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  • Journal article
    DEWIT TD, KRASNOSELSKIKH VV, BALE SD, DUNLOP MW, LUHR H, SCHWARTZ SJ, WOOLLISCROFT LJCet al., 1995,

    , GEOPHYSICAL RESEARCH LETTERS, Vol: 22, Pages: 2653-2656, ISSN: 0094-8276
    • Cite
    • Citations: 62
  • Journal article
    MCCOMAS DJ, BARRACLOUGH BL, GOSLING JT, HAMMOND CM, PHILLIPS JL, NEUGEBAUER M, BALOGH A, FORSYTH RJet al., 1995,

    , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 100, Pages: 19893-19902, ISSN: 2169-9380
    • Cite
    • Citations: 62
  • Journal article
    YOSHINO K, ESMOND JR, MURRAY JE, PARKINSON WH, THORNE AP, LEARNER RCM, COX Get al., 1995,

    , JOURNAL OF CHEMICAL PHYSICS, Vol: 103, Pages: 1243-1249, ISSN: 0021-9606
    • Cite
    • Citations: 34
  • Journal article
    FLOWERDEW RJ, HAIGH JD, 1995,

    , GEOPHYSICAL RESEARCH LETTERS, Vol: 22, Pages: 1693-1696, ISSN: 0094-8276
    • Cite
    • Citations: 67
  • Journal article
    Balogh A, Southwood DJ, Forsyth RJ, Horbury TS, Smith EJ, Tsurutani BTet al., 1995,

    , Science, Vol: 268, Pages: 1007-1010, ISSN: 0036-8075

    Magnetic field measurements from the Ulysses space mission overthe south polar regions of the sun showed that the structure and properties of the three-dimensional heliosphere were determined by the fast solar wind flow and magnetic fields from the large coronal holes in the polar regions of the sun. This conclusion applies at the current, minimum phase of the 11-year solar activity cycle. Unexpectedly, the radial component of the magnetic field was independent of latitude. The high-latitude magnetic field deviated significantly from the expected Parker geometry, probably because of large amplitude transverse fluctuations. Low-frequency fluctuations had a high level of variance. The rate of occurrence of discontinuities also increased significantly at high latitudes.
  • Journal article
    BALOGH A, SMITH EJ, TSURUTANI BT, SOUTHWOOD DJ, FORSYTH RJ, HORBURY TSet al., 1995,

    , SCIENCE, Vol: 268, Pages: 1007-1010, ISSN: 0036-8075
    • Cite
    • Citations: 261
  • Journal article
    HAMMOND CM, CRAWFORD GK, GOSLING JT, KOJIMA H, PHILLIPS JL, MATSUMOTO H, BALOGH A, FRANK LA, KOKUBUN S, YAMAMOTO Tet al., 1995,

    , GEOPHYSICAL RESEARCH LETTERS, Vol: 22, Pages: 1169-1172, ISSN: 0094-8276
    • Cite
    • Citations: 20
  • Journal article
    PICKERING JC, SEMENIUK JI, 1995,

    , MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Vol: 274, Pages: L37-L42, ISSN: 0035-8711
    • Cite
    • Citations: 12
  • Journal article
    SOUTHWOOD D, 1995,

    , NATURE, Vol: 375, Pages: 10-10, ISSN: 0028-0836
  • Journal article
    HAMMOND CM, FELDMAN WC, PHILLIPS JL, GOLDSTEIN BE, BALOGH Aet al., 1995,

    , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 100, Pages: 7881-7889, ISSN: 2169-9380
    • Cite
    • Citations: 22
  • Journal article
    Blanco-Cano X, Schwartz SJ, 1995,

    , Advances in Space Research, Vol: 15, Pages: 97-101-97-101
  • Journal article
    THOMPSON P, DOUGHERTY MK, SOUTHWOOD DJ, 1995,

    , PLANETARY AND SPACE SCIENCE, Vol: 43, Pages: 625-634, ISSN: 0032-0633
  • Journal article
    Reiner MJ, Anderson KA, Roelof E, Armstrong T, Hospodarsky GB, Fainberg J, Stone RG, Lanzerotti L, Gurnett DA, Phillips JL, Forsyth Ret al., 1995,

    , Space Science Reviews, Vol: 72, Pages: 261-266, ISSN: 0038-6308

    Both the Ulysses and Galileo spacecraft detected energetic electrons and Langmuir waves that were associated with a type III radio burst on 10 December 1990. At the time of these observations, these spacecraft were in the ecliptic plane and separated by 0.4 AU, with Galileo near the Earth at 1 AU and Ulysses at 1.36 AU. From the measured electron arrival times, the propagation path lengths of the electrons to both Ulysses and Galileo were estimated to be significantly longer than the length of the Parker spiral. These long path lengths are interpreted as due to draping of the interplanetary magnetic field lines around a CME. The onset times of the Langmuir waves at Ulysses and Galileo coincided with the estimated arrival time of the 9 keV and 14 keV electrons, respectively. © 1995 Kluwer Academic Publishers.
  • Conference paper
    Phillips JL, Bame SJ, Gary SP, Gosling JT, Scime EE, Forsyth RJet al., 1995,

