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29 results on '"McKibben, R.B."'

4. The Sun and heliosphere at solar maximum

Author

Smith, E.J., Marsden, R.G., Balogh, A., Gloeckler, G., Geiss, J., McComas, D.J., McKibben, R.B., MacDowall, R.J., Lanzerotti, L.J., Krupp, N., Krueger, H., and Landgraf, M.

Subjects
Geophysics -- Research, Sun -- Observations -- Research, Solar wind -- Research, Science and technology, Observations, Research
Abstract

Recent Ulysses observations from the Sun's equator to the poles reveal fundamental properties of the three-dimensional heliosphere at the maximum in solar activity. The heliospheric magnetic field originates from a magnetic dipole oriented nearly perpendicular to, instead of nearly parallel to, the Sun's rotation axis. Magnetic fields, solar wind, and energetic charged particles from low-latitude sources reach all latitudes, including the polar caps. The very fast high-latitude wind and polar coronal holes disappear and reappear together. Solar wind speed continues to be inversely correlated with coronal temperature. The cosmic ray flux is reduced symmetrically at all latitudes., The space between the Sun and nearby stars is filled with ionized and neutral gas, dust, magnetic fields, and charged particles. The Sun excludes this pristine interstellar medium from a [...]

Published
2003

8. Corotating Interaction Regions at High Latitudes

Author

Kunow, H., Lee, M.A., Fisk, L.A., Forsyth, R.J., Heber, B., Horbury, T.S., Keppler, E., Kóta, J., Lou, Y.-Q., McKibben, R.B., Paizis, C., Potgieter, M.S., Roelof, E.C., Sanderson, T.R., Simnett, G.M., Von Steiger, R., Tsurutani, B.T., Wimmer-Schweingruber, R.F., and Jokipii, J.R.

Published
1999
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9. Anomalous Cosmic Rays

Author

Klecker, B., Mewaldt, R.A., Bieber, J.W., Cummings, A.C., Drury, L., Giacalone, J., Jokipii, J.R., Jones, F.C., Krainev, M.B., Lee, M.A., Le Roux, J.A., Marsden, R.G., Mcdonald, F.B., McKibben, R.B., Steenberg, C.D., Baring, M.G., Ellison, D.C., Lanzerotti, L.J., Leske, R.A., Mazur, J.E., Moraal, H., Oetliker, M., Ptuskin, V.S., Selesnick, R.S., and Trattner, K.J.

Published
1998
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12. Cosmic ray and solar particle investigations over the south polar regions of the sun

Author

Simpson, J.A., Anglin, J.D., Bothmer, V., Connell, J.J., Ferrando, P., Heber, B., Kunow, H., Lopate, C., Marsden, R.G., McKibben, R.B., Muller-Mellin, R., Paizis, C., Rastoin, C., Raviart, A., Sanderson, T.R., Sierks, H., Trattner, K.J., Wenzel, K.-P., Wibberenz, G., and Zhang, M.

Subjects
Ulysses (Space probe) -- Observations, Sun -- Observations, Cosmic rays -- Observations, Science and technology, Observations
Abstract

Observations of galactic cosmic radiation and anomalous component nuclei with charged particle sensors on the Ulysses spacecraft showed that heliospheric magnetic field structure over the south solar pole does not permit substantially more direct access to the local interstellar cosmic ray spectrum than is possible in the equatorial zone. Fluxes of galactic cosmic rays and the anomalous component increased as a result of latitude gradients by less than 50% from the equator to -80°. Thus, the modulated cosmic ray nucleon, electron, and anomalous component fluxes are nearly spherically symmetric in the inner solar system. The cosmic rays and the anomalous nuclear component underwent a continuous, 26 day recurrent modulation to -80.2°, whereas all recurring magnetic field compressions and recurring streams in the solar wind disappeared above 55°S latitude., The heliosphere is the region of space in the local galactic arm that encompasses the solar system and is dominated by plasmas and magnetic fields originating at the sun. Within [...]

Published
1995

13. Energetic charged-particle phenomena in the Jovian magnetosphere: first results from the Ulysses COSPIN collaboration

Author

Simpson, J.A., Anglin, J.D., Balogh, A., Burrows, J.R., Cowley, S.W.H., Ferrando, P., Heber, B., Hynds, R.J., Kunow, H., Marsden, R.G., McKibben, R.B., Muller-Mellin, R., Page, D.E., Raviart, A., Sanderson, T.R., Staines, K., Wenzel, K.-P., Wilson, Margaret D., and Zhang, M.

