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Cassini-Huygens Mission to Saturn
Overview




                                    QuickTime™ and a
                          TIFF (Uncompressed) decompressor
                             are needed to see this picture.
JPL Overview
NASA’s Jet Propulsion Laboratory,
   managed by the California Institute
   of Technology, is the world leader in
   robotic exploration of the solar
   system.




http://photojournal.jpl.nasa.gov
Mission Overview
Huygens and Cassini
                The Scientists and the Machines




                      Giovanni Domenico Cassini
Christiaan Huygens
                      (1625-1712), Italo-French
(1629-1695) Dutch
                      astronomer, who discovered
scientist, who
                      several of Saturn’s satellites:
discovered the true
                      Iapetus, Rhea, Tethys and
nature of Saturn’s
                      Dione. In 1675, he
rings, and in 1655,
                      discovered what is today
Titan
                      called “Cassini Division” the
                      gap in-between the two
                      main rings of Saturn
Cassini Orbiter & Huygens Probe
Launched on October
                                  15, 1997 from KSC
       QuickTime™ and a
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                                  7 year cruise on
are needed to see this picture.
                                  VVEJGA trajectory
Cassini Spacecraft


Cassini Spacecraft Specs
• Height: 6.8 m (22 ft)
• Diameter: 4 m (13 ft)
• Mass: 2125 kg (2.8 tons)
  (fueled+probe): 5700 kg (6
  tons)
• Power: 700 Watts at SOI
• .5 GB recorder
• Huygens Probe:
  320 kg (~700 lbs)

Cassini Instruments:
                                                 Magnetospherie and Plasma Science (MAPS)
Optical Remote Sensing (ORS)
                                                 CDA: Cosmic Dust Analyzer
CIRS: Composite Infrared Spectrometer
                                                 INMS: Ion and Neutral Mass Spectrometer
ISS: Imaging Science Subsystem
                                                 MAG: Dual Technique Magnetometer
UVIS: Ultraviolet Imaging Spectrograph
                                                 MIMI: Magnetospheric Imaging Instrument
VIMS: Visual and Infrared mapping Spectrometer
                                                 RPWS: Radio and Plasma Wave Science
Microwave Remote Sensing
RADAR: Cassini Radar
RSS: Radio Science Subsystem
Cassini-Huygens Mission to Saturn Overview
Cost
• Cassini total cost $3 billion
   – $2.5 B NASA for Cassini, $0.5 B ESA for Huygens
   – Spread over ~20 y -> $150 M/y
   – Cassini 0.5% of NASA annual budget ($16.8 B)

• NASA annual budget $16.8 B
   – 1.7% of U.S. discretionary spending ($982 B)
   – 0.6% total U.S. budget ($2800 B)
Cassini-Huygens Mission to Saturn Overview
Tour Overview
                       4 year Prime Mission
                       – 75 orbits
                       – 45 targeted Titan flybys
                       – 8 targeted icy satellite flybys




5 Science Objectives
                                 QuickTime™ and a
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    Titan
–                         are needed to see this picture.



    Saturn
–
    Rings
–
    Icy Satellites
–
    Magnetosphere
–
                                                        Tour (Petal) movie
#1: Huygens on Titan
Why Titan?
• Diameter – 5150km; larger than Mercury and Pluto
• Only planetary satellite with a dense atmosphere
• Surface: P: 1.5 X Earth’s; T: 94 K (-179 C)
• Composition – Nitrogen (N2); Methane (CH4) and
  rich array of hydrocarbons (CxHx) and nitriles
  (HCN)
• Surface – obscured by photochemical haze
• Murky atmosphere may be similar to that which
  existed on Earth before life formed.
• Most Earth-like body in the solar system: rivers,
  lakes, seas, mountains, dunes, channels, winds,
  volcanos, thick atmosphere - chemically complex
Huygens Separation & Entry
Release: December 24, 2004
Decent: January 14, 2005
Data Collection:
     •Decent: 2h 27m
     •Surface: 1h 12m
     •Radiometric: 5h 52m
                                        QuickTime™ and a
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The Huygens
  Descent



         QuickTime™ and a
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The Surface of Titan
Arial view of Titan
Huygens “News”
#2: Enceladus
Cassini-Huygens Mission to Saturn Overview
National Geographic, 1981
Slide 22
Cassini-Huygens Mission to Saturn Overview
Enceladus, July 14, 2005




                       175 km flyby!!
Cassini-Huygens Mission to Saturn Overview
Two UVIS stellar occultations. The one in July identified a
local atmosphere around the south pole.
Cassini-Huygens Mission to Saturn Overview
Enceladus Flyby: 12 November
            2005
GEYSER COMPOSITION
 (Waite et al. 2006; Hansen et al., 2006)




