outer solar system (oss) a planetary and fundamental physics mission to neptune, triton and kbo b....

Outer Solar System (OSS)A Planetary and Fundamental Physics Mission to Neptune, Triton and KBO

B. Christophe on behalf of OSS Team

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OSS

Eddington’s Parameter at 10-7

Deep SpaceGravity at 10 pm/s2

NeptuneTriton

Kuiper Belt Object

Od

ysse

y, C

osm

ic V

isio

n 1

Mis

sion

to

test

dee

p sp

ace

grav

ityA

rgo

, New

Fro

ntiers 4

Mission to N

eptune, Triton and K

BO

Planetary PhysicsFundamental Physics

Inline with Fundamental Physics Roadmaps Advisory Group Report

3

Deep Space Gravity Test

Accurate Navigation of S/CAccurate Navigation of S/C

Radio-Science

Laser-Science

PositioningPositioning

1-way or2-waysX+Ka band

VLBI

What is the S/C trajectory ?What is the S/C trajectory ?

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Laser Science: two concepts

One-way pulsed laser(proposed by E. Samain – OCA)

Two-ways continuous coherent laser(proposed by P. Wolf – SYRTE)

Clock

Spectral Filter

Linear Photo-

Detection

Coarse Timing (FPGA)

Res = 10 ns

Temporal Filter (x pseudo

random code)

Calculator

Fine Timing(Vernier)

Res = 10 ps

Frequency Synthesis

Telemetry

Laser pulse

Clock

Spectral Filter

Linear Photo-

Detection

Coarse Timing (FPGA)

Res = 10 ns

Temporal Filter (x pseudo

random code)

Calculator

Fine Timing(Vernier)

Res = 10 ps

Frequency Synthesis

Telemetry

Laser pulse

TESA TCL Terminal

PLL Laser

USO

100 MHzfrom ground

to ground

PBS

1064 nmMercury Ion JPL or Horace Syrte clock

Adaptative Optics on ground

5

Deep Space Gravity Test

Accurate Navigation of S/CAccurate Navigation of S/C

Radio-Science

Laser-Science

PositioningPositioning

1-way or2-ways

Non Gravitational ForcesNon Gravitational Forces

DC Accelerometer< 10 pm/s2

X+Ka bandVLBI

Is S/C on a geodesic ?Is S/C on a geodesic ?

What is the S/C trajectory ?What is the S/C trajectory ?

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DC Accelerometer GAP

Noise of MicroSTAR

1.E-13

1.E-12

1.E-11

1.E-10

1.E-09

1.E-08

1.E-05 1.E-04 1.E-03 1.E-02 1.E-01 1.E+00

Frequency (Hz)

No

ise

(m

/s2 /H

z1/

2 )

Total

Detector

Wire damp

ADC

CPD

Meas

Recomb

PID

Electrostatic accelerometer MicroSTAR based on heritage of

CHAMP, GRACE and GOCE missions(developed by ONERA)

Bias Rejection System rotating stage with piezo-electric motor

(developed by ZARM)

Perfo ~ 1 pm/s2

For more details, see Benjamin Lenoir Poster

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General Relativity Test / Geodesy

Deep Space Gravity(OSS)

Gravitational Wave(LISA)

Equivalence Principle(Microscope)

GRACE / NGGMCHAMP GOCE

Orbit determinationMeasure of NG

Variation of Laser LinkDrag Compensation

Differential accelerationDrag Compensation

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OSS Spacecraft

RPW (x3)

MAG

Imaging instruments

Laser telescope

HGA

Towards Earth

Towards ram

Boresights direction for planetary observation GAP on

settable plate

ASRG

ASRG

4 tanks symmetric wrt GAP,

interconnected fluid

Imaging instruments

Fundamental Physics Inst.

