To further our understanding of important photochemical processes in the Martian atmosphere, a synthesis can be used to investigate the temporal and spatial agreement between model and observations and determine any possible causes of identified differences. In this study [1], we have assimilated, for the first time, total ozone into a Mars Global Circulation model (GCM) to study the ozone cycle

Holmes, J. A.

Lefèvre, F.

Lewis, S. R.

Patel, M. R.

English

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Open Research OnlineThe Open University’s repository of research publicationsand other research outputsFirst ozone reanalysis on Mars using SPICAM dataConference or Workshop ItemHow to cite:Holmes, J. A.; Lewis, S. R.; Patel, M. R. and Lefe`vre, F. (2018). First ozone reanalysis on Mars using SPICAM data.In: From Mars Express to ExoMars, 27-28 Feb 2018, Madrid.For guidance on citations see FAQs.c© 2018 The AuthorsVersion: Version of RecordLink(s) to article on publisher’s website:https://www.cosmos.esa.int/documents/1499429/1583871/Holmes J.pdfCopyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyrightowners. For more information on Open Research Online’s data policy on reuse of materials please consult the policiespage.oro.open.ac.ukScientific Workshop: “From Mars Express to ExoMars” 27–28 February 2018, ESAC Madrid, Spain  Workshop organized by ESA-ESAC & IAA-CSIC, with the support of the ESAC Faculty and the EU H2020 project UPWARDS First ozone reanalysis on Mars using SPICAM data J. A. Holmes1, S. R. Lewis1, M. R. Patel1,2 and F. Lefèvre3 1School of Physical Sciences, Open University, UK, 2 Space Science and Technology De-partment, STFC, RAL, UK, 3LATMOS, CNRS/Université Pierre et Marie Curie, France   Introduction: To further our understanding of important photochemical processes in the Mar-tian atmosphere, a synthesis can be used to investigate the temporal and spatial agreement between model and observations and determine any possible causes of identified differences. In this study [1], we have assimilated, for the first time, total ozone into a Mars Global Circulation model (GCM) to study the ozone cycle.  Model Setup & Assimilation: We use the UK version of the Laboratoire de Météorologie Dy-namique (LMD) Mars GCM. This 4D-model uses the physical parameterisations [2] and LMD photochemical module [3] shared with a recent version of the LMD Mars GCM coupled to a UK-only spectral dynamical core and semi-Lagrangian advection scheme [4].It has been developed in a collaboration between the LMD, the Open University, the University of Oxford and the Instituto de Astrofisica de Andalucia. The model was run at T31 resolution in the hori-zontal, corresponding to a resolution of 5° latitu-de by 5° longitude, with 32 vertical levels in the range 0–105 km. The Mars GCM includes the latest sub-models to provide the most realistic modelling of the planetary boundary layer and water and dust cycles [5,6,7]. The photochemi-cal module provides multiple photolytic and chemical reactions with up-to-date reaction ra-tes between 16 advected species including car-bon dioxide, water vapour and ozone. It also includes heterogeneous processes removing odd hydrogen radicals, a process which has been shown to improve the agreement between models and observations [8]. The assimilation is performed using a form of the Analysis Correction scheme [9] converted to martian con- ditions, and has been shown in the past to be a computation- ally inexpensive and robust method [10]. Using this methodology, observations of short-lived (and long-lived) spe-cies can be supplemented by knowledge of the transport and atmospheric chemistry from a Mars GCM.  SPICAM retrievals: The retrievals assimilated in this study (displayed in Figure 1a) are from the SPICAM instrument on Mars Express pre-sented in [11]. Maximum total ozone values are seen around northern hemisphere spring equi-nox at northern polar latitudes, as a result of polar night conditions in the recent past and a lack of odd hydrogen species. The SPICAM ins-trument is able to observe large ozone abun-dance before water vapour and associated odd hydrogen species are transported into the nort-hern polar regions resulting in destruction of ozone.  Figure 1: SPICAM nadir retrievals for LS = 341° MY 26 to LS = 69° MY 28 as a function of latitude and solar longitude displaying a) the total ozone abundance and b) number of retrievals. The number of SPICAM retrievals are binned every 5° LS and 5° latitude.  