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All issues Volume 9 (2019) J. Space Weather Space Clim., 9 (2019) A3 References
Issue
J. Space Weather Space Clim.
Volume 9, 2019
Planetary Space Weather
Article Number A3
Number of page(s) 11
DOI https://doi.org/10.1051/swsc/2018050
Published online 14 January 2019
  • Auster HU, Apathy I, Berghofer G, Fornacon KH, Remizov A, et al. 2015. The nonmagnetic nucleus of comet 67P/Churyumov-Gerasimenko. Science 349: 6247, aaa5102. DOI: 10.1126/science.aaa5102. [NASA ADS] [CrossRef] [Google Scholar]
  • Balsiger H, Altwegg K, Bochsler P, Eberhardt P, Fischer J, et al. 2007. Rosina – Rosetta orbiter spectrometer for ion and neutral analysis. Space Sci Rev 128: 745–801. DOI: 10.1007/s11214-006-8335-3. [CrossRef] [Google Scholar]
  • Bieler A, Altwegg K, Balsiger H, Belthelier JJ, Calmonte U, et al. 2015. Comparison of 3D kinetic and hydrodynamic models to ROSINA-COPS measurements of the neutral coma of 67P/Churyumov-Gerasimenko. A&A 583: A7. [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  • Boudouridis A, Zesta E, Lyons R, Anderson PC, Lummerzheim D. 2003. Effect of solar wind pressure pulses on the size and strength of the auroral oval. J Geophys Res 108: 8012. DOI: 10.1029/2002JA009373. [CrossRef] [Google Scholar]
  • Clarke JT, Nichols J, Gérard JC, Grodent D, Hansen KC, et al. 2009. Response of Jupiter’s and Saturn’s auroral activity to the solar wind. J Geophys Res 114: A05210. DOI: 10.1029/2008JA013694. [Google Scholar]
  • Crary FJ, Clarke JT, Dougherty MK, Hanlon PG, Hansen KC, et al. 2005. Solar wind dynamic pressure and electric field as the main factors controlling Saturn's aurorae. Nature 433: 720–722. DOI: 10.1038/nature03333. [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
  • Cravens TE. 1986. The physics of the cometary contact surface. In: ESA SP-250: ESLAB Symposium on the Exploration of Halley’s Comet, Battrick B, Rolfe EJ, Reinhard R (Eds.), ESA, Noordwijk, The Netherlands. p. 241. [Google Scholar]
  • Cravens TE. 1987. Theory and observations of cometary ionospheres. Adv Space Res 12: 147–158. [Google Scholar]
  • Cravens TE. 1991. Plasma processes in the inner coma. Int Astron Union Colloq 116: 121. DOI: 10.1017/S0252921100012884. [CrossRef] [Google Scholar]
  • Crider DH, Vignes D, Krymskii AM, Breus TK, Ness NF, et al. 2003. A proxy for determining solar wind dynamic pressure at Mars using Mars Global Surveyor data. J Geophys Res 108(A12): 1461. DOI: 10.1029/2003JA009875. [CrossRef] [Google Scholar]
  • Dósa M, Opitz A, Dálya Z, Szegö K. 2018. Magnetic lasso: an enhanced ballistic solar wind propagation method. Sol Phys 293: 127. DOI: 10.1007/s11207-018-1340-3. [CrossRef] [Google Scholar]
  • Dubinin E, Sauer K, Lundin R, Norberg O, Trotignon JG, et al. 1996. Plasma characteristics of the boundary layer in the Martian magnetosphere. J Geophys Res 101(A12): 27061–27075. DOI: 10.1029/96JA02021. [CrossRef] [Google Scholar]
  • Edberg NJT, Eriksson AI, Odelstad E, Henri P, Lebreton JP, et al. 2015. Spatial distribution of low-energy plasma around comet 67P/CG from Rosetta measurements. Geophys Res Lett 42: 4263–4269. DOI: 10.1002/2015GL064233. [CrossRef] [Google Scholar]
  • Edberg NJT, Alho M, André M, Andrews DJ, Behar E, et al. 2016. CME impact on comet 67P/Churyumov-Gerasimenko. MNRAS 462: S45–S56. DOI: 10.1093/mnras/stw2112. [CrossRef] [Google Scholar]
  • Galand M, Héritier KL, Odelstad E, Henri P, Broiles TW, et al. 2016. Ionospheric plasma of comet 67P probed by Rosetta at 3 AU from the Sun. MNRAS 462: S331–S351. DOI: 10.1093/mnras/stw2891. [CrossRef] [Google Scholar]
