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1. Corotating Interaction Regions at High Latitudes

Author

Dept. of Atmospheric and Space Sciences, University of Michigan, Ann Arbor, Michigan, USA, Extraterrestrische Physik, Universit??t Kiel, Kiel, Germany, Space Science Center, University of New Hampshire, Durham, New Hampshire, USA, The Blackett Laboratory, Imperial College, London, United Kingdom, Max-Planck-Institut f??r Aeronomie, Katlenburg-Lindau, Germany, The Blackett Laboratory, Imperial College, London, United Kingdom; Queen Mary and Westfield College, London, United Kingdom, Depts. of Planetary Sciences and Astronomy, University of Arizona, Tucson, Arizona, USA, Dipartimento di Fisica, Universit?? di, Milano, Milano, Italy, Enrico Fermi Institute, University of Chicago, Chicago, Illinois, USA, Potchefstroom University for CHE, Potchefstroom, South Africa, Applied Physics Laboratory, Johns Hopkins University, Laurel, Maryland, USA, Space Science Dept.,???ESA/ESTEC, Noordwijk, The Netherlands, Physics and Astronomy Dept., University of Birmingham, Birmingham, United Kingdom, International Space Science Institute, Bern, Switzerland, Jet Propulsion Laboratory, Pasadena, California, USA, Physikalisches Institut der Universit??t Bern, Bern, Switzerland, Ann Arbor, Potgieter, M.S., Von Steiger, R., Sanderson, T.R., Kunow, H., Lee, M.A., Fisk, Len A., Heber, B., Keppler, E., Lou, Y.-Q., McKibben, R.B., Paizis, C., Roelof, E.C., Simnett, G.M., Tsurutani, B.T., Wimmer-Schweingruber, R.F., Jokipii, J.R., Forsyth, R.J., Horbury, T.S., K??ta, J., Dept. of Atmospheric and Space Sciences, University of Michigan, Ann Arbor, Michigan, USA, Extraterrestrische Physik, Universit??t Kiel, Kiel, Germany, Space Science Center, University of New Hampshire, Durham, New Hampshire, USA, The Blackett Laboratory, Imperial College, London, United Kingdom, Max-Planck-Institut f??r Aeronomie, Katlenburg-Lindau, Germany, The Blackett Laboratory, Imperial College, London, United Kingdom; Queen Mary and Westfield College, London, United Kingdom, Depts. of Planetary Sciences and Astronomy, University of Arizona, Tucson, Arizona, USA, Dipartimento di Fisica, Universit?? di, Milano, Milano, Italy, Enrico Fermi Institute, University of Chicago, Chicago, Illinois, USA, Potchefstroom University for CHE, Potchefstroom, South Africa, Applied Physics Laboratory, Johns Hopkins University, Laurel, Maryland, USA, Space Science Dept.,???ESA/ESTEC, Noordwijk, The Netherlands, Physics and Astronomy Dept., University of Birmingham, Birmingham, United Kingdom, International Space Science Institute, Bern, Switzerland, Jet Propulsion Laboratory, Pasadena, California, USA, Physikalisches Institut der Universit??t Bern, Bern, Switzerland, Ann Arbor, Potgieter, M.S., Von Steiger, R., Sanderson, T.R., Kunow, H., Lee, M.A., Fisk, Len A., Heber, B., Keppler, E., Lou, Y.-Q., McKibben, R.B., Paizis, C., Roelof, E.C., Simnett, G.M., Tsurutani, B.T., Wimmer-Schweingruber, R.F., Jokipii, J.R., Forsyth, R.J., Horbury, T.S., and K??ta, J.

Abstract

Ulysses observed a stable strong CIR from early 1992 through 1994 during its first journey into the southern hemisphere. After the rapid latitude scan in early 1995, Ulysses observed a weaker CIR from early 1996 to mid-1997 in the northern hemisphere as it traveled back to the ecliptic at the orbit of Jupiter. These two CIRs are the observational basis of the investigation into the latitudinal structure of CIRs. The first CIR was caused by an extension of the northern coronal hole into the southern hemisphere during declining solar activity, whereas the second CIR near solar minimum activity was caused by small warps in the streamer belt. The latitudinal structure is described through the presentation of three 26-day periods during the southern CIR. The first at???24??S shows the full plasma interaction region including fast and slow wind streams, the compressed shocked flows with embedded stream interface and heliospheric current sheet (HCS), and the forward and reverse shocks with associated accelerated ions and electrons. The second at 40??S exhibits only the reverse shock, accelerated particles, and the 26-day modulation of cosmic rays. The third at 60??S shows only the accelerated particles and modulated cosmic rays. The possible mechanisms for the access of the accelerated particles and the CIR-modulated cosmic rays to high latitudes above the plasma interaction region are presented. They include direct magnetic field connection across latitude due to stochastic field line weaving or to systematic weaving caused by solar differential rotation combined with non-radial expansion of the fast wind. Another possible mechanism is particle diffusion across the average magnetic field, which includes stochastic field line weaving. A constraint on connection to a distant portion of the CIR is energy loss in the solar wind, which is substantial for the relatively slow-moving accelerated ions. Finally, the weaker northern CIR is compared with the southern CIR. It is weak