Subjects
Ulysses (Space probe) -- Observations, Jupiter (Planet) -- Atmosphere, Magnetosphere -- Research, Interplanetary medium -- Research, Particles (Nuclear physics) -- Research, Science and technology, Observations, Research
Abstract

The Ulysses spacecraft made the first exploration of the region of Jupiter's magnetosphere at high Jovigraphic latitudes ([unkeyable] 37 ° south) on the dusk side and reached higher magnetic latitudes ([unkeyable] 49 ° north) on the day side than any previous mission to Jupiter. The cosmic and solar particle investigations (COSPIN) instrumentation achieved a remarkably well integrated set of observations of energetic charged particles in the energy ranges of [unkeyable] 1 to 170 megaelectron volts for electrons and 0.3 to 20 megaelectron volts for protons and heavier nuclei. The new findings include (i) an apparent polar cap region in the northern hemisphere in which energetic charged particles following Jovian magnetic field lines may have direct access to the interplanetary medium, (ii) high-energy electron bursts (rise times [is less than or equal to] 1 minute and energies extending to > [unkeyable] 17 megaelectron volts) on the dusk side that are apparently associated with field-aligned currents and radio burst emissions, (iii) persistence of the global 10-hour relativistic electron 'clock' phenomenon throughout Jupiter's magnetosphere, (iv) on the basis of charged-particle measurements, apparent dragging of magnetic field lines at large radii in the dusk sector toward the tail, and (v) consistent outflow of megaelectron volt electrons and large- scale departures from corotation for nucleons., Measurements of the population of high-energy electrons, protons, and heavier nuclei in Jupiter's magnetic field are essential for understanding the energetic and dynamic processes that govern the Jovian magnetosphere. For [...]

Published
1992

19. 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

20. 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

23. Characterization of SEP events at high heliographic latitudes.

Author

Dalla, S., Balogh, A., Krucker, S., Posner, A., Müller-Mellin, R., Anglin, J.D., Hofer, M.Y., Marsden, R.G., Sanderson, T.R., Heber, B., Zhang, M., and McKibben, R.B.

Subjects
SOLAR energy, PARTICLES (Nuclear physics), HELIOSPHERE
Abstract

Between February 2000 and May 2002, the Ulysses spacecraft made the first ever measurements of solar energetic particles (SEPs) at high heliographic latitudes. Nine large gradual SEP events were detected at latitudes greater than 45°, their signatures being clearest at high particle energies, i.e. protons >30 MeV and electrons >0.1 MeV. In this paper we measure the onset times of Ulysses high latitude events in several energy channels, and plot them versus inverse particle speed. We repeat the procedure for near Earth observations by Wind and SOHO. Velocity dispersion is observed in all the events near Earth and in most of them at Ulysses. The plots of onset times versus inverse speed allow to derive an experimental path length and time of release from the solar atmosphere. We find that the derived path lengths at Ulysses are longer than the length of a Parker spiral magnetic field line connecting it to the Sun, by a factor between 1.2–2.7. The time of particle release from the Sun is typically between 100 and 200 mins later than the relase time derived from in-ecliptic measurements. Unlike near Earth observations, Ulysses measurements are therefore not compatible with scatter-free propagation from the Sun to the spacecraft. © 2003 American Institute of Physics [ABSTRACT FROM AUTHOR]

Published
2003
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29. Accelerator test of an angle detecting inclined sensor (ADIS) prototype with beams of 48Ca and fragments

Author

Connell, J.J., Lopate, C., McKibben, R.B., and Enman, A.

Subjects
*ACCELERATION principle (Economics), *PROTOTYPES, *SOLAR energetic particles, *COSMIC rays, *HELIOSPHERE, *SPACE vehicles, *METEOROLOGICAL satellites
Abstract

Abstract: The measurement of cosmic rays and Solar energetic particles in space is basic to our understanding of the Galaxy, the Sun, phenomena in the Heliosphere and what has come to be known broadly as “space weather”. For these reasons, cosmic ray instruments are common on both scientific spacecraft and operational spacecraft such as weather satellites. The resource constraints on spacecraft generally mean that instruments that measure cosmic rays and Solar energetic particles must have low mass (a few kg) and low power (a few W), be robust and reliable yet still highly capable. Such instruments must identify ionic species (at least by element, preferably by isotope) from protons through the iron group. The charge and mass resolution of heavy ion instruments in space depends upon determining ions’ angles of incidence. The Angle Detecting Inclined Sensor (ADIS) system is a highly innovative and uniquely simple detector configuration used to determine the angle of incidence of heavy ions in space instruments. ADIS replaces complex position sensing detectors (PSDs) with a system of simple, reliable and robust Si detectors inclined at an angle to the instrument axis. In August 2004, we tested ADIS prototypes with a 48Ca beam at the National Superconducting Cyclotron Laboratory''s (NSCL) Coupled Cyclotron Facility (CCF). Among the analyses performed on the data taken at the NSCL, we demonstrate that our prototype design with an ADIS system has a charge resolution of less than 0.25e. We also present a more generalized analytic derivation of instrument response and report on the corresponding analysis of Monte-Carlo modeling data. [Copyright &y& Elsevier]

Published
2007
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