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FUTURE OBSERVATIONS OF THE OUTER HELIOSPHERE

FUTURE OBSERVATIONS OF THE OUTER HELIOSPHERE. M. Hilchenbach and H. Rosenbauer Max-Planck-Institut für Aeronomie, D-37189 Katlenburg-Lindau, Germany. outer heliosphere ....the next frontier. NASA 1964. Frisch 2000. Observables. Based on Frisch 2000. Sun - Heliosphere. Fisk 1996.

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FUTURE OBSERVATIONS OF THE OUTER HELIOSPHERE

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  1. FUTURE OBSERVATIONS OF THE OUTER HELIOSPHERE M. Hilchenbach and H. Rosenbauer Max-Planck-Institut für Aeronomie, D-37189 Katlenburg-Lindau, Germany

  2. outer heliosphere ....the next frontier NASA 1964 Frisch 2000

  3. Observables Based on Frisch 2000

  4. Sun - Heliosphere Fisk 1996 Axford Suess 1994 Woch 1997

  5. Anomalous Cosmic Rays Charge State Determination via earth’s magnetic field Keppler 1998 Leske 2000 based on Dichter 1990

  6. Micro-Calorimeter Stacks will be used for the Advanced Cosmic-Ray Composition Experiment for the Space Station (ACCESS 2005)

  7. Ion Detectors Russel

  8. Neutral Hydrogen Solar and Interstellar Kohl 1998 SOHO SWAN 1999

  9. Principles of Neutral Particle Detection Gruntman 1997

  10. Neutral Particle Detectors ASPERA-3 Mars Express 2003 Cheng 1993 MENA IMAGE 2000

  11. Neutral Particle Detection Efficiency H - Barat 2000 from Gruntman 1997

  12. Interstellar Helium Detector Witte 1992 NIHEAD Interplanetary Pathfinder 1998 Witte 1999

  13. Surface conversion and detection Metastable atoms Borovik 2000 H Denier van der Gon 2000 Schwarz-Selinger 2000

  14. Wave properties of photons or atoms UV Suppression Gruntman 1997 focussing of ‘cold atom beam’ Doak 1999

  15. Time-of-flight analyzer with a floatable drift tube Simultaneous energy distribution and ion/neutral fraction measurements using a linear time-of-flight Morozov 1999

  16. Hadamard transform time-of-flight mass spectrometer High duty cycle: about 50% Brock 1999

  17. Mass spectroscopy using a rotating electric field E time-of-flight phase Clemmons 1998

  18. E B Energy-Mass Spectrograph for Measurement of Ions and Neutral Atoms Funsten 1996

  19. Silicon Anode Detector (CCD) Vickers 1999

  20. A Capacitance Standard Based on Counting Electrons ‘Quantum dots’ Temperature 40 mK Keller 1999

  21. Ion Propulsion System DS1 1998 Possible ionisation of interstellar atoms of the LISM

  22. Space and Time SOHO LASCO C2 1996

  23. 2 D Pictures : Example SOHO LASCO C1 Inhester 1998

  24. Model and Observation: Example Inhester 2000

  25. Towards a 3D Picture Stereoscopy (and Tomography) Tools: Photons and Neutral Atoms* *Trajectories are ballistic orbits, for energetic neutrals far off the sun a straight line is appropriate.

  26. Stereoscopy of “heliospheric” objects (I) point-like objects line objects - an overdetermined problem - a well determined problem Based on Inhester 2000

  27. Stereoscopy of “heliospheric” objects (II) ambiguities of a single line position error multiple crossings of the epipolar plane The error is proportional to pixel size / sin (f/2) , where f is the angle between projection surface normals at intersection. The error is particular large at the line tops.

  28. Stereoscopy of “heliospheric” objects (III) ambiguities for line systems Surfaces and clouds - an underdeterminded problem Additional constrains, e.g. assumption of a curvature radius R in the epipolar plane can help. Multiple solutions if a unique correspondence between individual lines in the two images cannot be found

  29. Stereoscopy vs tomography Fundamental assumption in stereoscopy: Generalisation in tomography: Emission from a single spot along line of sight - a second view is sufficient to determine d. Emission distributed along line of sight - a large number of other views required to resolve F(d). - not possible from the inner heliosphere….

  30. Observations including the event timing Events resolved in time and angular space Fluctuations in time A tA C B observed f(t) along line-of-sight vB * tB vA * tA ambiguities for line systems can be resolved Coincidence measurement requires good detection efficiency. Inversion from inner helio- sphere possible ?

  31. View beyond the heliosphere (about 250 years ago)

  32. The Next Frontier Stereoscopic (and Tomgraphic) Observations of the Outer Heliosphere Observables in the Inner Heliosphere - Photons - Energetic Neutral Atoms - Solar wind, Pick-up ions, Cosmic Rays Requirements: - Models of Global and Local Structures in Space and Time - Multispacecraft observation with Resolution in 2D Space and Time - High efficiency and resolution instruments (Coincidence Measurements)

  33. MCP Detectors and Friction Marckwordt 2000

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