.7b (MIROC 4.0 at present)
3-D primitive equations (spectral solver)Started to be called as “DRAMATIC MGCM” since ~2010(DRAMATIC = Dynamics, RAdiation, MAterial Transport and their mutualInteraCtions)

Resolution- Horizontal: T21(~5.6º× 5.6º, grid interval in equator of ~333km)- Vertical: σ level, currently 49-69 layers(model top of ~80-100 km)

Surface parameters (current)- Topography: MGS-MOLA observations [Smith et al., 1999]- Albedo and thermal inertia: MGS-TES observations[Putzig and Mellon, 2007]- Roughness: From MGS-MOLA data [Heavens et al., 2008]

From Forget et al. [1998]

CO2 phase change (1)The condensed CO2 ice falls by the gravitational sedimentation.
Then the thermodynamic effects (①-③ below) and resulting
exchange between atmosphere and ice are made.
If T * (predicted temperature) < Tc (condensation temperature)T * = Tc

δmN =
δml =

cpM NLcpM l(T − T )*NcN1(T − T ) − [g (z − z ) + c (T − T )] ∑ δm (in l ≤ N - 1)
LLN*l +1lcl②①icelcl +1clk =l +1k③()

If all the falling ice sublimes in layer l i.e. − δml > ∑k =l +1 δmk ,Tl = Tl * +[N)](N1− L + g ( zl +1 − zl ) + cice Tcl +1 − Tcl ∑ δmkcpM lk =l +1

At surface (l = 0), c p M l is replaced by cs A,and ∑k =0 δmk is added to the ground ice amount m0 .
N()

If the ground ice completely sublimes i.e. − δm0 > m0 + ∑k =1 δmk ,T0 = T0* −

[N()]

NL
1L − g ( zl +1 − zl ) − cice Tc1 − Tc0 ∑ δmkm0 −
cs A
cs A
k =1

Accounting for the loss of atmospheric mass due to condensation,

δp 0 = −g N
∑ δmkA k =0

① Release of the latent heat
② Potential energy released by ice
falling③ Energy used to heat the ice tothe condensation temperature oflower level

Previously the condensed CO2fell to the surface immediately,
but with the way the result of
CO2 ice cap thickness largely
depended on the timestep ofcalculation: bad for different
resolution or model top height.

Modify the surface pressure to conserve
the total mass of CO2 (caps + atmosphere)CO2 phase change (2)Implementation of gravitational sedimentation (since 2010)
Modified Stokes’ law [Kasten, 1968]
2 ρgr 2  λ  Cr 
vsed = 
1 +  A + B exp −9η  r λ 

η: Dynamic viscosity
λ: Mean free path length
r: CO2 ice radiusρ: Density of CO2 ice (=1600 kg m-3)
A, B, C: Dimensionless empirical constants;
A=1.15, B=0.497, C=0.92 for CO2 air [Rader, 1990]

Definition of CO2 ice radius
r0: Radius at 0m height (=50μm) [e.g. Hayne et al., 2012](very simple)r ( z ) = r0 exp(− z h )h: Particle radius scale height (=20km)→1μm at ~78km height, which is consistent with the observations of
mesospheric CO2 ice clouds [e.g. Määttänen et al., 2010]

Seasonal-latitudinal crosssection of simulated zonal-mean
CO2 ice cloud distributions at1Pa(~64km) [ppm of mass]
Consistent with the observations[Määttänen et al., 2010;
McConnochie et al., 2010](presented in Paris workshop, 2011)

CO2 snowfalls in winter polar atmosphere[Kuroda et al., 2013, GRL]
Figure on the paper(a) 25km height snowfall(b) surface accumulation rate
at 80°N(Animation)(3-D feature)

Radiation (from my Ph.D. thesis, 2006)- CO2: Absorption and emission in the infrared wavelength(15μm, 4.3μm) and near-infrared solar absorption(the non-LTE effect is not considered)- Dust: Absorption, emission and scattering in 0.2-200μm- CO2 infrared: mstrnX[Sekiguchi and Nakajima, 2008]- CO2 NIR heating:from Forget et al. [1999, 2003]
Ls=90°

Ls=270°[Forget et al., 2003,
Granada workshop]

Heating rate by
CO2 NIR solar
absorption [K/sol]Dust radiation
Assuming the refractive index and particle size distribution
based on the observations of Martian dust
ImaginaryReal

Refractive index: fromWolff and Clancy [2003](Refractive B)
Refractive A: oldstandards [Ockert-Bell etal., 1997; Toon et al.,
1977; Forget, 1998]Particle size distribution:from Tomasko et al. [1999](reff=1.6 μm, veff=0.2 μm)(Modified Gammafunction)n(r ) = cr

(1−3ν eff ) ν eff[exp − r / reff ν eff]Sensitivity test of dust
parameters on the heating
rate and temperatureτdust~2.2, Ls=207.5° (assuming MY25 storm), daytime
Refractive B,
PSD 1

Heating
rate in<4μm[K/sol]T[K]

