the new horizons mission to pluto and the kuiper belt leslie young new horizons deputy project...
TRANSCRIPT
The New Horizons mission to Pluto and the Kuiper Belt
Leslie Young
New Horizons Deputy Project Scientist
303-546-6057 (USA)
Janvier 12 2006Workshop 3e zone Slide 2
Pluto, Charon, Nix, and Hydraas seen from HST
Janvier 12 2006Workshop 3e zone Slide 3
Pluto, Charon, Nix, and Hydraas seen in the Louvre
Janvier 12 2006Workshop 3e zone Slide 4
New Horizons trajectory
Pluto-Charon14 July 2015
KBOs2016-2020
Jupiter System28 Feb 2007
Launch19 Jan 2006
Janvier 12 2006Workshop 3e zone Slide 5
Instrument Payload
SWAPSolar wind analyzer
PEPSSIEnergetic particle detector
LORRILong-rangevisible imager
Ralphvisible pan. and color imager, IR spectrometer
AliceUV imagingspectrometer
REXRadio science & radiometry
Star TrackersGuidance and control
+Y
+X
+Z
SDCStudent dust counter(under spacecraft)
Janvier 12 2006Workshop 3e zone Slide 6
New Horizons Remote Sensing Instrument Fields of View (-X)
Janvier 12 2006Workshop 3e zone Slide 7
Ralph/LEISA (Linear Etalon Imaging Spectral Array)Infrared imaging spectrometer
256 x 256 pix, 64 microradian/pixel
2.10-2.25 µm, R≈560
1.25-2.50 µm, R≈240
scanned to form 256 x 256 x n spectral image cube4444-4762 cm-1
4000-8000 cm-1
40008000 wavenumber (cm-1)
Janvier 12 2006Workshop 3e zone Slide 8
Ralph/LEISA (Linear Etalon Imaging Spectral Array)Infrared Imaging Spectrometer
256 x 256 pix, 64 microradian/pixel
2.10-2.25 µm, R≈560
1.25-2.50 µm, R≈240
scanned to form 256 x 256 x n spectral image cube
Janvier 12 2006Workshop 3e zone Slide 9
Ralph/MVIC (Multi-spectral Visible Imaging Camera) Four Color Time Delay Integration (TDI)
780-975 nm860-910 nm
400-550 nm540-700 nm
5000 pix, 20 microradian/pixel
scanned to formfour 5000 x n images
Janvier 12 2006Workshop 3e zone Slide 10
Ralph/MVIC (Multi-spectral Visible Imaging Camera) Panchromatic Time Delay Integration (TDI)
400-975 nm
5000 pix, 20 microradian/pixel
scanned to form 5000 x N image
Janvier 12 2006Workshop 3e zone Slide 11
Ralph/MVIC (Multi-spectral Visible Imaging Camera) Panchromatic Framing Array
400-975 nm
5000 pix, 20 microradian/pixel
128 pix,20 microradian/pixel
5 km
0.6 km/pix
Janvier 12 2006Workshop 3e zone Slide 12
LORRI (LOng Range Reconnaissance Imager)High-resolution Imager
1024 x 1024 pix, 5 microradian/pixel
400-975 nm
0.6 km/pix
0.1 km/pix
Janvier 12 2006Workshop 3e zone Slide 13
Alice Ultraviolet Long-slit Spectrometer
465-1881 Å
"Box""Slot""
32 pix (30 active), 0.27°/pixel
1024 pix (780 active), 1.8 Å/pixel
46.5-118.1 nm.
FWHM = 2.7-3.5 Å (point source), 172 Å (filled slit)
465-1181 Å.
FWHM = 3-4.5 Å (point source), 9 Å (filled slit)
Pluto's EUV/FUV Line-of-sight Atmospheric Opacity
Wavelength (nm)60 180Wavelength (nm)60 180
Alti
tde
(km
)
0
2000
10-4
104
Pluto Airglow Brightness SNR Model
Mod
el B
right
ness
(R
)
10-3
104
Janvier 12 2006Workshop 3e zone Slide 14
January 19, 2006On our way!