    , Pages: 109-112, ISSN: 0038-6308

    Ulysses plasma measurement from 1.15 to 5.31 AU and from S6.4° to S48.3° solar latitude are used to assess the trends in the solar wind thermal electron temperature and anisotropy. Improved spacecraft potential corrections and data products have been incorporated. The radial temperature gradient is steeper than in previous determinations, but flatter than adiabatic. When normalized to 1 AU, temperature decrease with increasing latitude. Little change in the average thermal anisotropy has been seen during the mission. © 1995 Kluwer Academic Publishers.
  • Conference paper
    McComas DJ, Gosling JT, Hammond CM, Moldwin MB, Phillips JL, Forsyth RJet al., 1995,

    , Pages: 129-132, ISSN: 0038-6308

    Plasma and magnetic field signatures from 29 November 1990 indicate that the Ulysses spacecraft passed through a series of interplanetary structures that were most likely formed by magnetic reconnection on open field lines ahead of a coronal mass ejection (CME). This reconnection changed the magnetic topology of the upstream region by converting normal open interplanetary magnetic field into a pair of regions: one magnetically disconnected from the Sun and the other, a tongue, connected back to the Sun at both ends. This process provides a new method for producing both heat flux dropouts and counterstreaming suprathermal electron signatures in interplanetary space. In this paper we expand upon the 29 November case study and argue that reconnection ahead of CMEs should be less common at high heliolatitudes. © 1995 Kluwer Academic Publishers.
  • Conference paper
    GOLDSTEIN BE, NEUGEBAUER M, GOSLING JT, BAME SJ, PHILLIPS JL, MCCOMAS DJ, BALOGH Aet al., 1995,

    , Publisher: SPRINGER, Pages: 113-116, ISSN: 0038-6308
    • Cite
    • Citations: 11
  • Conference paper
    SMITH EJ, NEUGEBAUER M, BALOGH A, BAME SJ, LEPPING RP, TSURUTANI BTet al., 1995,

    , Publisher: SPRINGER, Pages: 165-170, ISSN: 0038-6308
    • Cite
    • Citations: 58
  • Conference paper
    KEPPLER E, FRANZ M, KORTH A, KRUPP N, REUSS MK, WILKEN B, BALOGH A, FORSYTH RJ, QUENBY JJ, BLAKE Bet al., 1995,

    , Publisher: SPRINGER, Pages: 285-290, ISSN: 0038-6308
    • Cite
    • Citations: 10
  • Conference paper
    GOSLING JT, BAME SJ, MCCOMAS DJ, PHILLIPS JL, BALOGH A, STRONG KTet al., 1995,

    , Publisher: SPRINGER, Pages: 133-136, ISSN: 0038-6308
    • Cite
    • Citations: 21
  • Conference paper
    RILEY P, SONETT CP, BALOGH A, FORSYTH RJ, SCIME EE, FELDMAN WCet al., 1995,

    , Publisher: SPRINGER, Pages: 197-200, ISSN: 0038-6308
    • Cite
    • Citations: 13
  • Conference paper
    SANDERSON TR, MARSDEN RG, WENZEL KP, BALOGH A, FORSYTH RJ, GOLDSTEIN BEet al., 1995,

    , Publisher: SPRINGER, Pages: 291-296, ISSN: 0038-6308
    • Cite
    • Citations: 17
  • Conference paper
    BALOGH A, GONZALEZESPARZA JA, FORSYTH RJ, BURTON ME, GOLDSTEIN BE, SMITH EJ, BAME SJet al., 1995,

    , Publisher: SPRINGER, Pages: 171-180, ISSN: 0038-6308
    • Cite
    • Citations: 101
  • Conference paper
    REUSS MK, KEPPLER E, FRANZ M, WITTE M, KRUPP N, WILKEN B, BALOGH A, FORSYTH RJ, MOUSSAS X, POLYGIANNAKIS JM, KAKOURIS AD, ALEVIZOS Aet al., 1995,

    , Publisher: SPRINGER, Pages: 343-346, ISSN: 0038-6308
  • Conference paper
    MURPHY N, SMITH EJ, TSURUTANI BT, BALOGH A, SOUTHWOOD DJet al., 1995,

    , Publisher: SPRINGER, Pages: 447-453, ISSN: 0038-6308
    • Cite
    • Citations: 49
  • 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
    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
    FORSYTH RJ, 1995,

    , Publisher: SPRINGER, Pages: 153-163, ISSN: 0038-6308
    • Cite
    • Citations: 16
  • 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
    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
    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.

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