       H2O                                           91 ± 3 % wt.
        2

       CO 2                                           3.2 ± 0.6 % wt.
       N2                                             4 ± 1 % wt.*
        2
       CH4                                            1.6 ± 0.4 % wt.
         4
       CO                                              < 0.9 % wt
                                        (i.e.,
                                        (i.e.,
       NH3, HCN, C2H2, C3H8 < 0.5 % wt. (i.e., detected)
         3        22    38



        *Inferred from a combination of INMS and UVIS data
Why the South Pole?
  Nimmo and Pappalardo (2006)
  • Low-density silicate or ice
    diapir can be sufficient to
    overcome the equatorial
    bulge and reorient Enceladus
  • Resulting stresses may be
    consistent with the observed
    tectonic patterns
  • Few mgal gravity anomaly: might
    be detectable by Cassini?




Slide 30
Planetary Heat Flow
                                Enceladus
              Avg Earth         South Polar Terrain
              87 mW/m2          250 mW/m2




                          Tiger Stripes
Yellowstone
                          13,000 mW/m2
2500 mW/m2
Cassini-Huygens Mission to Saturn Overview
Cassini-Huygens Mission to Saturn Overview
“Mimas Paradox”




NASA/JPL/SSI

                       Mimas     Enceladus
                                             Bistable tidal heating?
Diameter               420 km    504 km          • Enceladus is warm,
                                                 dissipative, stays warm.
Density                1.2       1.6
                                                 • Mimas is cold, rigid, stays
Distance from Saturn   3.1 RS    3.9 RS
                                                 cold.
Orbital Eccentricity   0.0206    0.0047
                                             Need a way to “kick start”
Tidal heating, solid             16 MW
                       160 MW                Enceladus initially
ice rigidity, Q = 20
Slide 34
#3: Titan from Space
Cassini-Huygens Mission to Saturn Overview
Titan: the most Earth-like body in the Solar System
detached haze                           mid-latitude streaks



                                                                       drainage
                                                                        channels

                huge cloud system                 mountains
                                                                       river channels




                wind driven dunes


                     aeolian patterns
                                                               lakes
      few craters
ISS map
          Titan @ 938 nm
VIMS map (r = 5 µm; g = 2 µm; b = 1.6 µm)
RADAR map (TA-T30)
87°W 20°N
                                            Impact basin (above) is
                                100 km      about 450 km in diameter
                                            Impact crater (left) is
                                            about 80 km in diameter



                                16°W 11°N
                                                 Impact Craters




Cryovolcano and surface flows
Cat Scratches” = Dunes?



                                       Longitudinal Dunes
                                       Arabian Peninsula




Dunes probably consist of wind-blown
hydrocarbon particles
Wispy terrain to east of Shikoku
Lucky                        (Great Britain) resembles dunes
                                seen in earlier SAR data
Number 13

 Circular feature
Guabonito may not
  be an impact
  crater after all
                                                     This complex area of hilly terrain and
                                                      erosional channels is located atop
                                                     Xanadu, the continent-sized region



                 QuickTime™ and a
         Sorenson Video 3 decompressor
          are needed to see this picture.
A Titan Lake?




Cassini had seen several “suspiciously
        lacustrine features”…
…until finally Cassini found the Titan
      equivalent of Minnesota.
Cassini-Huygens Mission to Saturn Overview
Titan's Atmospheric Variability
                                                             mid-latitude streaks
                                         Seasonal
 detached haze
                                         changes in
 150 km higher
                                         weather
 than observed
                                         patterns
   by Voyager




                                             South-polar convective clouds




    VIMS images of mid-latitude clouds




                                                    complex, variable haze structure
What Would the INMS Measure in Other
              Ionospheres?




We have discovered that Titan has the most chemically complex
ionosphere in the solar system. There are likely strong
connections to neutral chemistry; these are still being explored.
Cassini-Huygens Mission to Saturn Overview
#4: Saturn Orbit Insertion
         and the
Rev 28 occultation Images
SOI Trajectory
Saturn Orbit Insertion Ring Plane Crossing




                                 QuickTime™ and a
                         Sorenson Video 3 decompressor
                    X     are needed to see this picture.
Approach picture from
                                             Cassini:
                                             May 10, 2004
                                F
                                             Dist: 27 million km.
                                             Pixel: 161 km.
                                             Moon: Prometheus
                       A
C   B


                                             Cassini ISS image: Space
                                             Science Institute (Boulder),
                                             NASA/JPL.




