Interstellar Medium (ISM) Interstellar Extinction Star Formation
A New Vision of Science and Strategy for an Interstellar Probe … · 2011-12-20 · A New Vision...
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A New Vision of Science and Strategy for an Interstellar Probe Mission Joe Mazur, USA, [email protected] Jonathan Slavin, USA, [email protected] Matthew E. Hill, USA, [email protected] Alexander Lazarian, USA, [email protected] Eberhard Moebius, USA, [email protected] Stuart D. Bale, USA, [email protected] Merav Opher, USA, [email protected] Nathan Schwadron, USA, [email protected] Dave McComas, USA, [email protected] Priscilla Frisch, USA, [email protected] Frederic Allegrini, USA, [email protected] Karlheinz Trattner, USA, [email protected] Pauette Liewer, USA, [email protected] Ralph L. McNutt, Jr., USA, [email protected] Edmond C. Roelof, USA, [email protected] Michael Gruntman, USA, [email protected] Stamatios M. Krimigis, USA, [email protected] Randall Smith, USA, [email protected] Mark Wiedenbeck, USA, [email protected] Pontus C. Brandt,USA, [email protected] David Humm, USA, [email protected] Nicola J. Fox, USA, [email protected] Gregory Matloff, USA, [email protected] John D. Richardson, USA, [email protected] Bryan A. Palaszewski, USA, [email protected] David J. Lawrence, USA, [email protected] Brian Wood, USA, [email protected] Alan Cummings, USA, [email protected] William Kurth, USA, [email protected] Louis J. Lanzerotti, USA, [email protected] Peter Wurz, USA, [email protected] George C. Ho, USA, [email protected] Gary P. Zank, USA, [email protected] Robert Henshaw, USA, [email protected] Nikolaos Paschalidis, USA, [email protected] Adam Szabo, USA, [email protected] Carey M. Lisse, USA, [email protected] Eric R. Christian, USA, [email protected] Mihir I. Desai, USA, [email protected] Christopher Paranicas, USA, [email protected] Robert E. Gold, USA, [email protected] Edgar Rhodes, USA, [email protected] Robert Decker, USA, [email protected] Steven D. Howe, USA, [email protected] Louis Friedman, USA, [email protected] Jakobus le Roux, USA, [email protected] Kelvin Long, UK, [email protected] Timothy Horbury, UK, [email protected] Robert J. Forsyth, UK, [email protected] Malcolm Macdonald, UK, [email protected] Richard Marsden, The Netherlands, [email protected] Wing-Huen Ip, Taiwan, [email protected] Peter Bochsler, Switzerland, [email protected] Stas Barabash, Sweden, [email protected] Adri Burger, South Africa, [email protected] Marius Potgieter, South Africa, [email protected] Vladislav Izmodenov, Russia, [email protected] Yury Malama, Russia, [email protected] Dmitry Aleksashov, Russia, [email protected] Sergey V. Chalov, Russia, [email protected] Vladimir B. Baranov, Russia, [email protected] Olga Katushkina, Russia, [email protected] Elena Provornikova, Russia, [email protected] Mikhail I. Panasyuk, Russia, [email protected] Yuri Yermolaev, Russia, [email protected] Stan Grzedzielski, Poland, [email protected] Roma Ratkiewicz, Poland, [email protected] Luca Sorriso-Valvo, Italy, [email protected] Gaetano Zimbardo, Italy, gaetano.zimbardo@fis.unical.it Marco Casolino, Italy, [email protected] Karl-Heinz Schartner, Germany, Karl-Heinz.Schartner@ exp1.physik.uni-giessen.de Horst W. Loeb, Germany, [email protected] Bernd Dachwald, Germany, [email protected] Andreas Ohndorf, Germany, [email protected] Wolfgang Seboldt, Germany, [email protected] Dieter Breitschwerdt, Germany, [email protected] Klaus Scherrer, Germany, [email protected] Horst Fichtner, Germany, [email protected] Eckart Marsch, Germany, [email protected] Karl Mannheim, Germany, [email protected] Ralf Srama, Germany, [email protected] Bernd Heber, Germany, [email protected] Wolfgang Droege, Germany, [email protected] Robert F. Wimmer-Schweingruber, Germany,[email protected] Milan Maksimovic, France, [email protected] Jean-Louis Bougeret, France, [email protected] Rosine Lallement, France, [email protected] Pekka Janhunen, Finland, pekka.janhunen@fmi.fi Timo Laitinen, Finland, timo.laitinen@utu.fi Ingrid Mann, Belgium, [email protected] Helmut O. Rucker, Austria, [email protected] Iver Cairns, Australia, [email protected] Lamartine Guimarães, [email protected] 11-04592 SH11A-1903 2011 AGU Fall Meeting San Francisco, CA 5 December 2011 (1) Department of Astronautical Engineering, University of Southern California, Los Angeles, CA, United States. (2) Space Department, The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, United States. (3) Institut fuer Experimentelle und Angewandte Physik, University of Kiel, Kiel, Germany. (4) Office of Space Research and Technology, Academy of Athens, Athens, Greece. The recent in situ and remote observations from the Voyager Interstellar Mission (VIM), the Interstellar Boundary Explorer (IBEX), and the Ion and Neutral Camera (INCA) on Cassini have revealed the interaction of the heliosphere with the very local interstellar medium (VLISM) to be much more complex than described by our present-day concepts. These