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  • Journal article
    TSURUTANI BT, SMITH EJ, HO CM, NEUGEBAUER M, GOLDSTEIN BE, MOK JSet al., 1995,

    , SPACE SCIENCE REVIEWS, Vol: 72, Pages: 205-210, ISSN: 0038-6308
    • Cite
    • Citations: 24
  • Conference paper
    WINTERHALTER D, NEUGEBAUER M, GOLDSTEIN BE, SMITH EJ, TSURUTANI BT, BAME SJ, BALOGH Aet al., 1995,

    , Publisher: SPRINGER, Pages: 201-204, ISSN: 0038-6308
    • Cite
    • Citations: 58
  • Conference paper
    MCCOMAS DJ, GOSLING JT, HAMMOND CM, MOLDWIN MB, PHILLIPS JL, FORSYTH RJet al., 1995,

    , Publisher: SPRINGER, Pages: 129-132, ISSN: 0038-6308
  • Conference paper
    MCKIBBEN RB, SIMPSON JA, ZHANG M, BAME S, BALOGH Aet al., 1995,

    , Publisher: SPRINGER, Pages: 403-408, ISSN: 0038-6308
    • Cite
    • Citations: 45
  • Conference paper
    SCIME EE, BAME SJ, PHILLIPS JL, BALOGH Aet al., 1995,

    , Publisher: SPRINGER, Pages: 105-108, ISSN: 0038-6308
  • Conference paper
    GOLDSTEIN BE, NEUGEBAUER M, GOSLING JT, BAME SJ, PHILLIPS JL, MCCOMAS DJ, BALOGH Aet al., 1995,

    Ulysses observations of solar wind plasma parameters in the ecliptic from 1.4 to 5.4 AU and out of the ecliptic

    , 28th ESLAB Symposium - The High Latitude Heliosphere, Pages: 113-116

    We report observations of radial and latitudinal gradients of Ulysses plasma parameters. The solar wind velocity increased rapidly with latitude from 0 degrees to 35 degrees, then remained approximately constant at higher latitudes. Solar wind density decreased rapidly from 0 degrees to 35 degrees of latitude, and also was approximately constant beyond that latitude. The mass flux similarly decreased away from the equator (but less than the density), whereas the momentum flux was relatively constant. The radial gradient of the entropy at high latitude indicated a value for the polytrope index of about 1.72 (close to adiabatic); the in-ecliptic estimates of radial gradients for temperature and entropy may be biased by temporal variation. A striking increase in the alpha particle-proton velocity difference with latitude is found.
  • Conference paper
    GOSLING JT, BAME SJ, MCCOMAS DJ, PHILLIPS JL, BALOGH A, STRONG KTet al., 1995,

    Coronal mass ejections at high heliographic latitudes: Ulysses

    , 28th ESLAB Symposium - The High Latitude Heliosphere, Pages: 133-136

    Nine coronal mass ejections (CMEs) have been detected in the solar wind by the Ulysses plasma experiment between 31 degrees and 61 degrees South. One of these events, which was also a magnetic cloud, was directly associated with an event observed by the soft X-ray telescope on Yohkoh in which large magnetic loops formed in the solar corona directly beneath Ulysses. This association suggests that the flux rope topology of the magnetic cloud resulted from reconnection between the ''legs'' of neighboring magnetic loops within the rising CME. The average CME speed (similar to 740 km s(-1)) at these latitudes was comparable to that of the normal solar wind there and is much greater than average CME speeds observed either in the solar wind in the ecliptic plane or in the corona close to the Sun. We suggest that the same basic acceleration process applies to both slow CMEs and the normal solar wind at any latitude.
  • Conference paper
    SOLOMON J, CORNILLEAUWEHRLIN N, CANU P, LENGYELFREY D, BAME SJ, SCIME EE, BALOGH A, FORSYTH Ret al., 1995,

    , Publisher: SPRINGER, Pages: 181-184, ISSN: 0038-6308
  • Conference paper
    FORSYTH RJ, 1995,

