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• Journal article
  Archer MO, Turner DL, Eastwood JP, Horbury TS, Schwartz SJet al., 2014,
  , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 119, Pages: 8117-8125, ISSN: 2169-9380
  • Cite
  • Citations: 50
• Journal article
  Slavin JA, DiBraccio GA, Gershman DJ, Imber SM, Poh GK, Raines JM, Zurbuchen TH, Jia X, Baker DN, Glassmeier K-H, Livi SA, Boardsen SA, Cassidy TA, Sarantos M, Sundberg T, Masters A, Johnson CL, Winslow RM, Anderson BJ, Korth H, McNutt RL, Solomon SCet al., 2014,
  , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 119, Pages: 8087-8116, ISSN: 2169-9380
  • Cite
  • Citations: 130
• Journal article
  Rieutord M, Beth A, 2014,
  , ASTRONOMY & ASTROPHYSICS, Vol: 570, ISSN: 0004-6361
  • Cite
  • Citations: 9
• Journal article
  Jinks SL, Bunce EJ, Cowley SWH, Provan G, Yeoman TK, Arridge CS, Dougherty MK, Gurnett DA, Krupp N, Kurth WS, Mitchell DG, Morooka M, Wahlund J-Eet al., 2014,
  , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 119, Pages: 8161-8177, ISSN: 2169-9380
  • Cite
  • Citations: 32
• Journal article
  Moore L, O'Donoghue J, Mueller-Wodarg I, Galand M, Mendillo Met al., 2014,
  , Icarus, Vol: 245, Pages: 355-366, ISSN: 0019-1035
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• Journal article
  Gryspeerdt E, Stier P, Partridge DG, 2014,
  , Atmospheric Chemistry and Physics, Vol: 14, Pages: 9677-9694, ISSN: 1680-7324
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• Journal article
  Ball WT, Mortlock DJ, Egerton JS, Haigh JDet al., 2014,
  , JOURNAL OF SPACE WEATHER AND SPACE CLIMATE, Vol: 4, ISSN: 2115-7251
  • Cite
  • Citations: 7
• Journal article
  Varsani A, Owen CJ, Fazakerley AN, Forsyth C, Walsh AP, Andre M, Dandouras I, Carr CMet al., 2014,
  , ANNALES GEOPHYSICAE, Vol: 32, Pages: 1093-1117, ISSN: 0992-7689
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• Journal article
  Provan G, Lamy L, Cowley SWH, Dougherty MKet al., 2014,
  , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 119, ISSN: 2169-9380
  • Cite
  • Citations: 44
• Journal article
  Newton B, Cowie S, Rijks D, Banks J, Brindley H, Marsham JHet al., 2014,
  , BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY, Vol: 95, Pages: 1325-1328, ISSN: 0003-0007
  • Cite
  • Citations: 3
• Journal article
  Cheung JCH, Haigh JD, Jackson DR, 2014,
  , JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES, Vol: 119, Pages: 9253-9266, ISSN: 2169-897X
  • Cite
  • Citations: 27
• Journal article
  Yang YY, Shen C, Zhang YC, Rong ZJ, Li X, Dunlop M, Ma YH, Liu ZX, Carr CM, Reme Het al., 2014,
  , Journal of Geophysical 91��ɫ: Space Physics, Vol: 119, Pages: 6327-6341, ISSN: 2169-9402

  Unambiguous knowledge of magnetic field structure and the electric current distribution is critical for understanding the origin, evolution, and related dynamic properties of magnetic flux ropes (MFRs). In this paper, a survey of 13 MFRs in the Earth's magnetotail are conducted by Cluster multipoint analysis, so that their force-free feature, i.e., the kind of magnetic field structure satisfying J × B = 0, can be probed directly. It is showed that the selected flux ropes with the bipolar signature of the south-north magnetic field component generally lie near the equatorial plane, as expected, and that the magnetic field gradient is rather weak near the axis center, where the curvature radius is large. The current density (up to several tens of nA/m2) reaches their maximum values as the center is approached. It is found that the stronger the current density, the smaller the angles between the magnetic field and current in MFRs. The direct observations show that only quasi force-free structure is observed, and it tends to appear in the low plasma beta regime (in agreement with the theoretic results). The quasi force-free region is generally found to be embedded in the central portion of the MFRs, where the current is approximately field aligned and proportional to the strength of core field. It is shown that ~60% of surveyed MFRs can be globally approximated as force free. The force-free factor α is found to be nonconstantly varied through the quasi force-free MFR, suggesting that the force-free structure is nonlinear.