DC Accelerometer : 3.5 kg / 3 WRadio-Science: 3.5 kg / 40 WUSO: 1.5 kg / 5.5 W1-way Laser Science: 14.5 kg / 20 W2-ways Laser Science:25 kg / 80 W

Planetary instruments

UV Spectrometer: 5.0 kg / 12 WHigh Resolution Narrow Camera: 9.8 kg / 14 WIR Spectrometer / Wide Angle Camera:

10.1 kg /7.5 WRadio Plasma Wave: 4.7 kg / 7.9 WThermal Map Imager: 7.0 kg / 20 WMagnetometer: 3.3 kg / 3 WDust Particle Detector: 3.5 kg / 9 W

S/C Data Sheet

Mass: 540 kg (48 kg payload)Available Power: 294 W BoL, 250 W EoLComm: 2.1 m antenna, Band KaAttitude Control: 3 axis (±0.03°)Propulsion: 4 tanks of hydrazine

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Self-gravity Management

• Accelerometer at S/C CoG• S/C mass far from accelerometer • Symmetry of tanks• Membranes for ergol location• Thermal Gauging & Book Keeping for ergol mass

Self-gravity < 14 pm/s2

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Conclusions

• OSS was not selected by ESA for Cosmic Vision M3• Fundamental Physics Objectives considered strong• Planetary Objectives considered weak (flyby instead orbiter)• RTG availability considered as a risk• Launcher cost by US considered as a strategic risk

• OSS allows to do pioneer work on• Merging of Fundamental and Planetary Physics as recommended by

FPRAT• Adaptative optics for 2-ways laser link• DC accelerometer with 1 pm/s2 accuracy• S/C design for severe self-gravity requirement

• Future works should concerns• Integration of the DC accelerometer in the S/C• Convincing planetary community of interest of accelerometer

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Acknowledgement to OSS scientific supporters

• European side: PI B. Christophe (ONERA)• CESR (France) : Nicolas André• DLR / Institute of Planetary Research (Germany): Ralf Jaumann, Jörn Helbert, Hauke Hussmann, Nicole Schmitz, Frank Sohl, Katrin Stephan• DLR / Institute of Space System (Germany): Hansjörg Dittus, Marco Sharringhausen, Tim van Zoest• GeoAzur / OCA (France) : Gilles Métris, Etienne Samain• IGEP, TU Braunschweig (Germany): Karl-Heinz Glassmeier, Daniel Heyner• Imperial College (United Kingdom) : Patrick Brown, Michelle Dougherty, Tim Sumner• Institute for Geophysics and Meteorology / Univ. Köln (Germany) : Martin Pätzold• Institute for Planetology / Westfälische Wilhelms Universität (Germany): Harry Hiesinger• Institut für Geowissenschaften / Max Planck Institute (Germany): Frank Postberg, Ralf Srama• Institut für Physik und Astronomie / Universität Postdam (Germany): Jürgen Schmidt• Instituto Superior Técnico (Portugal): Frederico Francisco, Paulo J.S. Gil, Jorge Páramos• JIVE (The Netherlands) : Sergei V. Progrebenko• LATMOS (France): Jean-Louis Bertaux, François Leblanc, Eric Quemerais• LESIA / Observatoire de Paris (France): Antonella Barucci, Baptiste Cecconi, Laurent Lamy• LKB / ENS (France) : Jean-Michel Courty, Brahim Lamine, Serge Reynaud• ONERA (France) : Bruno Christophe, Bernard Foulon, Benjamin Lenoir, Agnès Levy, Vincent Michau, Clélia Robert, Marc Séchaud, Pierre Touboul• Rutherford Appleton Laboratory (United Kingdom): Robert Bingham• Service d'Astrophysique/IRFU CEA Saclay (France) : Roland Lehoucq• SYRTE / Observatoire de Paris (France): Peter Wolf• Universidade do Porto (Portugal): Orfeu Bertolami• University of Oxford (UK): Leigh Fletcher• ZARM (Germany) : Claus Lämmerzahl, Hanns Selig

• US side: co-PI L. Spilker (JPL)• Cornell University: Dr. Don Banfield• JPL / NASA: Dr. John D. Anderson (retired), Dr. Sami W. Asmar, Dr. Glenn Orton, Dr. Kim R. Reh, Dr. Linda J. Spilker, Dr. Thomas R. Spilker• Lowell Observatory: Dr. Will Grundy• Planetary Science Institute: Dr. Candice Hansen• UCLA: Dr. Johnatan Aurnou, Dr. Ravit Helled, Dr. Kunio Sanayagi