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SECOND MOSCOW SOLAR SYSTEM SYMPOSIUM (2M-S3) SPACE RESEARCH INSTITUTE (IKI) October 10-14, 2011

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.org. SECOND MOSCOW SOLAR SYSTEM SYMPOSIUM (2M-S3) SPACE RESEARCH INSTITUTE (IKI) October 10-14, 2011.

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SECOND MOSCOW SOLAR SYSTEM SYMPOSIUM (2M-S3) SPACE RESEARCH INSTITUTE (IKI) October 10-14, 2011

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

  2. The Spanish Science for this Mission…

  3. 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).

  4. Main activities in the Spanish Scientific Program of MEIGA-METNET 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

  5. 1.- SIS: Solar Irradiance Sensor 4.- Eclipsess: Geodesic Studies Si photodiodes Optical Bands detection Solar Irradiance Eclipses: Phobos and Deimos

  6. 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.

  7. 3.- MARTIAN MAGNETIC FIELD • Useful 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.

  8. 2 – MOURA: A magnetometer for Mars surface • Based on the AMR technology • (AnisotropicMagnetoResistance) • Previous heritage • Target resolution < 3 nT • Mass in the order of 45 g • Deployement system (tbd) Mars: A magnetic world!

  9. 3.- MARTIAN MAGNETIC FIELD 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.

  10. 5.- Dust Deposited and Dust Airbone Sensor

  11. 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 dm3) 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

  12. 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 5.- Dust Deposited and Dust Airbone Sensor MEDIA: Particle size distribution: radius vs.cm-3 Random or specific location (xpn, ypn, zpn) Illustration of detection principles Volume of interaction Origin x0, y0, z0 Light Source collimated beam S11 (l) Back Scattering Forward Scattering FOV Detector size Operation bands OUTPUT: Incident power in each band Relative position xd,yd, zd

  13. 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. 5.- Dust Deposited and Dust Airbone Sensor Models developed IR source Multispectral MWIR Detector Calibration element SMA linear actuator

  14. 5.- Dust Deposited and Dust Airbone Sensor Data retrieval methodologies Example: results obtained with two different dust distributions: • 70% diameter= 4 mm and 30% diameter= 2 mm • 70% diameter= 2 mm and 30% diameter= 4 mm Scatter plot (100 simulations) Model output Separation of the output of eachdistribution B2 B1

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

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

  17. ‘Terrestrial Environment’for Martian Studies: Outreach

  18. ‘Terrestrial Environment’for Martian Studies: Outreach www.rusiahoy.com/blogs/limites-cientificos

  19. 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.

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

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