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LLR: how to reach 1 mm?

Join the discussion at the LLR workshop in Bern, Switzerland to explore the scientific motivation, ground-based stations, lunar targets, model and software code needed to achieve 1mm precision in lunar laser ranging. We will also address collaboration, code verification, funding, personnel, and synergistic opportunities with GRAIL, SELENE 2, ILN, India, Russia, and more.

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LLR: how to reach 1 mm?

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  1. LLR: how to reach 1 mm? General Discussion @ the First LLR workshop “Theory and Model for the New Generation of the Lunar Laser Ranging Data”Bern, Switzerland, 16-19 February 2010

  2. Where Are We Now? What do we need? • Scientific Motivation • Ground-based stations • New lunar targets • Model and software code Other issues: • Collaboration (and the current “LLR business model”) • Code verification Challenges: • Funding • Personnel Synergistic Opportunities: • GRAIL, SELENE 2, ILN, India, Russia, etc.

  3. What Do We Need to Reach 1mm? Scientific Motivation (for factor ~25 improvement): • Lunar interior (compare with GRAIL): • Fluid core, solid inner core, their interaction • Collaboration with geophysical community (seismometers, heat flow, etc.) • Gravitational physics (compare with APOLLO): • EP (1e-15), G-dot (1e-14), other? Ground-based LLR stations: • Individual station performance: • Laser pulse width <1mm • Calibration procedures • Atmospheric monitoring procedures • Local geophysical environment monitoring • Continuity… • Other factors: • Coverage: we need more stations and also in the southern hemisphere; • Formats (normal points, auxiliary data, etc.) • Network of LLR-capable stations; real-time auxiliary data (e.g., E. Pavlis talk)

  4. What do we need to reach 1mm? Lunar CCR: • Individual retro-reflector performance: • Target precision: less than 1mm return pulse (single CCR) • Return flux comparable with A15 • Stability of emplacement, pointing and clocking • Other factors: • More reflectors • Wider geographical spread • Collaboration with geophysics community (seismic, heat, etc.) Model for LLR Observable: • Earth-moon orbital motion • Lunar rotation: • Lunar librations – 1 mm • Reference frames, time scales, etc.

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