discoveries call for a major revision of the strategy for the Interstellar Probe, a mission to explore the interstellar medium surrounding the Solar System. Voyager 1 and Voyager 2 continue to reveal unanticipated flow patterns and significant fluxes of energetic particles in the heliosheath (beyond the solar wind termination shock) while pointing to a more remote location for the modulation region and source of the anomalous cosmic rays (ACRs). Remarkably, over the past year Voyager 1 has been reporting near-zero plasma flows (tens of kilometers per second) beyond 115 AU. One implication of this flow stagnation is that Voyager is already in a “transition layer” that could lead to the interstellar plasma. Consequently, an Interstellar Probe Mission may “punch out” into the deflected interstellar plasma flow at a much smaller distance than previous models had predicted. Global imaging observations by IBEX and INCA of energetic neutral atoms (ENAs) originating from the interaction region(s) of the solar wind and the VLISM show unexpected structure and possible time dependence on a variety M. Gruntman 1 ; R. L. McNutt 2 ; S. M. Krimigis 2,4 ; E. C. Roelof 2 ; R. F. Wimmer-Schweingruber 3 ; R. E. Gold 2 of scales. In addition to the general “glow” of the sky in ENAs, IBEX revealed a relatively narrow “ribbon” of enhanced atomic hydrogen emission from ~200 eV to ~6 keV. The neutrals from both the glow and ribbon are also characterized by nonthermal distribution functions. In addition, INCA sees a “belt” of emission in ENAs, broader than the ribbon and tilted significantly away from it, at even higher energies (tens of kiloelectron volts). This evidence supports the idea that the bulk of the energy density in the heliosheath plasma resides in a nonthermal component that extends to very high energies. We have never sampled such a huge and dynamic plasma regime that is dominated by nonthermal pressure, but this regime must be representative of the astrospheres of stars similar to our Sun. These new quantitative and qualitative implications for the overall heliospheric structure already call for a new generation of measurements to understand the global nature of our Sun’s interaction with the local galactic environment. An interstellar probe with modern instruments and measurement requirements better defined by these recent observations will certainly advance our understanding of the heliospheric interaction and the VLISM. New launch vehicles in the evolving fleet, including the Atlas V, Delta IV and Falcon Heavy, offer new capabilities that can enable such a mission with an acceptable development and launch cost. The 93 signatories to the Heliophysics Decadal Survey White Paper advocating an Interstellar Probe: ABSTRACT
Transcript of A New Vision of Science and Strategy for an Interstellar Probe … · 2011-12-20 · A New Vision...
A New Vision of Science and Strategy for an Interstellar Probe Mission
Joe Mazur, USA, [email protected] Jonathan Slavin, USA, [email protected] Matthew E. Hill, USA, [email protected] Alexander Lazarian, USA, [email protected] Eberhard Moebius, USA, [email protected] Stuart D. Bale, USA, [email protected] Opher, USA, [email protected] Nathan Schwadron, USA, [email protected] Dave McComas, USA, [email protected] Priscilla Frisch, USA, [email protected] Frederic Allegrini, USA, [email protected] Karlheinz Trattner, USA, [email protected] Pauette Liewer, USA, [email protected] Ralph L. McNutt, Jr., USA, [email protected] Edmond C. Roelof, USA, [email protected] Michael Gruntman, USA, [email protected] Stamatios M. Krimigis, USA, [email protected] Randall Smith, USA, [email protected] Mark Wiedenbeck, USA, [email protected] Pontus C. Brandt,USA, [email protected] Humm, USA, [email protected] J. Fox, USA, [email protected] Gregory Matloff, USA, [email protected] John D. Richardson, USA, [email protected]
Bryan A. Palaszewski, USA, [email protected] David J. Lawrence, USA, [email protected] Wood, USA, [email protected] Cummings, USA, [email protected] Kurth, USA, [email protected] J. Lanzerotti, USA, [email protected] Wurz, USA, [email protected] George C. Ho, USA, [email protected] Gary P. Zank, USA, [email protected] Robert Henshaw, USA, [email protected] Nikolaos Paschalidis, USA, [email protected] Szabo, USA, [email protected] M. Lisse, USA, [email protected] R. Christian, USA, [email protected] I. Desai, USA, [email protected] Paranicas, USA, [email protected] E. Gold, USA, [email protected] Rhodes, USA, [email protected] Decker, USA, [email protected] D. Howe, USA, [email protected] Friedman, USA, [email protected] le Roux, USA, [email protected] Long, UK, [email protected] Horbury, UK, [email protected]