Janvier 12 2006Workshop 3e zone Slide 15
New Horizons in Flight Ralph/MVIC Imager and IR Spectrograph
Ralph pan frameImage of M7: The oddly shaped “blobs” (in rectangles) are energetic particle hits.
Digitized Sky Surveyimage of same field:
Janvier 12 2006Workshop 3e zone Slide 16
New Horizons in FlightAlice UV Spectrometer
Sky background showing Lyman-, the shape of the box and slot, the decrease in flux in the middle of the photocathode gap from 2006 Aug 31.
Janvier 12 2006Workshop 3e zone Slide 17
New Horizons in Flight REX Radio Science
1.2° full width between 3 dB points
Mapping out the High Gain Antenna (HGA)
Janvier 12 2006Workshop 3e zone Slide 18
New Horizons in Flight LORRI High Resolution Imager
Janvier 12 2006Workshop 3e zone Slide 19
New Horizons in Flight SWAP Solar Wind Analyzer
• Solar wind speed, temperature and density variations observed.• Three instrument cycles are required for the solar wind to be observed at each energy step.
This gives the appearance of the solar wind flux changing over 3 cycles.
Speed Changes
Day of Year (Oct 17 - Nov 17)
• Compression & or Shock
• Increase in temperature, velocity, & number density
Janvier 12 2006Workshop 3e zone Slide 20
New Horizons in FlightPEPSSI Energetic Particle Detector
Cou
nts/
bin
(log)
1
10
Very good Alpha / proton separationdown to 20 keVDOY 172 (June 21) – 2000V
Janvier 12 2006Workshop 3e zone Slide 21
New Horizons in FlightSDC Student Dust Counter
July 14 - August 16
Janvier 12 2006Workshop 3e zone Slide 22
New Horizons Jupiter Gravity Assist
• Achieve the Pluto JGA• Serve as practice for Pluto-system encounter• Do good Jupiter science - Jovian meteorology, satellite
geology and composition, auroral phenomena, and magnetospheric physics
Jupiter closest approach
2007 February 28
31 Jupiter radii
Press conference
2007 January 18
PEPSSI, LORRI (Jupiter), LEISA (Callisto), ...
Janvier 12 2006Workshop 3e zone Slide 23
New Horizons at Jupiter: Jupiter Meteorology and Aurorae
• NIR image cubes of storm activity near the GRS• Hi-res imaging of the Little Red Spot• Global imaging of atmospheric circulation• UV stellar occultation• UV, NIR scans of polar aurorae and airglow
Janvier 12 2006Workshop 3e zone Slide 24
New Horizons at Jupiter:Galilean Satellites
• Visible and NIR imaging of high-temperature volcanic thermal emission on Io
• Mapping plumes and surface changes on Io
• Mapping global topography on Europa• UV stellar occultations and auroral
emission studies of satellite atmospheres
• NIR mapping of surface composition
LORRI
MVICLEISA
New Horizons view of Io at closest approachIo atmosphere
stellar occultation signature
Janvier 12 2006Workshop 3e zone Slide 25
New Horizons at Jupiter:Rings and Small Satellites
• Search for small satellites embedded in the rings
• Map ring vertical structure during ring-plane crossing
• Map spatial distribution of “gossamer” rings
• Determine ring particle phase function
• Phase function for outer satellites Himalia, Elara
Janvier 12 2006Workshop 3e zone Slide 26
New Horizons at Jupiter:Magnetosphere
• Fly down the magnetotail for the first time– Investigate plasma loss mechanisms