Published
2006

2. Global Processes that Determine Cosmic Ray Modulation

Author

Dept. of Atmospheric, Oceanic, and Space Sciences, Univ. of Michigan, Ann Arbor, MI, 48109, USA, Lebedev Physical Institute, Russian Academy of Sciences, Moscow, 117924, Russia, Institut für Experimentelle und Angewandte Physik, Universität Kiel, 24118, Kiel, Germany, Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Japan, Potchefstroom University for CHE, Potchefstroom, South Africa, Enrico Fermi Institute and Dept. of Physics, The University of Chicago, Chicago, IL, 60637, USA, California Institute of Technology, Pasadena, CA, 91125, USA, Space Science Department of ESA, ESTEC, NL-2200 AG, Noordwijk, The Netherlands, The Blackett Laboratory, Imperial College, London, SW7 2BZ, United Kingdom, Bartol Research Institute, University of Delaware, Newark, DE, 19716, USA, University of Arizona, Tucson, AZ, 85721, USA, Institute for Physical Science and Technology, Univ. of Maryland, College Park, MD, 20742, USA, NASA Marshall Space Flight Center/ES82, Huntsville, AL, 35812, USA, New Mexico State University, Las Cruces, NM, 88003-001, USA, CEA, DSM/DAPNIA/Service d'Astrophysique, CE-Saclay, F-91191, Gif-sur-Yvette Cedex, France, Space Science Center, University of New Hampshire, Durham, NH, 03842, USA, Ann Arbor, Fisk, Len A., Wenzel, K.-P., Balogh, A., Burger, R.A., Cummings, A.C., Evenson, P., Heber, B., Jokipii, J.R., Krainev, M.B., Kóta, J., Kunow, H., Le Roux, J.A., McDonald, F.B., McKibben, R.B., Potgieter, M.S., Simpson, J.A., Steenberg, C.D., Suess, S., Webber, W.R., Wibberenz, G., Zhang, M., Ferrando, P., Fujii, Z., Lockwood, J.A., Moraal, H., Stone, E.C., Dept. of Atmospheric, Oceanic, and Space Sciences, Univ. of Michigan, Ann Arbor, MI, 48109, USA, Lebedev Physical Institute, Russian Academy of Sciences, Moscow, 117924, Russia, Institut für Experimentelle und Angewandte Physik, Universität Kiel, 24118, Kiel, Germany, Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Japan, Potchefstroom University for CHE, Potchefstroom, South Africa, Enrico Fermi Institute and Dept. of Physics, The University of Chicago, Chicago, IL, 60637, USA, California Institute of Technology, Pasadena, CA, 91125, USA, Space Science Department of ESA, ESTEC, NL-2200 AG, Noordwijk, The Netherlands, The Blackett Laboratory, Imperial College, London, SW7 2BZ, United Kingdom, Bartol Research Institute, University of Delaware, Newark, DE, 19716, USA, University of Arizona, Tucson, AZ, 85721, USA, Institute for Physical Science and Technology, Univ. of Maryland, College Park, MD, 20742, USA, NASA Marshall Space Flight Center/ES82, Huntsville, AL, 35812, USA, New Mexico State University, Las Cruces, NM, 88003-001, USA, CEA, DSM/DAPNIA/Service d'Astrophysique, CE-Saclay, F-91191, Gif-sur-Yvette Cedex, France, Space Science Center, University of New Hampshire, Durham, NH, 03842, USA, Ann Arbor, Fisk, Len A., Wenzel, K.-P., Balogh, A., Burger, R.A., Cummings, A.C., Evenson, P., Heber, B., Jokipii, J.R., Krainev, M.B., Kóta, J., Kunow, H., Le Roux, J.A., McDonald, F.B., McKibben, R.B., Potgieter, M.S., Simpson, J.A., Steenberg, C.D., Suess, S., Webber, W.R., Wibberenz, G., Zhang, M., Ferrando, P., Fujii, Z., Lockwood, J.A., Moraal, H., and Stone, E.C.

Abstract

The global processes that determine cosmic ray modulation are reviewed. The essential elements of the theory which describes cosmic ray behavior in the heliosphere are summarized, and a series of discussions is presented which compare the expectations of this theory with observations of the spatial and temporal behavior of both galactic cosmic rays and the anomalous component; the behavior of cosmic ray electrons and ions; and the 26-day variations in cosmic rays as a function of heliographic latitude. The general conclusion is that the current theory is essentially correct. There is clear evidence, in solar minimum conditions, that the cosmic rays and the anomalous component behave as is expected from theory, with strong effects of gradient and curvature drifts. There is strong evidence of considerable latitude transport of the cosmic rays, at all energies, but the mechanism by which this occurs is unclear. Despite the apparent success of the theory, there is no single choice for the parameters which describe cosmic ray behavior, which can account for all of the observed temporal and spatial variations, spectra, and electron vs. ion behavior.

