1. Scientific Aspects of the MEIGA Payload for MetNet Luis VÁZQUEZ Facultad de Informática Universidad Complutense de Madrid (UCM) lvazquez @fdi.ucm.es / www.meiga-metnet.orgwww.meiga-metnet.org SECOND MOSCOW SOLAR SYSTEM SYMPOSIUM (2M-S3) SPACE RESEARCH INSTITUTE (IKI) October 10-14, 2011 Spanish Royal Academy of Sciences Instituto Nacional de Técnica Aeroespacial

2. The Spanish Science for this Mission…

5. Main activities in the Spanish Scientific Program of MEIGA-METNET 1.- The Modelling and Simulation of the Planetary Boundary Layer on Mars “The TKE budget in the convective Martian planetary boundary layer”. G.M. Martínez, F. Valero and L. Vázquez. “Quarterly Journal of the Royal Meteorological Society (2011) DOI: 10.1002/qj.883. 2.- Solar Irradiation on Martian Surface The objective is the measurement of the Local Radiation Martian Environment in the range 190-1100 nm: Intensity of the ultraviolet (UV) radiation in the Martian surface. The atmospheric opacity due to the Martian dust. Measure of the seasonal asymmetries in the ground Martian radiation. Concentration of Ozone and Water Vapour in the Martian atmosphere. Correlations between the radiation with the temperature, pressure and water on the Martian surface “Retrieval of ultraviolet spectral irradiance from filtered photodiode measurements”. M-P Zorzano, L. Vázquez and S. Jiménez. Inverse Problems 25, 115023, (2009).

6. 3.- Magnetic Studies The magnetic field on the Martian surface has the static components, related to the crustal magnetic field, and the dynamic components associated to the interaction with the solar wind, atmospheric dynamics and induced planetary magnetic effects. For the first time, we will have the opportunity to measure the Martian magnetic field at surface. These data will shed light on the internal structure and composition of the Martian magnetic field. 4.- Geodesic Studies Characterization of the eclipses of Phobos and Deimos. They will be detected through the variations of the flux radiation on the Martian surface. This will provide information about the rotation and orbit of Mars. “Spatial chronogram to detect Phobos eclipses on Mars with the MetNet Precursor Lander” P. Romero, G. Barderas, J.L. Vázquez-Poletti, I.M. Llorente. Planetary and Space Science 59, 1542-1550 (2011). 5.- Martian Dust Studies 6.- Data Mining Besides: Ph.D. Programme and Outreach Activities Main activities in the Spanish Scientific Program of MEIGA-METNET

7. 1.- SIS: Solar Irradiance Sensor 4.- Eclipsess: Geodesic Studies SOLAR IRRADIANCE SENSOR ACQUISITION CHANNELS ChannelWavelengthUsePositionWavelengthUseChannel 1----Background reference Top Surface Side 2 440 / 660 nmDust Optical Depth21 2190 - 1100 nmTotal luminosity reference 700 - 1100 nmIR22 3710 - 730 nmH2OH2O 400 - 700 nmVIS23 4810 - 830 nmH2OH2O 24 5930 - 950 nmH2OH2O Side 3 440 / 660 nmDust Optical Depth25 6759 - 771 nmA Band - O 2 700 - 1100 nmIR26 7315 - 400 nmUVA 400 - 700 nmVIS27 8280 - 315 nmUVB 28 9200 - 280 nmUVC Side 4 440 / 660 nmDust Optical Depth29 10200 - 310 nmHartley Band - O 3 700 - 1100 nmIR30 11300 - 345 nmHuggins Band - O 3 400 - 700 nmVIS31 12440 nmDust Optical Depth 32 13600 nmDust Optical Depth Additional features non opticalTemperature33 14700 - 1100 nmIR non opticalTemperature34 15400 - 700 nmVIS non opticalTemperature35 16245 - 290 nmUV Redundancy non opticalTemperature36 17440 / 660 nmDust Optical Depth Side 1 760 - 1100 nmSolar incidence angle 37 18700 - 1100 nmIR 38 19400 - 700 nmVIS 760 - 1100 nmSolar incidence angle 39 20 40 Optical Bands detection Eclipses: Phobos and Deimos Solar Irradiance Si photodiodes

8. 4.- Objectives of the Geodesic Studies –The Phobos ECLIPSES will be detected through the variations of the flux radiation on the Martian surface. This will provide information about the rotation and orbit of Mars. –Development of a chronogram of eclipses of Phobos and Deimos in the band of latitude ± 5º, and its geometric parametrization in order to determine the position of the landing site. Study of the accuracy by analizing the influence of Phobos's irregular shape, the precision of the light curves, and Mars and Phobos orbits. –Characterization, by using a rotation model, of the core inertia moments and nucleous size from the proper frequencies obtained from the derived polar motion data.

