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Saturn Ring Results from the Cassini Composite Infrared Spectrometer

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Presentation on theme: "Saturn Ring Results from the Cassini Composite Infrared Spectrometer"— Presentation transcript:

1 Saturn Ring Results from the Cassini Composite Infrared Spectrometer
E. Deau1,2, L. J. Spilker1, R. Morishima1,2, C. Ferrari3, Stuart Pilorz4, M. R. Showalter4, S. M. Brooks1, S. G. Edgington1 1NASA Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA, 91109, USA, 2 University of California at Los Angeles, Los Angeles, CA 90095, USA, 3Universite Paris-Diderot, USPC, Paris, FRANCE, 4SETI Institute, Mountain View, CA 94043, USA,

2 Motivation Plateaus Temperatures for large ring structures (dR = 3,000 km) derived earlier in mission Diurnal eclipse, seasons, phase angle effects Temperature-Optical depth (T- ) correlations Thermal behavior of small scale structures (plateaus, halos: dR < 300 km) is not well characterized Use Grand Finale data Very high spatial resolution Do small scale structures thermally behave like large scale structures? C ring Plateaus Mimas 5:3

3 Motivation Plateaus Temperatures for large ring structures (dR = 3,000 km) derived earlier in mission Diurnal eclipse, seasons, phase angle effects Temperature-Optical depth (T- ) correlations Thermal behavior of small scale structures (plateaus, halos: dR < 300 km) is not well characterized Use Ring-Grazing and Grand Finale data Very high spatial resolution Do small scale structures thermally behave like large scale structures? C ring Plateaus Mimas 5:3

4 Composite Infrared Spectrometer (CIRS)
Fourier Transform Spectrometer Wavelength range : FP4 : 7-9 m FP3: 9-17 m FP1: m Spectral Resolution 0.5, 1, 3, 15.5 cm-1 FP1: 3.9 mrad diameter Rings: T~ K ==> Max emission around ~50 microns JPL / August

5 Planck Fits to CIRS Spectra
B A C I I =  * B(Tring)  = ε (1- e-/μ) Wavenumber (cm-1)

6 CIRS spectrogram a = 62º B = 62º B’ = 17º Rs/c = 9 Rs

7 CIRS spectrogram a = 62º B = 62º B’ = 17º Rs/c = 9 Rs spectra

8 a = 62º B = 62º B’ = 17º Rs/c = 9 Rs spectra radial profile CIRS
spectrogram a = 62º B = 62º B’ = 17º Rs/c = 9 Rs spectra radial profile

9 a = 62º B = 62º B’ = 17º Rs/c = 9 Rs CIRS spectrogram Low res Vs.
High res. a = 62º B = 62º B’ = 17º Rs/c = 9 Rs

10 a = 62º B = 71º B’ = 26º Rs/c = 3 Rs CIRS spectrogram Low res Vs.
High res. a = 62º B = 71º B’ = 26º Rs/c = 3 Rs

11 a = 62º B = 71º B’ = 26º Rs/c = 3 Rs Encke Gap Plateaus ER17 CIRS
spectrogram Low res Vs. High res. a = 62º B = 71º B’ = 26º Rs/c = 3 Rs Encke Gap 325 km Plateaus (245 km) ER17 (250 km)

12 a = 62º B = 71º B’ = 26º Rs/c = 3 Rs spectra Encke Gap Plateaus ER17
CIRS spectrogram Low res Vs. High res. a = 62º B = 71º B’ = 26º Rs/c = 3 Rs spectra Encke Gap 325 km Plateaus (245 km) ER17 (250 km)

13 T : Effective temperature (Kelvin) : scaling factor  = ε (1- e-/μ)
CIRS spectrogram Low res Vs. High res. Blackbody fits Blackbody fit ( cm-1): spectra Planck function: Output parameters: T : Effective temperature (Kelvin) : scaling factor  = ε (1- e-/μ)

14 Lit face Unlit face CIRS spectrogram Low res Vs. High res.
Blackbody fits Lit face Unlit face Tiscareno et al. Science under review

15 CIRS spectrogram Low res Vs. High res. Blackbody fits T- correlations
Tiscareno et al. Science under review

16 Lit face CIRS spectrogram Low res Vs. High res. Blackbody fits
T- correlations Spilker et al. 2006 Lit face We now observe the rings with much more detail, compared to the beginning of the mission. In particular on the lit side. Tiscareno et al. Science under review