• In-situ plasma measurements in the middle magnetosphere• Solar wind observations on approach to complement Earth-based auroral
observations• High-resolution imaging spectroscopy of the Io plasma torus
Janvier 12 2006Workshop 3e zone Slide 27
New Horizons at Jupiter:Education/Public Outreach Imaging
• Imaging of selected scenic alignments between bodies in the Jupiter system
Janvier 12 2006Workshop 3e zone Slide 28
New Horizons at PlutoClosest Approach 2015 July 14
• S/C trajectory time ticks: 10 min• Charon orbit time ticks: 12 hr• Occultation: center time• Position and lighting at Pluto
C/A• Distance relative to body center
Pluto
Charon
0.24°
SunEarth
12:40
13:40
11:40
Pluto C/A11:59:0011,095 km13.77 km/s
Charon C/A12:12:5226,937 km13.87 km/s
Pluto-Sun Occultation12:49:00
Pluto-Earth Occultation12:49:50
Charon-Sun Occultation14:15:41
Charon-Earth Occultation14:17:50
Janvier 12 2006Workshop 3e zone Slide 29
New Horizons at Pluto:Geology and Geomorphology
Young et al 1999
Young et al 2001• Hemispheric panchromatic maps (<0.5 km/pixel)
• Hemispheric color maps (<5 km/pixel) • Phase integrals (moderate and high phase angles)• Topography (stereo imaging, photoclimometry)• High-resolution terminator images• Bolometric Bond albedos (normal reflectance and
photometric phase functions)
Janvier 12 2006Workshop 3e zone Slide 30
New Horizons at Pluto:Geology and Geomorphology
• Hemispheric panchromatic maps– Encounter hemispheres of Pluto (MVIC) and Charon (MVIC, LORRI) at 0.5 km/pix– Maps of Pluto and Charon at 12-hour intervals from 6 days out at 36 km/pix (LORRI)– Nightside maps of Pluto in reflected Charon-light. 0.4 km/pix (MVIC), resolution depends on SNR
• Hemispheric color maps (<5 km/pixel)– Redundant four-color maps of Pluto at 0.7 km/pix, of Charon at 1.4 km/pix (MVIC)– Maps of Pluto and Charon at 12-hour intervals from 6 days out at 144 km/pix (MVIC)
• Phase integrals (moderate and high phase angles)– Phase studies during cruise and approach, 5-15 deg– Pluto at 9 phases 16-161° (attempt at 170°). Charon at 6 phases 18-104°.
• Topography (stereo imaging, photoclimometry)– <1 km heights (at baselines of > 1000 km). <5 km heights (at baselines < 250 km)
• High-resolution terminator images– Pluto: 6-10 images 38x1500 km at 0.30 km/pix (MVIC),
6-10 72x72 km images at 0.07 km/pix (LORRI).– Charon: entire hemisphere at 0.52 km/pix (MVIC), – 2-8 143x143 km images at 0.14 km/pix (LORRI).
• Bolometric Bond albedos (normal reflectance and photometric phase functions)– Same dataset as phase integrals
Janvier 12 2006Workshop 3e zone Slide 31
New Horizons at Pluto:Surface Composition
• Hemispheric infrared spectra (1.25-2.5 micron)
• Spatial distribution of N2, CO, CH4
• Presence of other volatiles, hydrocarbons, or minerals• High spatial resolution spectral images• Map surface temperatures
wavelength (micron)1.5
1995
1998
2.5
Douté et al 1999
N2
CH4
CO
Grundy and Buie 2001
2.0
Geo
met
ric A
lbed
o
0.0
0.8
1 nbar
1 μbar
1 mbar
32 36 40 44 48 52 56 60
Equilibrium Vapor Pressure of Pure Ice
Frost Temperature
N2
CO
CH4
Janvier 12 2006Workshop 3e zone Slide 32
