picam sur mars express putain 10 ans n.
Download
Skip this Video
Loading SlideShow in 5 Seconds..
PICAM sur Mars Express: ( putain ,)10 ans ! PowerPoint Presentation
Download Presentation
PICAM sur Mars Express: ( putain ,)10 ans !

Loading in 2 Seconds...

play fullscreen
1 / 39

PICAM sur Mars Express: ( putain ,)10 ans ! - PowerPoint PPT Presentation


  • 102 Views
  • Uploaded on

PICAM sur Mars Express: ( putain ,)10 ans !. F. Montmessin et l’équipe SPICAM au LATMOS France : LATMOS, LMD, IAS Russia : IKI Belgium : IASB, Univ. Liège U.S .: SwRI , Univ. of Arizona. L’équipe SPICAM.

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about 'PICAM sur Mars Express: ( putain ,)10 ans !' - tudor


An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
picam sur mars express putain 10 ans

PICAM sur Mars Express: (putain,)10 ans !

F. Montmessin et l’équipe SPICAM au LATMOS

France: LATMOS, LMD, IASRussia: IKIBelgium: IASB, Univ. LiègeU.S.: SwRI, Univ. of Arizona

l quipe spicam
L’équipe SPICAM
  • France (LATMOS, LMD, IAS): F. Montmessin (PI), J.-L. Bertaux (ex-PI), A. Reberac, G. Lacombe, N. Chapron, F. Lefèvre, J.-Y. Chaufray, F. Leblanc, F. Forget, S. Lebonnois, E. Quémerais, L. Maltagliati, A. Määttänen, C. Listowski, B. Gondet
  • Russie (IKI) : O. Korablev (CoPI), A. Fedorova, A. Trokhimovsky, A.V. Rodin
  • Belgique(IASB, Univ. de Liège) : A.-C. Vandaele, N. Mateshvili, Y. Willamme, J.-C. Gérard, A. Stiepen, D. Fussen, C. Simon
  • U.S. (LPL): B. Sandel, A. Stern
  • Collaborations: P. Withers, S. Bougher, T. McDunn, N. Schneider, etc.
slide3

SPICAM « light » on Mars Express:4.8 kg

SPICAM on Mars 96: 40 kg

SPICAM UV/Vis étoile (17 kg)

IR AOTF Spectrometer (0.8 kg)

UV Grating Imaging Spectrometer (4 kg)

SPICAM IR solar (23 kg)

sch ma optique
SchémaOptique

UV

IR

Bertaux et al. (JGR,2006)

slide5

Instrument développé au LATMOS (ex-Service d’aéronomie).

  • Le même instrument vole sur la mission ESA Venus Express.
  • Bandespectrale / Résolution:UV: 118-320 nm R=150 IR: 1.0-1.7 µm R=1300
  • Modes d’observation:
  • Occultation (étoile / soleil)
  • Nadir
  • Limbe

IR Spectrometer -800 g-

UV Spectrometer -3 kg-

slide6

Transducer

OUT

Light IN

RF IN

TeO2crystal

slide7

NADIR : l’instrument vise dans la direction du centre de la planète

= mesure du spectre de la lumière solaireréfléchie par la surface et l’atmosphère

  • Colonne d’abondance des constituants CO2, O3, H2O responsables des absorptions observées

Mars Express spacecraft

orbit

Atmosphere

MARS

slide8

LIMBE : L’instrument vise le “bord”dela planète

= mesure du spectre des émissionset diffusion du spectresolaire par l’atmosphère

 Profil vertical en altitude des émissions aéronomiques et des poussières

Mars Express spacecraft

orbit

Atmosphere

MARS

slide9

Spectrum of the star :

outside the atmosphere

through the atmosphere

OCCULTATION : L’instrument vise uneétoileà travers l’atmosphère de la planète

= mesure du spectre de l’étoileà travers et hors atmosphère

 profilsverticaux des constituants responsables des absorptions observées (CO2, O3, O2, CO, H2O, aérosols)

Line of sight

Mars Express spacecraft

star

orbit

Atmosphere

MARS

slide10

Spectre UV (côténuit)

NO δC2  – X2 

NO γA2  + – X2 

H Lyα

Bertaux et al. (Science, 2005)

slide11

O21Dg

Korablev et al. (JGR, 2006)