Robert J. Forsyth, UK, [email protected] Macdonald, UK, [email protected] Marsden, The Netherlands, [email protected] Ip, Taiwan, [email protected] Bochsler, Switzerland, [email protected] Barabash, Sweden, [email protected] Burger, South Africa, [email protected] Potgieter, South Africa, [email protected] Izmodenov, Russia, [email protected] Malama, Russia, [email protected] Aleksashov, Russia, [email protected] Sergey V. Chalov, Russia, [email protected] B. Baranov, Russia, [email protected] Katushkina, Russia, [email protected] Provornikova, Russia, [email protected] I. Panasyuk, Russia, [email protected] Yermolaev, Russia, [email protected] Grzedzielski, Poland, [email protected] Ratkiewicz, Poland, [email protected] Sorriso-Valvo, Italy, [email protected] Zimbardo, Italy, [email protected] Casolino, Italy, [email protected] Schartner, Germany, Karl-Heinz.Schartner@ exp1.physik.uni-giessen.de
Horst W. Loeb, Germany, [email protected] Dachwald, Germany, [email protected] Ohndorf, Germany, [email protected] Seboldt, Germany, [email protected] Breitschwerdt, Germany, [email protected] Scherrer, Germany, [email protected] Fichtner, Germany, [email protected] Marsch, Germany, [email protected] Mannheim, Germany, [email protected] Srama, Germany, [email protected] Heber, Germany, [email protected] Droege, Germany, [email protected] F. Wimmer-Schweingruber, Germany,[email protected] Maksimovic, France, [email protected] Bougeret, France, [email protected] Lallement, France, [email protected] Janhunen, Finland, [email protected] Laitinen, Finland, [email protected] Ingrid Mann, Belgium, [email protected] O. Rucker, Austria, [email protected] Cairns, Australia, [email protected] Guimarães, [email protected]
11-04592
SH11A-19032011 AGU Fall MeetingSan Francisco, CA5 December 2011
(1) Department of Astronautical Engineering, University of Southern California, Los Angeles, CA, United States. (2) Space Department, The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, United States. (3) Institut fuer Experimentelle und Angewandte Physik, University of Kiel, Kiel, Germany. (4) Office of Space Research and Technology, Academy of Athens, Athens, Greece.
The recent in situ and remote observations from the Voyager Interstellar Mission (VIM), the Interstellar Boundary Explorer (IBEX), and the Ion and Neutral Camera (INCA) on Cassini have revealed the interaction of the heliosphere with the very local interstellar medium (VLISM) to be much more complex than described by our present-day concepts. These discoveries call for a major revision of the strategy for the Interstellar Probe, a mission to explore the interstellar medium surrounding the Solar System. Voyager 1 and Voyager 2 continue to reveal unanticipated flow patterns and significant fluxes of energetic particles in the heliosheath (beyond the solar wind termination shock) while pointing to a more remote location for the modulation region and source of the anomalous cosmic rays (ACRs). Remarkably, over the past year Voyager 1 has been reporting near-zero plasma flows (tens of kilometers per second) beyond 115 AU.
One implication of this flow stagnation is that Voyager is already in a “transition layer” that could lead to the interstellar plasma. Consequently, an Interstellar Probe Mission may “punch out” into the deflected interstellar plasma flow at a much smaller distance than previous models had predicted. Global imaging observations by IBEX and INCA of energetic neutral atoms (ENAs) originating from the interaction region(s) of the solar wind and the VLISM show unexpected structure and possible time dependence on a variety
M. Gruntman1; R. L. McNutt2; S. M. Krimigis2,4; E. C. Roelof2; R. F. Wimmer-Schweingruber3; R. E. Gold2
of scales. In addition to the general “glow” of the sky in ENAs, IBEX revealed a relatively narrow “ribbon” of enhanced atomic hydrogen emission from ~200 eV to ~6 keV. The neutrals from both the glow and ribbon are also characterized by nonthermal distribution functions. In addition, INCA sees a “belt” of emission in ENAs, broader than the ribbon and tilted significantly away from it, at even higher energies (tens of kiloelectron volts). This evidence supports the idea that the bulk of the energy density in the heliosheath plasma resides in a nonthermal component that extends to very high energies. We have never sampled such a huge and dynamic plasma regime that is dominated by nonthermal pressure, but this regime must be representative of the astrospheres of stars similar to our Sun.
These new quantitative and qualitative implications for the overall heliospheric structure already call for a new generation of measurements to understand the global nature of our Sun’s interaction with the local galactic environment. An interstellar probe with modern instruments and measurement requirements better defined by these recent observations will certainly advance our understanding of the heliospheric interaction and the VLISM. New launch vehicles in the evolving fleet, including the Atlas V, Delta IV and Falcon Heavy, offer new capabilities that can enable such a mission with an acceptable development and launch cost.
The 93 signatories to the Heliophysics Decadal Survey White Paper advocating an Interstellar Probe:
ABSTRACT
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