For the first assimilation of ozone for Mars, the dynamically determined wind field from the Mars GCM is used to transport ozone and all other chemical species, but future investigations could potentially also assimilate thermal profiles alongside ozone retrievals. This highlights anot-her benefit of data assimilation, in that data sparse regions are potentially influenced by SPICAM retrievals of total ozone being advected into the local unobserved region.  Results of the ozone reanalysis: To investi-gate the effect of total ozone assimilation on the seasonal cycle, we ran a ‘control’ simulation with no assimilation and a second simulation in which total ozone retrievals from SPICAM were assimilated (hereafter the SPICAM ozone rea-Scientific Workshop: “From Mars Express to ExoMars” 27–28 February 2018, ESAC Madrid, Spain  Workshop organized by ESA-ESAC & IAA-CSIC, with the support of the ESAC Faculty and the EU H2020 project UPWARDS nalysis). Differences in the modelled and ob-served ozone cycle (Figure 2b) are efficiently identified by the assimilation process, with the largest total ozone percentage differences iden-tified between 45°S–10°S from LS = 135–180° and at northern polar (60°N–90°N) latitudes from LS = 150–195°, at the onset of northern polar winter. An asymmetry in the magnitude of total ozone percentage differences in northern fall (LS = 150–195°) and early northern spring (LS = 0–30°) at northern polar latitudes is also identified. Through investigation of the water cycle, underestimated amounts of total ozone in the control simulation were found to be due to excessive northward transport of water vapour west of the Tharsis region and over Arabia Terra throughout northern polar winter resulting in in-creased increments in total ozone necessary in the SPICAM ozone reanalysis. Neither model-ling biases in water vapour or heterogeneous pro- cesses on water ice clouds can explain outstanding differences in total ozone between the SPICAM ozone reanalysis and the control simulation at northern polar latitudes from LS = 150–195°. In this region in particular, investiga-tion of the vertical profiles of water vapour/ice and ozone are needed to try and explain the difference in total ozone between the control simulation and SPICAM ozone reanalysis, and determine whether it is a further unidentified process which is not adequately represented.  Figure 2: (a) Assimilated zonally averaged ozone column at 12 p.m. everywhere and (b) the percentage difference between the SPICAM ozone reanalysis and control simulation for MY 27 and start of MY 28. Shading indicates regions where there are no nearby SPICAM retrievals at the corresponding time and space.  The assimilation of SPICAM retrievals can also provide potential information on the polar maxi-mum, with chemical changes as a result of the assimilation process shown to affect the south-ern polar high altitude ozone layer. For a more realistic study of the polar dynamics, assimila-tion of total ozone, and ideally water vapour too, would provide a more accurate ozone spatial distribution.  In the future, observations from NOMAD [12] on the ExoMars TGO spacecraft, will provide a more comprehensive dataset to assimilate, with the SPICAM observational dataset extremely useful also for cross-validation purposes. Assimilation of vertical profiles of ozone and water vapour/ice alongside column retrievals, such as will be possible from the NOMAD instrument on the ExoMars TGO, will also be of great use to further study the origin of differences in total ozone between the SPICAM ozone reanalysis and global circulation models.  References: [1] Holmes, J. A. et al., Icarus 302, 308-318, 2018. [2] Forget, F. et al., JGR 104, 24155-24175, 1999. [3] Lefèvre, F. et al., JGR 109, E07004, 2004. [4] Newman, C. E. et al., JGR 107, 5123, 2002.  [5] Colaïtis, A. et al., JGR (Planets) 118, 1468-1487, 2013. [6] Navarro, T. et al., JGR (Planets) 119, 1479-1495, 2014. [7] Madeleine, J.-B. et al., JGR (Planets) 116, E11010, 2011. [8] Lefèvre, F. et al., Nature 454, 971-975, 2008. [9] Lorenc, A. C. et al., QJRMS 117, 59-89, 1991. [10] Lewis, S. R. et al., Icarus 192, 327-347, 2007. [11] Perrier, S. et al., JGR 111, E09S06, 2006. [12] Patel, M. R. et al., Appl. Opt. 56 (10), 2771-2782, 2017.  Acknowledgements: All authors acknowledge support as part of the project UPWARDS-633127, funded by the European Union Horizon 2020 Programme. JAH, SRL and MRP also acknowledge the support of the UK Space Agency/STFC. We are grateful for an ongoing collaboration with François Forget and cowork-ers at LMD. 

First ozone reanalysis on Mars using SPICAM data

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