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Comparison of Interstellar Boundary Explorer Observations with 3D Global Heliospheric Models
N. A. Schwadron,1,13,*M. Bzowski,2G. B. Crew,3M. Gruntman,4H. Fahr,5H. Fichtner,6P. C. Frisch,7H. O. Funsten,8S. Fuselier,9J. Heerikhuisen,10V. Izmodenov,11H. Kucharek,12M. Lee,12G. Livadiotis,13D. J. McComas,13,14E. Moebius,12T. Moore,15J. Mukherjee,13N.V. Pogorelov,10C. Prested,1D. Reisenfeld,16E. Roelof,17G.P. Zank10
Simulations of energetic neutral atom (ENA) maps predict fluxmagnitudes that are, in some cases, similar to those observedby the Interstellar Boundary Explorer (IBEX) spacecraft, butthey miss the ribbon. Our model of the heliosphere indicatesthat the local interstellar medium (LISM) magnetic field (BLISM)is transverse to the line of sight (LOS) along the ribbon, suggestingthat the ribbon may carry its imprint. The force-per-unit areaon the heliopause from field line draping and the LISM ram pressureis comparable with the ribbon pressure if the LOS ~ 30 to 60astronomical units and BLISM ~ 2.5 microgauss. Although variousmodels have advantages in accounting for some of the observations,no model can explain all the dominant features, which probablyrequires a substantial change in our understanding of the processesthat shape our heliosphere.
1 Department of Astronomy, Boston University, Boston, MA 02215, USA. 2 Space Research Centre of the Polish Academy of Sciences, 00-716 Warsaw, Poland. 3 Kavli Institute, Massachusetts Institute of Technology, Cambridge, MA 02139, USA. 4 Astronomical Engineering Division, University of Southern California, Los Angeles, CA 90089, USA. 5 Institut für Astrophysik und Extraterrestrische Forschung, University of Bonn, 53115 Bonn, Germany. 6 Institut für Theoretische Physik IV, Ruhr-Universitaet Bochum, 44780 Bochum, Germany. 7 Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA. 8 Los Alamos National Laboratory, Los Alamos, NM 87545, USA. 9 Lockheed Martin Advanced Technology Center, Palo Alto, CA 94304, USA. 10 Department of Physics, University of Alabama, Huntsville, Alabama 35805, USA. 11 Department of Aeromechanics and Gas Dynamics, Moscow State University, and Space Research Institute (IKI) and Institute for Problems in Mechanics Russian Academy of Sciences, 117997 Moscow, Russia. 12 Department of Physics, University of New Hampshire, Space Science Center, Durham, NH 03824, USA. 13 Department of Space Science and Engineering, Southwest Research Institute, San Antonio, TX 78228, USA. 14 Department of Physics, University of Texas at San Antonio, San Antonio, TX 78249, USA. 15 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. 16 Department of Physics, University of Montana, Missoula, MT 59812, USA. 17 Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 20723, USA.
* To whom correspondence should be addressed. E-mail: nathanas{at}bu.edu
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D. J. McComas, F. Allegrini, P. Bochsler, M. Bzowski, E. R. Christian, G. B. Crew, R. DeMajistre, H. Fahr, H. Fichtner, P. C. Frisch, H. O. Funsten, S. A. Fuselier, G. Gloeckler, M. Gruntman, J. Heerikhuisen, V. Izmodenov, P. Janzen, P. Knappenberger, S. Krimigis, H. Kucharek, M. Lee, G. Livadiotis, S. Livi, R. J. MacDowall, D. Mitchell, E. Möbius, T. Moore, N. V. Pogorelov, D. Reisenfeld, E. Roelof, L. Saul, N. A. Schwadron, P. W. Valek, R. Vanderspek, P. Wurz, and G. P. Zank (13 November 2009) Science326 (5955), 959.
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