    , Publisher: SPRINGER, Pages: 153-163, ISSN: 0038-6308
    • Cite
    • Citations: 16
  • Conference paper
    MACDOWALL RJ, DESCH MD, KAISER ML, STONE RG, HESS RA, BALOGH A, BAME SJ, GOLDSTEIN BEet al., 1995,

    , Publisher: SPRINGER, Pages: 125-128, ISSN: 0038-6308
  • Conference paper
    PHILLIPS JL, BAME SJ, GARY SP, GOSLING JT, SCIME EE, FORSYTH RJet al., 1995,

    , Publisher: SPRINGER, Pages: 109-112, ISSN: 0038-6308
    • Cite
    • Citations: 26
  • Journal article
    EVANS SJ, HAIGH JD, 1995,

    , GEOPHYSICAL RESEARCH LETTERS, Vol: 22, Pages: 695-698, ISSN: 0094-8276
  • Journal article
    BUTTIGHOFFER A, PICK M, ROELOF EC, HOANG S, MANGENEY A, LANZEROTTI LJ, FORSYTH RJ, PHILLIPS JLet al., 1995,

    , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 100, Pages: 3369-3381, ISSN: 2169-9380
    • Cite
    • Citations: 17
  • Journal article
    RUZMAIKIN AA, FEYNMAN J, GOLDSTEIN BE, SMITH EJ, BALOGH Aet al., 1995,

    , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 100, Pages: 3395-3403, ISSN: 2169-9380
    • Cite
    • Citations: 82
  • Journal article
    Pantellini FGE, Schwartz SJ, 1995,

    , \jgr, Vol: 100, Pages: 3539-3549-3539-3549
  • Journal article
    LEAMON RJ, DOUGHERTY MK, SOUTHWOOD DJ, HAYNES PLet al., 1995,

    , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 100, Pages: 1829-1835, ISSN: 2169-9380
    • Cite
    • Citations: 10
  • Conference paper
    BALOGH A, 1995,

    , 14th European Cosmic Ray Symposium (14th ECRS) - Cosmic Rays 94: Solar, Heliospheric, Astrophysical and High-Energy Aspects, Publisher: ELSEVIER, Pages: 69-74, ISSN: 0550-3213
  • Journal article
    Gosling JT, McComas DJ, Phillips JL, Pizzo VJ, Goldstein BE, Forsyth RJ, Lepping RPet al., 1995,

    , Geophysical Research Letters, Vol: 22, Pages: 1753-1756, ISSN: 0094-8276

    A solar wind disturbance produced by a fast coronal mass ejection, CME, that departed from the Sun on Feburary 20, 1994 was observed in the ecliptic plane at 1 AU by IMP 8 and at high heliographic latitudes at 3.53 AU by Ulysses. In the ecliptic the disturbance included a strong forward shock but no reverse shock, while at high latitudes the disturbance was bounded by a relatively weak forwardreverse shock pair. It is clear that the disturbance in the ecliptic plane was driven primarily by the relative speed between the CME and a slower ambient solar wind ahead, whereas at higher latitudes the disturbance was driven by expansion of the CME. The combined IMP 8 and Ulysses observations thus provide a graphic illustration of how a single fast CME can produce very different types of solar wind disturbances at low and high heliographic latitudes. Simple numerical simulations help explain observed differences at the two spacecraft. Copyright 1995 by the American Geophysical Union.
  • Journal article
    ZHONG WY, HAIGH JD, 1995,

    , JOURNAL OF THE ATMOSPHERIC SCIENCES, Vol: 52, Pages: 124-138, ISSN: 0022-4928
    • Cite
    • Citations: 54
  • Journal article
    HORBURY T, BALOGH A, FORSYTH RJ, SMITH EJet al., 1995,

