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

Spanish Royal Academy of Sciences

Instituto Nacional deTécnica Aeroespacial

The Spanish Science forthis Mission…

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).

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

1.- SIS: Solar Irradiance Sensor1.- SIS: Solar Irradiance Sensor4.- Eclipsess: Geodesic Studies4.- Eclipsess: Geodesic Studies

Optical Bands detection

Eclipses: Phobos and Deimos

Solar Irradiance

Si photodiodes

4.- Objectives of the Geodesic Studies4.- 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.

3.- MARTIAN MAGNETIC FIELD3.- MARTIAN MAGNETIC FIELD

• Useful data about the magnetic field and about the plasma environment near Mars: Missions Phobos 2Phobos 2 and Mars Global SurveyorMars 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.

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 surface2 – MOURA: A magnetometer for Mars surface

Mars: A magnetic world!

Moment vs. Temperature for different composition of (1-x)Fe3O4 xFe2TiO4

0

20

40

60

80

100

120

140

160

180

10 60 110 160 210 260 310 360

Temperature (K)

Ma

gn

etiz

atio

n (

em

u/c

m3 )

60%

65%

70 %

75%

80%

85%

85 % (2)

90%

95%

100%

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 FIELD3.- MARTIAN MAGNETIC FIELD

5.- Dust Deposited and Dust Airbone Sensor 5.- Dust Deposited and Dust Airbone Sensor

• 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 5.- Dust Deposited and Dust Airbone Sensor

OBJECTIVES

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 xd,yd, zd

MEDIA:Particle size distribution: radius vs.cm-3

Random or specific location (xpn, ypn, zpn)

Origin x0, y0, z0

Volume of interaction

Light Sourcecollimated

beam

FOVDetector size

Operation bands

S11 ()

OUTPUT:Incident power in

each band

Forward Scattering Back Scattering

5.- Dust Deposited and Dust Airbone Sensor 5.- Dust Deposited and Dust Airbone Sensor

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 5.- Dust Deposited and Dust Airbone Sensor

Data retrieval methodologies

0,5 1,0 1,5 2,0 2,5 3,0 3,5 4,0 4,5 5,00,00E+000

5,00E-009

1,00E-008

1,50E-008

2,00E-008

2,50E-008

3,00E-008

Pow

er on d

ete

ctor / s

ourc

e p

ow

er [dm

-1]

Wavelength (m)

30% 4m - 70% 2m 30% 2m - 70% 4m

x5

1E-10 1E-9 1E-8

1E-10

1E-9

1E-8

70% 4m & 30% 2m 70% 2m & 30% 4m

B2 (

3

m -

6

m)

B1 (1,3 m - 2,6 m)

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 5.- Dust Deposited and Dust Airbone Sensor

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.

Besides: Ph.D. Programme and Outreach Activities

‘Terrestrial Environment’ for Martian Studies: Outreach

‘Terrestrial Environment’ for Martian Studies: Outreach

www.rusiahoy.com/blogs/limites-cientificos

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.

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