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• Journal article
  Pulupa MP, Salem C, Phan TD, Gosling JT, Bale SDet al., 2014,
  , ASTROPHYSICAL JOURNAL LETTERS, Vol: 791, ISSN: 2041-8205
  • Cite
  • Citations: 12
• Journal article
  Oieroset M, Sundkvist D, Chaston CC, Phan TD, Mozer FS, McFadden JP, Angelopoulos V, Andersson L, Eastwood JPet al., 2014,
  , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 119, ISSN: 2169-9380
  • Cite
  • Citations: 30
• Journal article
  Reveret V, de la Broise X, Fermon C, Pannetier-Lecoeur M, Pigot C, Rodriguez L, Sauvageot J-L, Jin Y, Marnieros S, Bouchier D, Putzeys J, Long Y, Kiss C, Kiraly S, Barbera M, Lo Cicero U, Brown P, Carr C, Whiteside Bet al., 2014,
  , JOURNAL OF LOW TEMPERATURE PHYSICS, Vol: 176, Pages: 446-452, ISSN: 0022-2291
  • Cite
  • Citations: 9
• Journal article
  Landi S, Matteini L, Pantellini F, 2014,
  , ASTROPHYSICAL JOURNAL LETTERS, Vol: 790, ISSN: 2041-8205
  • Cite
  • Citations: 26
• Journal article
  Alconcel LNS, Fox P, Brown P, Oddy TM, Lucek EL, Carr CMet al., 2014,
  , GEOSCIENTIFIC INSTRUMENTATION METHODS AND DATA SYSTEMS, Vol: 3, Pages: 95-109, ISSN: 2193-0856
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• Journal article
  Ruffoni MP, Den Hartog EA, Lawler JE, Brewer NR, Lind K, Nave G, Pickering JCet al., 2014,
  , Monthly Notices of the Royal Astronomical Society, Vol: 441, Pages: 3127-3136, ISSN: 0035-8711

  The Gaia-ESO Public Spectroscopic Survey (GES) is conducting a large-scale study of multi-element chemical abundances of some 100 000 stars in the Milky Way with the ultimate aim of quantifying the formation history and evolution of young, mature and ancient Galactic populations. However, in preparing for the analysis of GES spectra, it has been noted that atomic oscillator strengths of important Fe I lines required to correctly model stellar line intensities are missing from the atomic data base. Here, we present new experimental oscillator strengths derived from branching fractions and level lifetimes, for 142 transitions of Fe I between 3526 and 10 864 Å, of which at least 38 are urgently needed by GES. We also assess the impact of these new data on solar spectral synthesis and demonstrate that for 36 lines that appear unblended in the Sun, Fe abundance measurements yield a small line-by-line scatter (0.08 dex) with a mean abundance of 7.44 dex in good agreement with recent publications.

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• Journal article
  Masters A, 2014,
  , Journal of Geophysical 91��ɫ: Space Physics, Vol: 119, Pages: 5520-5538, ISSN: 2169-9380

  The magnetosphere of Uranus has barely been explored by spacecraft but is distinct from other solar system magnetospheres in many respects. Determining how this magnetosphere is coupled to the solar wind is central to understanding energy flow through the system. Here we assess how the solar wind interacts with the Uranian magnetosphere via magnetic reconnection. Analytical models of conditions at the magnetopause are combined with current understanding of reconnection onset to predict where reconnection may occur on the boundary. The results suggest that conditions at Uranus' magnetopause are generally less favorable for reconnection than those at the magnetopause of any planet closer to the Sun, as a result of how typical solar wind parameters vary with heliocentric distance. The location of reconnection sites on the Uranian magnetopause is likely to be highly dependent on not only the interplanetary magnetic field orientation but also planetary longitude and season. Solar wind–magnetosphere coupling via magnetic reconnection may be stronger under near‐solstice conditions than under near‐equinox conditions. We discuss the typical reconnection electric field strength at Uranus' magnetopause and suggest that the typical reconnection voltage is considerably less than 40 kV. Complimentary assessments of other means of coupling to the solar wind (e.g., via a “viscous‐like” interaction) are needed to establish the overall nature of solar wind–magnetosphere coupling at Uranus.

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• Journal article
  Sulaiman AH, Masters A, Dougherty MK, Jia Xet al., 2014,
  , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 119, Pages: 5651-5661, ISSN: 2169-9380
  • Cite
  • Citations: 21
• Journal article
  McAndrews HJ, Thomsen MF, Arridge CS, Jackman CM, Wilson RJ, Henderson MG, Tokar RL, Khurana KK, Sittler EC, Coates AJ, Dougherty MKet al., 2014,
  , PLANETARY AND SPACE SCIENCE, Vol: 97, Pages: 86-87, ISSN: 0032-0633
  • Cite
  • Citations: 5
• Journal article
  Jackman CM, Slavin JA, Kivelson MG, Southwood DJ, Achilleos N, Thomsen MF, DiBraccio GA, Eastwood JP, Freeman MP, Dougherty MK, Vogt MFet al., 2014,
  , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 119, Pages: 5465-5494, ISSN: 2169-9380
  • Cite
  • Citations: 67
• Journal article
  Selzer LA, Hnat B, Osman KT, Nakariakov VM, Eastwood JP, Burgess Det al., 2014,
  , ASTROPHYSICAL JOURNAL LETTERS, Vol: 788, ISSN: 2041-8205
  • Cite
  • Citations: 5
• Journal article
  Owens MJ, Horbury TS, Wicks RT, McGregor SL, Savani NP, Xiong Met al., 2014,
  , Space Weather, Vol: 12, Pages: 395-405, ISSN: 1539-4956