The oxygen O21Dg emission line at 1.27 mm is produced by UV dissociation of O3

CO2 ice

H2O ice

etat des lieux
Etat des lieux
  • Instrument health:
    • UV channel defects noticed since orbit #2639 = additional “cleaning” stage in the pipeline
    • Further degradation since Safe Mode #25 of Mars Express in summer 2011
    • IR channel has operated flawlessly and continues to do so
  • Data Production:
    • MEx has completed its 10,000th orbit in 2011
    • SPICAM has achieved >10,000 observations and collected 13,500,000 UV spectra and 2,000,000 IR spectra to date
    • 63 Giga-Octets of data transmitted to Earth
  • Science Production:
    • 60 publications
    • JGR special edition (SPICAM results) in 2006
    • >180 communications in workshops/conferences
th mes scientifiques couverts
Thèmesscientifiquescouverts
  • Emissions spontanées de l’atmosphère:
    • NO detection and characterization (UV)
    • Auroras and Dayglows (CO2+, CO, etc.) (UV)
    • Hydrogen and Oxygen corona (UV)
    • O2dayglow/nightglow (IR) (also relevant to 2.)
  • Composition et climat:
    • Ozone, carbon dioxide (temperature) and water vapor mapping and vertical profiling (UV& IR)
    • Aerosols and clouds characterization (UV & IR)
  • Surface(s) :
    • Phobos and Deimos observations (UV)
quelques accomplissements spicamesques
QuelquesaccomplissementsSPICAMesques…..
  • Martian Airglows:
  • First detection of Nitric Oxide emissions, revealing atmospheric global circulation pattern;
  • First detection of auroras above crustal magnetic field anomalies;
  • Characterization of dayglow and nightglow emissions;
  • Characterization of the O and H Martian corona.
  • Atmospheric Composition & Climate
  • Detection of mesospheric (>100 km) cloud layers, of likely CO2 ice origin;
  • First annual mapping of O3, simultaneously with H2O;
  • 4D (x,y,z,t) distribution of O3 and H2O through combination of occultation and nadir modes;
  • Compilation of the largest density/temperature dataset in the mesospheric/thermospheric 70 to 140 km altitude range;
  • Detection of water vapor in a high supersaturation state.
slide15

Spectrum of the star :

outside the atmosphere

through the atmosphere

Atmospheric Transmission

SPICAM Ultra-Violet observations, orbit #17 13 jan. 2004

ratio

Line of sight

Mars Express spacecraft

star

orbit

Atmosphere

MARS

occultation sequence
Occultation sequence

1 spectrum / second z~1-3 km

Prominent signatures of CO2, O3 and aerosols

CO2 profile gives T(z)

Aerosols affect wholespectral range and exhibits a pronounced spectral slope

slide17

Large differences between SPICAM observations and LMD GCM predictions for the mesopause altitude and temperature

  • O underestimated by model = CO2 cooling underestimated

Forget et al. (JGR, 2009)

slide18

Nuagesmésosphériquesmartiens

Montmessin et al.(Icarus, 2006)

slide19

Nuagesmésosphériquesmartiens : de la glace de CO2 ?

Simultaneous temperature profile inversion indicates that layers appear partly inside supersaturated pockets of CO2

slide20

Evolution spatio-temporelle de l’activiténuages/aérosols :

  • Occultationsstellaires/solairesconfondues
  • Suivi de la hauteur max (plafond) des aérosolscorrespondantàuneopacitécolonne le long de la ligne de visée de 1

Ztop

Määttänen et al., Icarus, 2013

slide21

NADIR : l’instrument vise dans la direction du centre de la planète

= mesure du spectre de la lumière solaire réfléchie par la surface de la planète après qu’elle est traversée l’atmosphère

  • comparaison spectre mesuré/spectre solaire : Colonne d’abondance des constituants CO2, O3, H2O responsables des absorptions observées

Mars Express spacecraft

orbit

Atmosphere

MARS

slide22

SPICAM relative albedo

1.4

model with Earth O3/200

model with Earth O3

1.2

1.0

0.8

Relative albedo

0.6

0.4

0.2

0.0

200

220

240

260

280

300

320

wavelength (nm)

CO2

Water vapour band

Observation nadir : principe

UV

MEX/ SPICAM

SPICAM – Ultra-Violet observations, orbit 8, 9 jan. 2004

IR

Absorption

by gas

tv vertical opticalthickness of absorption, varies stronglywithwavelength

θ1

SPICAM – nearInfraredobservations, orbit 8, 9 jan. 2004

Scattering by surface with albedo A

slide25

Multi-annual monitoring of H2O water vapor

H2O, pr.mm

MY27

MY27

MY28

MY28

MY29

MY30

Ls

slide26

Annual water vapor cycle: an average view

H2O pr.mm

All years combined

1 km3

of ice

slide27

Interannualvariability of H2O vapor

H2O, pr.mm

MY27

MY28

MY29

MY30

slide28

Atmospheric Transmission

SPICAM Infrared observations

Line of sight

Mars Express spacecraft

sun

orbit

Atmosphere

slide29

SPICAM data

LMD GCM predictions

north

south

northern spring-summer

Maltagliati et al. (Science, 2011)

slide32

SPICAM data

LMD GCM predictions

north

south

southern spring

Maltagliati et al. (Icarus, 2013)

meeting spicam spicav
Meeting SPICAM/SPICAV

Poros Island (Greece): 28 june to 2 july 2010

slide35

Climate Model results:Water vapor contours (colors) superimposed on circulation pattern

Northern summer

Southern summer

60 km

Aphelion cloud belt formation

at z ~15 km

0.1

50

200

ppm

Montmessin et al., 2004

slide36

On an annual average, the climatic asymmetry favors accumulation/storage of water in the north.

Northern summer

Southern summer

60 km

Aphelion cloud belt formation

at z ~15 km

0.1

50

200

ppm

Montmessin et al., 2004

slide37

Northern summer

Southern summer

60 km

SPICAM

GCM

0.1

50

200

ppm

Montmessin et al., 2004

slide38

Interannualvariability of H2O vapor

H2O, pr.mm

MY27

MY28

MY29

MY30

slide39

Interannualvariability of H2O vapor

H2O, pr.mm

MY27

MY28

MY29

MY30