17 Lit face Unlit face CIRS spectrogram Low res Vs. High res.
Blackbody fits T- correlations Spilker et al. 2006 Lit face Unlit face Tiscareno et al. Science under review

18 Temperature T - Optical depth 
CIRS spectrogram Low res Vs. High res. Blackbody fits T- correlations Spilker et al. 2006 Temperature T - Optical depth  correlations Across ring system (Low- rings Vs High- rings)

19 Temperature T - Optical depth 
CIRS spectrogram Low res Vs. High res. Blackbody fits T- correlations Spilker et al. 2006 Temperature T - Optical depth  correlations Across ring system (Low- rings Vs High- rings) T- correlation Lit Unlit - Low- rings (C & CD) are the warmest

20 Temperature T - Optical depth 
CIRS spectrogram Low res Vs. High res. Blackbody fits T- correlations Spilker et al. 2006 Temperature T - Optical depth  correlations Across ring system (Low- rings Vs High- rings) T- correlation Lit Unlit - For the rings, it’s more than an optical depth effect, the major driver is albedo Low- rings (C & CD) are the warmest Low filling factor and low albedo --> less shadowing and more sunlight is absorbed

21 Temperature T - Optical depth 
CIRS spectrogram Low res Vs. High res. Blackbody fits T- correlations Spilker et al. 2006 Temperature T - Optical depth  correlations Across ring system (Low- rings Vs High- rings) Across a single ring (Low- regions Vs High- regions) T- correlation Lit Unlit - Low- rings (C & CD) are the warmest Low filling factor and low albedo --> less shadowing and more sunlight is absorbed

22 Temperature T - Optical depth 
CIRS spectrogram Low res Vs. High res. Blackbody fits T- correlations Spilker et al. 2006 Temperature T - Optical depth  correlations Across ring system (Low- rings Vs High- rings) Across a single ring (Low- regions Vs High- regions) T- correlation Lit Unlit - T- correlation Lit Unlit + - Low- rings (C & CD) are the warmest Low filling factor and low albedo --> less shadowing and more sunlight is absorbed

23 Temperature T - Optical depth 
CIRS spectrogram Low res Vs. High res. Blackbody fits T- correlations Spilker et al. 2006 Temperature T - Optical depth  correlations Across ring system (Low- rings Vs High- rings) Across a single ring (Low- regions Vs High- regions) T- correlation Lit Unlit - T- correlation Lit Unlit + - Within rings, albedo differences are minimal, whereas optical depth differences are strong Low- rings (C & CD) are the warmest Low filling factor and low albedo --> less shadowing and more sunlight is absorbed High- regions are the warmest on lit face High- regions are the coldest on unlit face

24 Temperature T - Optical depth 
CIRS spectrogram Low res Vs. High res. Blackbody fits T- correlations Spilker et al. 2006 Temperature T - Optical depth  correlations Across ring system (Low- rings Vs High- rings) Across a single ring (Low- regions Vs High- regions) T- correlation Lit Unlit - T- correlation Lit Unlit + - Low- rings (C & CD) are the warmest Low filling factor and low albedo --> less shadowing and more sunlight is absorbed High- regions are the warmest on lit face High- regions are the coldest on unlit face --> sunlight does not penetrate deeply into layer

25 Temperature T - Optical depth 
CIRS spectrogram Low res Vs. High res. Blackbody fits T- correlations Spilker et al. 2006 Temperature T - Optical depth  correlations Across ring system (Low- rings Vs High- rings) Across a single ring (Low- regions Vs High- regions) T- correlation Lit Unlit - T- correlation Lit Unlit + - Low- rings (C & CD) are the warmest Low filling factor and low albedo --> less shadowing and more sunlight is absorbed High- regions are the warmest on lit face High- regions are the coldest on unlit face --> sunlight does not penetrate deeply into layer Still valid for small scale structures ?