9. 3.- MARTIAN MAGNETIC FIELD Phobos 2 Mars Global SurveyorUseful data about the magnetic field and about the plasma environment near Mars: Missions Phobos 2 and Mars Global Surveyor. The magnetic field on the Martian surface has the static components, related to the crustal magnetic field, and the dynamic components associated to the interaction with the solar wind, atmospheric dynamics and induced planetary magnetic effects. In situ measurements for the first time of the Martian magnetic field at surface. These data will shed light on the internal structure and composition of Mars. Local and global models of the Martian magnetic field.

10. Based on the AMR technology (AnisotropicMagnetoResistance) Previous heritage Target resolution < 3 nT Mass in the order of 45 g Deployement system (tbd) 2 – MOURA: A magnetometer for Mars surface Mars: A magnetic world!

11. Surface magnetic measurements will provide information for the following science objectives Solar wind-atmosphere interactions. Mars magnetosphere properties. Ionosphere. Solar explosive events and Martian environment. Geophysical properties of the landing site (see figure). Correlation of the induction effects and Mars interior. 3.- MARTIAN MAGNETIC FIELD

12. 5.- Dust Deposited and Dust Airbone Sensor

13. Study of the Martian airborne dust Determination of the local particles distribution Data correlation with other meteorological factors Airborne dust influence in the heat transfer of the Martian Atmosphere Research in new measurements methodologies with multispectral IR sensors Local scattering computational models Data retrieval algorithms based on multiespectral data Implementation of these methodologies in low mass (<40 g.), low volume (<0,5 dm 3 ) and low power consumption (<1W) sensors, according with Project constraints Multiespectral sensor with no-moving parts (integrated IR filters) New Shape Memory Alloy (SMA) devices as actuators 5.- Dust Deposited and Dust Airbone Sensor OBJECTIVES

14. A specific computational model have been developed based on scattering properties of Martian particles. By means of this model and other engendering model (physical) a data retrieval procedures are under developing Illustration of detection principles Relative position x d,y d, z d MEDIA: Particle size distribution: radius vs.cm -3 Random or specific location (x pn, y pn, z pn ) Origin x 0, y 0, z 0 Volume of interaction Light Source collimated beam FOV Detector size Operation bands S 11 ( ) OUTPUT: Incident power in each band Forward Scattering Back Scattering 5.- Dust Deposited and Dust Airbone Sensor

15. Different engineering and qualified models have been developed in collaboration with Spanish company Arquimea in order to validate the detection principles and the technology. Flight Model to be fabricated by October 2011. Models developed IR source Multispectral MWIR Detector Calibration element SMA linear actuator 5.- Dust Deposited and Dust Airbone Sensor

16. Data retrieval methodologies Model output Scatter plot (100 simulations) B1 B2 Example: results obtained with two different dust distributions: 1.70% diameter= 4  m and 30% diameter= 2  m 2.70% diameter= 2  m and 30% diameter= 4  m Separation of the output of each distribution 5.- Dust Deposited and Dust Airbone Sensor

17. Besides: Ph.D. Programme and Outreach Activities

18. “Mars as a Service: Cloud Computing for the Red Planet Exploration Era”. José Luis Vázquez-Poletti. HPC in the Cloud, February 7 th, 2011. Besides: Ph.D. Programme and Outreach Activities

19. ‘Terrestrial Environment’ for Martian Studies: Outreach

20. www.rusiahoy.com/blogs/limites-cientificos

21. POSSIBLE FUTURE COLABORATION The Russia-Finish-Spanish collaboration within MetNet programme should be boosted. To develop jointly scientific instrumentation for Planetary Exploration Common Integration and tests of scientific payloads. Organization of a series of Joint Summer Space Schools. Interchange of students in the framework of a Space Programme.

22. Cпасибо! ¡Muchas gracias! Thank you!...