Refractive A,
PSD 1

Refractive A,
PSD 2

Refractive A,
PSD 3

Water cycle (since 2008)- Based on the large scalecondensation(supersaturated water vapor
condenses to the water ice)
- Implementation of thegravitational sedimentation(modifies Stokes’ law, same
Estimation of water particle size
based on Montmessin et al. [2004]
as CO2 ice)(no supersaturation)- Accumulation of surface
r : Radius of water ice
water ice, including the
1 / 3 M : Water ice mass in the grid/layer
ρ : Density of water ice (917 kg m )change of surface albedo rc =  M c + r03  N:
Number of dust particles in the (4 / 3)πρi N grid/layer(absorption by the regolithr ： Radius of dust particle (as nuclei)
is not assumed)M
M : Mass of dust in the grid/layer
N=- Sublimation of surface iceρ : Density of dust (2500 kg m )( 4 / 3)πρ r
by the turbulent fluxr : Radius at 0km height(0.8μm)
cc-3

i0d3d 0r0 ( z ) = rz 0 exp(− z h )dd-3z0h: Scale height of the particle radius (18km)

Water vapor column density(8-20 Martian years from the isothermal state)
No supersaturation

Assuming 10 times
supersaturation (simplythe saturation amountof water vapor is set to
10 times of thetheoretical value)

In the initial isothermal state, About the possibility
north of 80°N is assumed asof 10-times superthe water ice sheet withsaturation (SPICAM)
limitless water, and no water[Maltagliati et al.,vapor/ice in the atmosphere.
2011]

Water ice cloud optical depth(8-20 Martian years from the isothermal state)

No supersaturation

10 times
supersaturation
Water ice radius in Ls=90º(no supersaturation)

Obviously too much, considering theimprovements.

HDO/H2O isotopic fractionation(since 2011)

SMOW(D/H): 1.56×10-4(Standard Mean Ocean Water)

Merlivat and Nief [1967]’s formula

α=1.72: 160K
1.51: 180K
1.37: 200K

Two idealized estimations [Montmessin et al., 2005]
Rapid isotopic Homogenization case (RH): Rayleigh Distillation case (RD):Appropriate for liquid clouds
Appropriate for ice clouds
(1)

(2)

(1) is adopted for the fractionation in the atmosphere, and(2) is adopted for the surface ice.

HDO/H2O ratio in the water vapor column density[vrt. SMOW]
No supersaturation

10 timessupersaturation[Kuroda et al., 2012,Mars Recent Climate
Change Workshop,
NASA/Ames]

Seasonal-latitudinal change of[Montmessin et al., 2005] dust opacity: 0.2~1 in visible

In the initial state, the HDO/H2O
ratio of the ice sheet in north of 80°
N is set to 5.6 vrt. SMOW, based on
the observations for Mars.

Radiative effects of water ice clouds(since 2015)
These are really preliminary results,
which still need a lot of improvements…
T by MGS-TES [Smith et al., 2001]

With radiative effects

T[K]Watercloudmass
mixingratioWithout radiative effects

MAOAM-GCM(German)• Project started in April 2002
• Based on COMMA (COlogne Model of the MiddleAtmosphere), from surface to ~130km height (lowerthermosphere)• New efficient non-LTE radiation scheme[Feofilov et al., 2006, Granada workshop]• Kuroda’s contribution:
Implementation of a dust
radiation scheme• First paper was published in2005 (Hartogh et al., JGR)
Strong polar warming produced

GCM intercomparison in 2006
(Second workshop on Mars atmosphere modelling andobservations @Granada, Spain)

MCS observation [McCleese et al., 2008]

Only MAOAM well
reproduced the winterpolar warming above~60 km!

New MAOAM-GCM(Medvedev et al., 2011, JGR; Medvedev and Yigit,2012, GRL; Medvedev et al., 2013, JGR)
• New dynamical core of Kühlungsborn Mechanistic General
Circulation Model (KMCM) with spectral solver• Horizontal resolution of ~5.6º× 5.6º , 67 hybrid vertical levels
up to 150-160 km• EUV heating is implemented[Torr et al., 1979; Richards et al., 1994]• Gravity wave drag parameterization (dynamical and thermaleffects)(a) No GW drag(b) GW drag (only dynamical)(c) GW drag (dynamical andthermal)(d) Geopotential height[Medvedev and Yigit, 2012]Effects of the global dust storm in MY25 and MY28 on
the thermosphere [Medvedev et al., 2013]

Future plans with both MGCMs(and more)• Radiation scheme of both MGCMs will be common(effects of CO2 and dust/cloud particles in lower atmosphere, nonLTE effects of CO2 radiation in middle atmosphere, EUV heating inupper atmosphere)• DRAMATIC: Implementation of the atmospheric chemistry for theapproach to the interactions between lower (water cycle, duststorm) and upper (atmospheric escape) atmospheres(DRAMATIC will be the abbreviation of “Dynamics, RAdiation, MAterial
Transport, Isotopomer and Chemistry”)• Medvedev and Kuroda participate in the MAVEN science team(IUVS, NGIMS): studies using the obtained data ofcomposition/density profiles are planned• Development of a Jupiter stratospheric GCM (will be talked onThursday)• And so on… (preparing for some publications…)