                       Encke Gap
                       W~350 km
                            The main rings
    Cassini Division
Complex Rings




                      QuickTime™ and a
            TIFF (Uncompressed) decompressor
               are needed to see this picture.
Cassini-Huygens Mission to Saturn Overview
Rev 28 Occultation
For the first time, we can see all the rings clearly in a single image!

                                    D-Ring
E-Ring                   Cassini
         G-Ring
                  F-Ring Division




                  A-Ring
                           B-Ring C-Ring




   There is a lot going
   on in this image, so
   let’s take a closer
   look….



                                             No need for these artist’s renditions anymore.
Out here, we
                see the light
                scattered by
                the rings




     A CD      B                D
                         C                 On the planet,
                                           we see the light
                                           blocked by the
                                           rings
                                       C

                                           B
                                               CD
                                                    A


The non-trivial relationship between
brightness and amount of material
leads to strange images….
Cassini-Huygens Mission to Saturn Overview
Cassini-Huygens Mission to Saturn Overview
Come join us! http://saturn.jpl.nasa.gov

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Cassini-Huygens Mission to Saturn Overview

  • 1. Cassini-Huygens Mission to Saturn Overview QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture.
  • 3. NASA’s Jet Propulsion Laboratory, managed by the California Institute of Technology, is the world leader in robotic exploration of the solar system. http://photojournal.jpl.nasa.gov
  • 5. Huygens and Cassini The Scientists and the Machines Giovanni Domenico Cassini Christiaan Huygens (1625-1712), Italo-French (1629-1695) Dutch astronomer, who discovered scientist, who several of Saturn’s satellites: discovered the true Iapetus, Rhea, Tethys and nature of Saturn’s Dione. In 1675, he rings, and in 1655, discovered what is today Titan called “Cassini Division” the gap in-between the two main rings of Saturn
  • 6. Cassini Orbiter & Huygens Probe
  • 7. Launched on October 15, 1997 from KSC QuickTime™ and a YUV420 codec decompressor 7 year cruise on are needed to see this picture. VVEJGA trajectory
  • 8. Cassini Spacecraft Cassini Spacecraft Specs • Height: 6.8 m (22 ft) • Diameter: 4 m (13 ft) • Mass: 2125 kg (2.8 tons) (fueled+probe): 5700 kg (6 tons) • Power: 700 Watts at SOI • .5 GB recorder • Huygens Probe: 320 kg (~700 lbs) Cassini Instruments: Magnetospherie and Plasma Science (MAPS) Optical Remote Sensing (ORS) CDA: Cosmic Dust Analyzer CIRS: Composite Infrared Spectrometer INMS: Ion and Neutral Mass Spectrometer ISS: Imaging Science Subsystem MAG: Dual Technique Magnetometer UVIS: Ultraviolet Imaging Spectrograph MIMI: Magnetospheric Imaging Instrument VIMS: Visual and Infrared mapping Spectrometer RPWS: Radio and Plasma Wave Science Microwave Remote Sensing RADAR: Cassini Radar RSS: Radio Science Subsystem
  • 10. Cost • Cassini total cost $3 billion – $2.5 B NASA for Cassini, $0.5 B ESA for Huygens – Spread over ~20 y -> $150 M/y – Cassini 0.5% of NASA annual budget ($16.8 B) • NASA annual budget $16.8 B – 1.7% of U.S. discretionary spending ($982 B) – 0.6% total U.S. budget ($2800 B)
  • 12. Tour Overview 4 year Prime Mission – 75 orbits – 45 targeted Titan flybys – 8 targeted icy satellite flybys 5 Science Objectives QuickTime™ and a Animation decompressor Titan – are needed to see this picture. Saturn – Rings – Icy Satellites – Magnetosphere – Tour (Petal) movie
  • 14. Why Titan? • Diameter – 5150km; larger than Mercury and Pluto • Only planetary satellite with a dense atmosphere • Surface: P: 1.5 X Earth’s; T: 94 K (-179 C) • Composition – Nitrogen (N2); Methane (CH4) and rich array of hydrocarbons (CxHx) and nitriles (HCN) • Surface – obscured by photochemical haze • Murky atmosphere may be similar to that which existed on Earth before life formed. • Most Earth-like body in the solar system: rivers, lakes, seas, mountains, dunes, channels, winds, volcanos, thick atmosphere - chemically complex