    ULYSSES MAGNETIC-FIELD OBSERVATIONS OF FLUCTUATIONS WITHIN POLAR CORONAL FLOWS

    , ANNALES GEOPHYSICAE-ATMOSPHERES HYDROSPHERES AND SPACE SCIENCES, Vol: 13, Pages: 105-107, ISSN: 0992-7689
    • Cite
    • Citations: 25
  • Journal article
    Pickering JC, Thorne AP, Rosberg M, 1995,

    UV Fourier transform spectroscopy and term analysis of Co I and Co II

    , Laboratory and Astronomical High Resolution Spectra, Vol: 81, Pages: 204-211
  • Conference paper
    Lim TL, Quenby JJ, Reuss MK, Keppler E, Kunow H, Heber B, Forsyth RJet al., 1995,

    Can diffusive shock acceleration work fast enough in interplanetary shocks? Evidence from the November 1992 event

    , Urbino, 24th international cosmic ray conference (xxiv icrc) AUG 28-SEP 08, 1995 ROME, ITALY, Publisher: Argalia Editore Delle Arti Grafiche Editoriali Srl, Pages: 353-356
  • Conference paper
    Leckband JA, Burgess D, Pantellini FGE, Schwartz SJet al., 1995,

    , D2.1 Symposium Symposium of COSPAR Scientific Commission D on Physics of Collisionless Shocks, at the 30th COSPAR Scientific Assembly, Publisher: PERGAMON PRESS LTD, Pages: 345-348, ISSN: 0273-1177
    • Cite
    • Citations: 20
  • Conference paper
    Baring MG, Ogilvie KW, Ellison DC, Forsyth Ret al., 1995,

    , D2.1 Symposium Symposium of COSPAR Scientific Commission D on Physics of Collisionless Shocks, at the 30th COSPAR Scientific Assembly, Publisher: PERGAMON PRESS LTD, Pages: 385-388, ISSN: 0273-1177
  • Journal article
    Schwartz SJ, 1995,

    Hot flow anomalies near the Earth’s bow shock

    , Advances in Space Research, Vol: 15, Pages: 107-116-107-116
  • Journal article
    Leckband JA, Burgess D, Pantellini FGE, Schwartz SJet al., 1995,

    , Advances in Space Research, Vol: 15, Pages: 345-348-345-348
  • Journal article
    Pantellini FGE, Burgess D, Schwartz SJ, 1995,

    , Advances in Space Research, Vol: 15, Pages: 341-344-341-344
  • Journal article
    Chisham G, Burgess D, Schwartz SJ, 1995,

    , Advances in Space Research, Vol: 15, Pages: 141-145-141-145
  • Conference paper
    WANG Z, KIVELSON MG, JOY S, KHURANA KK, POLANSKEY C, SOUTHWOOD DJ, WALKER RJet al., 1995,

    Solar wind interaction with small bodies .1. Whistler wing signatures near Galileo's closest approach to Gaspra and Ida

    , D1 Symposium of COSPAR Scientific Commission D, at the 30th COSPAR Scientific Assembly, Pages: 47-57

    Data from Galileo's two asteroid flybys reveal magnetic fluctuations that ive interpret as perturbations of the solar wind magnetic field caused by an interaction with the nearby asteroid. The scale sizes of the bodies (similar to 14 km for Gaspra and similar to 30 km for Ida) are intermediate between the ion and electron gyroradii, which implies that the asteroid-imposed perturbations propagate in the whistler mode. Special properties of the whistler mode include phase velocities that can exceed the solar wind speed and confinement of the disturbance to directions nearly aligned with the magnetic field. These features of the interaction impose a structure on the solar wind disturbance that differs greatly from the forms familiar for either magnetized or unmagnetized bodies of magnetohydrodynamic spatial scales. We examine both data and computer simulations of the interaction with special attention to what can be inferred about the interaction itself from analysis of the data.
  • Journal article
    Learner RCM, Thorne AP, Murray JE, Semeniuk JIet al., 1995,

    UV Fourier transform spectroscopy of emission line spectra

    , Laboratory and Astronomical High Resolution Spectra, Vol: 81, Pages: 227-228

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