• Hemispheric infrared spectra (1.25-2.5 micron) – "Far-side" maps at < 446 km/pixel (LEISA) at /D ≈ 240 (1.25-2.50 µm) and /D ≈ 550 (2.10-2.25 µm)
– Pluto: two maps of approach hemisphere, at 6 and 10 km/pixel (LEISA)
– Charon: two maps of approach hemisphere, at 5 and 10 km/pixel (LEISA)
• Spatial distribution of N2, CO, CH4
– Pure N2 at 2.15 µm, and N2:CH4 from shifts in CH4 bands at e.g., 2.2 µm
– CH4, CH4:N2, or N2:CH4 at many weak and strong bands throughout Pluto's spectrum
– CO at 1.58 and 2.25 µm
• Presence of other volatiles, hydrocarbons, or minerals– H2O at e.g., 2.0 µm. Crystalline form at 1.65 µm
– NH3 or NH3 hydrate at 2.2 µm
– CO2 at 1.96 µm
– C2H6 at 1.68, 2.33 µm. C2H2 at 2.45 µm, C2H4 at 2.22, 2.26 µm, CH3OH at 2.28 µm
– SO2 at 2.13 µm, H2S at 1.64 µm, HCN at 1.91 µm, HC3N at 1.83 µm
– Pyroxene at 1.79-2.33 µm, kaolinite-serpentine clays at 1.40 µm, Al-bearing phyllosilicates at 2.115 µm
• High spatial resolution spectral images– Pluto: 824 x 333 km scan at 1.3 km/pixel
– Charon: 1033 x 486 km scan at 1.9 km/pixel
– Color (0.89 µm CH4 band) maps of Pluto at 0.7 km/pix, of Charon at 1.4 km/pix, and far-side at 144 km/pix (MVIC)
• Map surface temperatures– Average temperature to 0.1 K at 1340 km or hemispheric averaged resolution (REX, radiometry at 4.2 cm emission)
– N2 temperature to 2.0 K at 56 km resolution (LEISA, Grundy, Schmitt and Quirico 1993, Tryka, Brown and Anicich 1995)
– Crystalline H2O temperature to 5 K at 40 km resolution (LEISA, Grundy et al. 1999)
– Pure CH4 temperature to 6 K at 96 km resolution (LEISA, Grundy Schmitt and Quirico 2002)
New Horizons at Pluto:Surface Composition
Janvier 12 2006Workshop 3e zone Slide 33
New Horizons at Pluto:Atmospheres
• Composition (N2, Ar, CO, CH4; H, H2, HCN, CxHy)
• Pressure, temperature, temperature gradient• Hazes and clouds• Escape rate• Ionosphere• Search for atmosphere around Charon
0
500
1000
1500
2000
2500
Altitude (km)
N2
CH4
CO
Ar (?)
Main OtherVolatiles
HydrocarbonsC
2H
2, C
2H
4
C2H
6, C
4H
2
NitrilesHCN, C
2N
2
Ions
N+, CO+, C2H
5+
Haze
Solid N2, CH
4, CO
LightPhotochemical
Products
H, H2, N
after Summers et al 1997
Young et al 2006
Janvier 12 2006Workshop 3e zone Slide 34
New Horizons at Pluto:Atmospheres
• Composition (N2, Ar, CO, CH4; H, H2, HCN, CxHy)– Solar occultations, 465-1181 Å, 3.5 Å spectral resoluton, Sun subtending 8 km (Alice) for N2, CH4, CxHy, HCN, others
– Airglow observations on approach, and nightglow on departure (Alice) for Ar, CO, H, Ne, others
– Stellar occultations planned, not yet identified
• Pressure, temperature, temperature gradient– N2 line-of-sight number density in the upper atmsphere from solar and stellar occultation (Alice)
– N2 line-of-sight number density in the lower atmsphere from uplink radio occultation, dual DSN sites (REX)
• Hazes and clouds– Near-surface opacity 1800-1881 Å from solar and stellar occultation (Alice)
– Low-phase imaging (MVIC, LORRI)
– High-phase imaging at < 0.4 km/pixel (MVIC), sensitive to 10% of Triton's haze from surface to 80 km
• Escape rate– Modelling from temperatures and pressures near 2.5 Pluto radii (Alice).
– Scale height of the Lyman- airglow for H-only escape flux (Alice)
– Also SWAP and PEPSSI (next slides).