  • 15. Huygens Separation & Entry Release: December 24, 2004 Decent: January 14, 2005 Data Collection: •Decent: 2h 27m •Surface: 1h 12m •Radiometric: 5h 52m QuickTime™ and a MPEG-4 Video decompressor are needed to see this picture.
  • 16. The Huygens Descent QuickTime™ and a Sorenson Video 3 decompressor are needed to see this picture.
  • 24. Enceladus, July 14, 2005 175 km flyby!!
  • 26. Two UVIS stellar occultations. The one in July identified a local atmosphere around the south pole.
  • 28. Enceladus Flyby: 12 November 2005
  • 29. GEYSER COMPOSITION (Waite et al. 2006; Hansen et al., 2006) H2O 91 ± 3 % wt. 2 CO 2 3.2 ± 0.6 % wt. N2 4 ± 1 % wt.* 2 CH4 1.6 ± 0.4 % wt. 4 CO < 0.9 % wt (i.e., (i.e., NH3, HCN, C2H2, C3H8 < 0.5 % wt. (i.e., detected) 3 22 38 *Inferred from a combination of INMS and UVIS data
  • 30. Why the South Pole? Nimmo and Pappalardo (2006) • Low-density silicate or ice diapir can be sufficient to overcome the equatorial bulge and reorient Enceladus • Resulting stresses may be consistent with the observed tectonic patterns • Few mgal gravity anomaly: might be detectable by Cassini? Slide 30
  • 31. Planetary Heat Flow Enceladus Avg Earth South Polar Terrain 87 mW/m2 250 mW/m2 Tiger Stripes Yellowstone 13,000 mW/m2 2500 mW/m2
  • 34. “Mimas Paradox” NASA/JPL/SSI Mimas Enceladus Bistable tidal heating? Diameter 420 km 504 km • Enceladus is warm, dissipative, stays warm. Density 1.2 1.6 • Mimas is cold, rigid, stays Distance from Saturn 3.1 RS 3.9 RS cold. Orbital Eccentricity 0.0206 0.0047 Need a way to “kick start” Tidal heating, solid 16 MW 160 MW Enceladus initially ice rigidity, Q = 20 Slide 34
  • 37. Titan: the most Earth-like body in the Solar System detached haze mid-latitude streaks drainage channels huge cloud system mountains river channels wind driven dunes aeolian patterns lakes few craters
  • 38. ISS map Titan @ 938 nm
  • 39. VIMS map (r = 5 µm; g = 2 µm; b = 1.6 µm)
  • 41. 87°W 20°N Impact basin (above) is 100 km about 450 km in diameter Impact crater (left) is about 80 km in diameter 16°W 11°N Impact Craters Cryovolcano and surface flows
  • 42. Cat Scratches” = Dunes? Longitudinal Dunes Arabian Peninsula Dunes probably consist of wind-blown hydrocarbon particles
  • 43. Wispy terrain to east of Shikoku Lucky (Great Britain) resembles dunes seen in earlier SAR data Number 13 Circular feature Guabonito may not be an impact crater after all This complex area of hilly terrain and erosional channels is located atop Xanadu, the continent-sized region QuickTime™ and a Sorenson Video 3 decompressor are needed to see this picture.
  • 44. A Titan Lake? Cassini had seen several “suspiciously lacustrine features”…
  • 45. …until finally Cassini found the Titan equivalent of Minnesota.
  • 47. Titan's Atmospheric Variability mid-latitude streaks Seasonal detached haze changes in 150 km higher weather than observed patterns by Voyager South-polar convective clouds VIMS images of mid-latitude clouds complex, variable haze structure
  • 48. What Would the INMS Measure in Other Ionospheres? We have discovered that Titan has the most chemically complex ionosphere in the solar system. There are likely strong connections to neutral chemistry; these are still being explored.
  • 50. #4: Saturn Orbit Insertion and the Rev 28 occultation Images
  • 52. Saturn Orbit Insertion Ring Plane Crossing QuickTime™ and a Sorenson Video 3 decompressor X are needed to see this picture.
  • 53. Approach picture from Cassini: May 10, 2004 F Dist: 27 million km. Pixel: 161 km. Moon: Prometheus A C B Cassini ISS image: Space Science Institute (Boulder), NASA/JPL. Encke Gap W~350 km The main rings Cassini Division
  • 54. Complex Rings QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture.
  • 57. For the first time, we can see all the rings clearly in a single image! D-Ring E-Ring Cassini G-Ring F-Ring Division A-Ring B-Ring C-Ring There is a lot going on in this image, so let’s take a closer look…. No need for these artist’s renditions anymore.
  • 58. Out here, we see the light scattered by the rings A CD B D C On the planet, we see the light blocked by the rings C B CD A The non-trivial relationship between brightness and amount of material leads to strange images….
  • 61. Come join us! http://saturn.jpl.nasa.gov