26 CIRS spectrogram Low res Vs. High res. Blackbody fits T- correlations
Tiscareno et al. Science under review

27 T- correlation Ring lit unlit C ring plateaus + - CIRS spectrogram
Low res Vs. High res. Blackbody fits T- correlations Tiscareno et al. Science under review T- correlation Ring lit unlit C ring plateaus + -

28 T- correlation Ring lit unlit C ring plateaus + - B ring B ring halo
CIRS spectrogram Low res Vs. High res. Blackbody fits T- correlations Tiscareno et al. Science under review T- correlation Ring lit unlit C ring plateaus + - B ring B ring halo (Janus 2:1) Janus 2:1 96,233 km

29 T- correlation Ring lit unlit C ring plateaus + - B ring B ring halo
CIRS spectrogram Low res Vs. High res. Blackbody fits T- correlations Tiscareno et al. Science under review T- correlation Ring lit unlit C ring plateaus + - B ring B ring halo (Janus 2:1) inner A ring A ring halos (Janus 4:3/5:4/6:5 Mimas 5:3) In the A ring, the signal is noisy on the lit side. On the unlit side, there is a strong correlation with optical depth. Same result is observed in the B ring halo located in the inner part of the ring.

30 T- correlation Ring lit unlit C ring plateaus + - B ring B ring halo
CIRS spectrogram Low res Vs. High res. Blackbody fits T- correlations C-B-A / halo dichotomy Tiscareno et al. Science under review T- correlation Ring lit unlit C ring plateaus + - B ring B ring halo (Janus 2:1) inner A ring A ring halos (Janus 4:3/5:4/6:5 Mimas 5:3) Janus 2:1 96, 247 km

31 A and B rings’ halos seem to not
CIRS spectrogram Low res Vs. High res. Blackbody fits T- correlations C-B-A / halo dichotomy Tiscareno et al. Science under review T- correlation Ring lit unlit C ring plateaus + - B ring B ring halo (Janus 2:1) inner A ring A ring halos (Janus 4:3/5:4/6:5 Mimas 5:3) A and B rings’ halos seem to not thermally behave like large structures (due to halo’s small and dark particles?)

32 Grand Finale results: CIRS spectra resolved small scale structure
spectrogram Low res Vs. High res. Blackbody fits T- correlations C-B-A / halo dichotomy Conclusions Grand Finale results: CIRS spectra resolved small scale structure Effective temperature derived from Planck fits

33 Grand Finale results: CIRS spectra resolved small scale structure
spectrogram Low res Vs. High res. Blackbody fits T- correlations C-B-A / halo dichotomy Conclusions Grand Finale results: CIRS spectra resolved small scale structure Effective temperature derived from Planck fits On unlit side, halos seem to not thermally behave like large scale structures (did CIRS see small and dark particles?) This could be due to small and dark particles in the halo, and could be an albedo effect. Still particles still have to be resolved by CIRS. Maybe CIRS can provide a high limit to small particle’ sizes

34 Next step: comparison with Saturn Orbit Insertion (SOI)
CIRS spectrogram Low res Vs. High res. Blackbody fits T- correlations C-B-A / halo dichotomy Conclusions Grand Finale results: CIRS spectra resolved small scale structure Effective temperature derived from Planck fits On unlit side, halos seem to not thermally behave like large scale structures (did CIRS see small and dark particles?) Next step: comparison with Saturn Orbit Insertion (SOI) CIRS SOI might resolve halo’s core

35 Saturn Ring Observer As part of larger mission to the Saturn system, which might deliver a Titan or Enceladus orbiter, you could add this spacecraft for the rings! Tom Spilker architected mission, Blue beams are thrust from ion engines to hover above rings Red beam is Lidar, send out a light bean and see what is reflected back to get 3D map of layer

36 Supplementary material

37 CIRS Temperature variations with changing solar elevation
B’=-21.3º B’=-14.6º B’=-09.2º B’=-02.7º EQUINOX Temperatures range from solar elevations of 0 to 24 deg. All data taken well outside Saturn’s shadow on the rings, between 6 am and 6 pm. Major temperature variations in a given ring are with phase angle. Lit rings Unlit rings Lit rings Unlit rings

38 Questions?

39

40

41 Outline CIRS: Infrared emission Effective temperatures Future work
Spectrograms Low resolution vs High resolution cubes Blackbody fits Effective temperatures Correlation with t Interpretation Future work Comparison with SOI

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