Published
2006

3. The Solar Origin of Corotating Interaction Regions and Their Formation in the Inner Heliosphere

Author

Dept. of Atmosph., Oceanic, and Space Sciences, University of Michigan, Ann Arbor, Mich., USA, Dept. of Physics and IPST, University of Maryland, College Park, Maryland, USA; Dept. of Atmosph., Oceanic, and Space Sciences, University of Michigan, Ann Arbor, Mich., USA, Science Applications International Corporation, San Diego, California, USA, International Space Science Institute, Bern, Switzerland, Mullard Radio Astronomy Observatory, Cavendish Laboratory, Cambridge, United Kingdom, The Blackett Laboratory, Imperial College, London, United Kingdom, Extraterrestrische Physik, Universität Kiel, Kiel, Germany, Center for Space Physics, Boston University, Boston, Massachusetts, USA, Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, Germany, Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany, Astrophysikalisches Institut, Potsdam, Germany, NASA/Goddard Space Flight Center, Greenbelt, Maryland, USA; Dept. of Physics and IPST, University of Maryland, College Park, Maryland, USA, Physikalisches Institut der Universität Bern, Bern, Switzerland, E.O. Hulburt Center for Space Research, Naval Research Laboratory, Washington, DC, USA, Ann Arbor, Crooker, N.U., Balogh, A., Bothmer, V., Forsyth, R.J., Gloeckler, George, Hewish, A., Hilchenbach, M., Kallenbach, R., Klecker, B., Linker, J.A., Lucek, E., Mann, G., Marsch, E., Posner, A., Richardson, I.G., Schmidt, J.M., Scholer, M., Wang, Y.-M., Wimmer-Schweingruber, R.F., Aellig, M.R., Bochsler, P., Hefti, S., Mikić, Z., Dept. of Atmosph., Oceanic, and Space Sciences, University of Michigan, Ann Arbor, Mich., USA, Dept. of Physics and IPST, University of Maryland, College Park, Maryland, USA; Dept. of Atmosph., Oceanic, and Space Sciences, University of Michigan, Ann Arbor, Mich., USA, Science Applications International Corporation, San Diego, California, USA, International Space Science Institute, Bern, Switzerland, Mullard Radio Astronomy Observatory, Cavendish Laboratory, Cambridge, United Kingdom, The Blackett Laboratory, Imperial College, London, United Kingdom, Extraterrestrische Physik, Universität Kiel, Kiel, Germany, Center for Space Physics, Boston University, Boston, Massachusetts, USA, Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, Germany, Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany, Astrophysikalisches Institut, Potsdam, Germany, NASA/Goddard Space Flight Center, Greenbelt, Maryland, USA; Dept. of Physics and IPST, University of Maryland, College Park, Maryland, USA, Physikalisches Institut der Universität Bern, Bern, Switzerland, E.O. Hulburt Center for Space Research, Naval Research Laboratory, Washington, DC, USA, Ann Arbor, Crooker, N.U., Balogh, A., Bothmer, V., Forsyth, R.J., Gloeckler, George, Hewish, A., Hilchenbach, M., Kallenbach, R., Klecker, B., Linker, J.A., Lucek, E., Mann, G., Marsch, E., Posner, A., Richardson, I.G., Schmidt, J.M., Scholer, M., Wang, Y.-M., Wimmer-Schweingruber, R.F., Aellig, M.R., Bochsler, P., Hefti, S., and Mikić, Z.

Abstract

Corotating Interaction Regions (CIRs) form as a consequence of the compression of the solar wind at the interface between fast speed streams and slow streams. Dynamic interaction of solar wind streams is a general feature of the heliospheric medium; when the sources of the solar wind streams are relatively stable, the interaction regions form a pattern which corotates with the Sun. The regions of origin of the high speed solar wind streams have been clearly identified as the coronal holes with their open magnetic field structures. The origin of the slow speed solar wind is less clear; slow streams may well originate from a range of coronal configurations adjacent to, or above magnetically closed structures. This article addresses the coronal origin of the stable pattern of solar wind streams which leads to the formation of CIRs. In particular, coronal models based on photospheric measurements are reviewed; we also examine the observations of kinematic and compositional solar wind features at 1 AU, their appearance in the stream interfaces (SIs) of CIRs, and their relationship to the structure of the solar surface and the inner corona; finally we summarise the Helios observations in the inner heliosphere of CIRs and their precursors to give a link between the optical observations on their solar origin and the in-situ plasma observations at 1 AU after their formation. The most important question that remains to be answered concerning the solar origin of CIRs is related to the origin and morphology of the slow solar wind.

Published
2006

43. Derivative chameleons

Author

Noller, Johannes [Theoretical Physics, Blackett Laboratory, Imperial College London, Prince Consort Road, London, SW7 2BZ (United Kingdom)]

Published
2012
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