  Advanced forecasting of space weather requires simulation of the whole Sun-to-Earth system, which necessitates driving magnetospheric models with the outputs from solar wind models. This presents a fundamental difficulty, as the magnetosphere is sensitive to both large-scale solar wind structures, which can be captured by solar wind models, and small-scale solar wind “noise,” which is far below typical solar wind model resolution and results primarily from stochastic processes. Following similar approaches in terrestrial climate modeling, we propose statistical “downscaling” of solar wind model results prior to their use as input to a magnetospheric model. As magnetospheric response can be highly nonlinear, this is preferable to downscaling the results of magnetospheric modeling. To demonstrate the benefit of this approach, we first approximate solar wind model output by smoothing solar wind observations with an 8 h filter, then add small-scale structure back in through the addition of random noise with the observed spectral characteristics. Here we use a very simple parameterization of noise based upon the observed probability distribution functions of solar wind parameters, but more sophisticated methods will be developed in the future. An ensemble of results from the simple downscaling scheme are tested using a model-independent method and shown to add value to the magnetospheric forecast, both improving the best estimate and quantifying the uncertainty. We suggest a number of features desirable in an operational solar wind downscaling scheme.

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• Journal article
  Hietala H, Eastwood JP, Isavnin A, 2014,
  , PLASMA PHYSICS AND CONTROLLED FUSION, Vol: 56, ISSN: 0741-3335
  • Cite
  • Citations: 17
• Journal article
  Miller RL, Schmidt GA, Nazarenko LS, Tausnev N, Bauer SE, DelGenio AD, Kelley M, Lo KK, Ruedy R, Shindell DT, Aleinov I, Bauer M, Bleck R, Canuto V, Chen Y, Cheng Y, Clune TL, Faluvegi G, Hansen JE, Healy RJ, Kiang NY, Koch D, Lacis AA, LeGrande AN, Lerner J, Menon S, Oinas V, Garcia-Pando CP, Perlwitz JP, Puma MJ, Rind D, Romanou A, Russell GL, Sato M, Sun S, Tsigaridis K, Unger N, Voulgarakis A, Yao M-S, Zhang Jet al., 2014,
  , JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS, Vol: 6, Pages: 441-477
  • Cite
  • Citations: 136
• Journal article
  Marlier ME, Voulgarakis A, Shindell DT, Faluvegi G, Henry CL, Randerson JTet al., 2014,
  , ATMOSPHERIC ENVIRONMENT, Vol: 89, Pages: 158-168, ISSN: 1352-2310
  • Cite
  • Citations: 12
• Journal article
  Gryspeerdt E, Stier P, Grandey BS, 2014,
  , GEOPHYSICAL RESEARCH LETTERS, Vol: 41, Pages: 3622-3627, ISSN: 0094-8276
  • Cite
  • Citations: 44
• Journal article
  Nichols JD, Badman SV, Baines KH, Brown RH, Bunce EJ, Clarke JT, Cowley SWH, Crary FJ, Dougherty MK, Gerard J-C, Grocott A, Grodent D, Kurth WS, Melin H, Mitchell DG, Pryor WR, Stallard TSet al., 2014,
  , Geophysical 91��ɫ Letters, Vol: 41, Pages: 3323-3330, ISSN: 1944-8007

  We present observations of significant dynamics within two UV auroral storms observedon Saturn using the Hubble Space Telescope in April/May 2013. Specifically, we discuss bursts of auroralemission observed at the poleward boundary of a solar wind-induced auroral storm, propagating at ∼330%rigid corotation from near ∼01 h LT toward ∼08 h LT. We suggest that these are indicative of ongoing, burstyreconnection of lobe flux in the magnetotail, providing strong evidence that Saturn’s auroral storms arecaused by large-scale flux closure. We also discuss the later evolution of a similar storm and show that theemission maps to the trailing region of an energetic neutral atom enhancement. We thus identify the auroralform with the upward field-aligned continuity currents flowing into the associated partial ring current.

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• Journal article
  Simon S, Saur J, van Treeck SC, Kriegel H, Dougherty MKet al., 2014,
  , GEOPHYSICAL RESEARCH LETTERS, Vol: 41, Pages: 3359-3366, ISSN: 0094-8276
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  • Citations: 14

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