• Ionosphere– Electron density from radio occultation (REX)
• Search for atmosphere around Charon– Search to nbar levels with solar occultation (Alice)
– Supporting radio occultaion (REX)
Janvier 12 2006Workshop 3e zone Slide 35
New Horizons at Pluto:Particles and Plasmas
• Atmospheric escape rate• Solar wind interaction• Energetic particle environments• Dust enviromment
McComas et al 2007
Janvier 12 2006Workshop 3e zone Slide 36
New Horizons at Pluto:Particles and Plasmas
• Atmospheric escape rate– Energetic particle flux and composition depends on escape rate (PEPSSI, SWAP)– Distance of interface with solar wind, which is proportional to escape rate (SWAP, PEPSSI)
• Solar wind interaction– Bow shock, wake effects from direction, spead, and temperature of solar wind (SWAP, PEPSSI)
• Energetic particle environments– Enegetic pick-up ions likely 1 million km (900 Pluto radii) upsteam of Pluto. PEPSSI and SWAP will measure direction, energy, and mass of energetic particles.
• Dust enviromment– Interplanetary dust environmet, with the first dust measurements beyond 18 AU (SDC)– Immediate dust environment downstream of the Pluto system (SDC)
Janvier 12 2006Workshop 3e zone Slide 37
New Horizons at Pluto:Origin and Evolution
• Orbits• Radii, mass, density• Additional rings or satellites• Magnetic field?
Canup 2005
10,000 km
PARTIALLY HYDRATED ROCK
WATER ICE I
BASELINE PLUTO
1180 km, 1.85 g cm3
DIFFERENTIATED
ROCK FRACTION=0.65
WATER ICE I +HYDRATED ROCK
ICE II +HYDRATED ROCK
BASELINE CHARON
625 km, 1.75 g cm3
UNDIFFERENTIATED
ROCK FRACTION=0.55
McKinnon et al 1997
Janvier 12 2006Workshop 3e zone Slide 38
New Horizons at Pluto:Origin and Evolution
• Orbits– 150 days of resolved images of Pluto, Charon, Nix and Hydra at 15° solar phase angle (LORRI)
• Radii, mass, density– Masses from orbits of Pluto and satellites around barycenter (LORRI)– Masses from the deflection of New Horizons using Doppler measurements (REX) – Radii and shapes from single 1024x1024 frames Pluto and Charon at 3 km/pixel (LORRI)– Additional shape measurements from the combination of all imaging data (LORRI, MVIC, LEISA)– Additional constraints on the radii from occultation chord lengths (Alice, REX)
• Additional rings or satellites– Imaging of the entire stability zone at low phase angle (LORRI, MVIC)– High-phase observations (MVIC)
• Magnetic field?– Not directly addressed by New Horizons. A strong magnetic field may affect the solar wind interaciton (SWAP, PEPSSI).
Janvier 12 2006Workshop 3e zone Slide 39
Number of accessible KBOs
KBO Diam., km at 41 AU For 200 m/s delta-V
Limiting R Mag p=0.04 p=0.12 Total Cold classical
(easier to find)
24.0 > 160 > 92 0.14 (13%) 0.1 (10%)
25.0 > 101 > 58 0.7 (50%) 0.35 (30%)
26.0 > 64 > 37 1.8 (83%) 1.1 (67%)
27.0 > 40 > 23 4 (98%) 2.5 (92%)
Based on KBO population statistics from Bernstein et al. (2004).See Spencer et al. 2003, Earth Moon and Planets 92, 483-491.
Janvier 12 2006Workshop 3e zone Slide 40
Radial Distribution of Accessible KBOs
Strong peak at 42 AU, due to
Intrinsic peak there
Narrow cone at smaller distances
Faintness of more distant KBOs
Encounter likely 2018 or 2019
for 115 m/s delta-V
Janvier 12 2006Workshop 3e zone Slide 41
Search Area, Now and in 2011
20112011
20042004
50% of KBOs50% of KBOs85% of KBOs85% of KBOsEncounter
Locations (2015 Pluto flyby)
• In the Milky Way at both epochs• Search area shrinks with time as it converges on the spacecraft trajectory
– Defined by KBO velocity dispersion, not available delta-V
Janvier 12 2006Workshop 3e zone Slide 42
New Horizons: Exploring the Third Zone
For more information (including technical papers), see
http://pluto.jhuapl.edu