  • Galeev AA. 1986. Theory and observations of solar wind/cometary plasma interaction processes. In: ESA Proceedings of the 20th ESLAB Symposium on the Exploration of Halley’s Comet, 27–31 October 1986, Heidelberg, Germany, Vol. 1, pp. 3–17. [Google Scholar]
  • Gan L, Cravens TE. 1990. Electron energetics in the inner coma of comet Halley. J Geophys Res 95(A5): 6285–6303. DOI: 10.1029/JA095iA05p06285. [Google Scholar]
  • Glassmeier KH, Boehnhardt H, Koschny D, Kührt E, Richter I. 2007a. The Rosetta mission: Flying towards the origin of the Solar System. Space Sci Rev 128: 1–21. [CrossRef] [Google Scholar]
  • Glassmeier KH, Richter I, Diedrich A, Musmann G, Auster U, et al. 2007b. RPC-MAG the fluxgate magnetometer in the Rosetta Plasma Consortium. Space Sci Rev 128: 649–670. [CrossRef] [Google Scholar]
  • Glassmeier KH. 2017. Interaction of the solar wind with comets: a Rosetta perspective. Philos Trans Ser A Math Phys Eng Sci 375: 2097. [Google Scholar]
  • Goetz C, Koenders C, Hansen KC, Burch J, Carr C, et al. 2016. Structure and evolution of the diamagnetic cavity at comet 67P/Churyumov–Gerasimenko. MNRAS 462(Suppl_1): S459–S467. DOI: 10.1093/mnras/stw3148. [Google Scholar]
  • Goetz C, Volwerk M, Richter I, Glassmeier KH. 2017. Evolution of the magnetic field at comet 67P/Churyumov-Gerasimenko. MNRAS 469(Suppl_2): S268–S275. [CrossRef] [Google Scholar]
  • Hajra R, Henri P, Vallières X, Moré J, Gilet N, et al. 2018. Dynamic unmagnetized plasma in the diamagnetic cavity around comet 67P/Churyumov–Gerasimenko. MNRAS 475(3): 4140–4147. DOI: 10.1093/mnras/sty094. [NASA ADS] [CrossRef] [Google Scholar]
  • Hansen C, Altwegg K, Berthelier JJ, Bieler A, Biver N, et al. 2016. Evolution of water production of 67P/Churyumov–Gerasimenko: an empirical model and a multi-instrument study. MNRAS 462: S491–S506. DOI: 10.1093/mnras/stw2413. [Google Scholar]
  • Hässig M, Altwegg K, Balsiger H, Bar-Nun A, Berthelier JJ, et al. 2015. Time variability and heterogeneity in the coma of 67P/Churyumov-Gerasimenko. Science 347: aaa0276. [Google Scholar]
  • Ip WH, Axford W. 1987. The formation of a magnetic-field-free cavity at comet Halley. Nature 325: 418. DOI: 10.1038/325418a0. [NASA ADS] [CrossRef] [Google Scholar]
  • Luhmann JG, Elphic RC, Russell CT, Mihalov JD, Wolfe JH. 1980. Observations of large scale steady magnetic fields in the dayside Venus ionosphere. Geophys Res Lett 7: 917–920. DOI: 10.1029/GL007i011p00917. [CrossRef] [Google Scholar]
  • Madanian H, Cravens TE, Rahmati A, Goldstein B, Burch J, et al. 2016a. Suprathermal electrons near the nucleus of comet 67P/Churyumov-Gerasimenko at 3 AU: Model comparisons with Rosetta data. J Geophys Res 121: 5815–5836. DOI: 10.1002/2016JA022610. [CrossRef] [Google Scholar]
  • Madanian H, Cravens TE, Burch J, Goldstein R, Rubin M, et al. 2016b. Plasma environment around comet 67P/Churyumov-Gerasimenko at perihelion: Model comparison with Rosetta data. Astron J 153: 30. DOI: 10.3847/1538-3881/153/1/30. [CrossRef] [Google Scholar]
  • Mandt KE, Eriksson A, Edberg NJT, Koenders C, Broiled T. 2016. RPC observation of the development and evolution of plasma interaction boundaries at 67P/Churyumov-Gerasimenko. MNRAS 462: S9–S22. DOI: 10.1093/mnras/stw1736. [NASA ADS] [CrossRef] [Google Scholar]
  • Mendis DA, Houpis HLF, Marconi ML. 1985. The physics of comets. Fundam Cosm Phys 10(1–4): 380. p. 2. ISSN 0094-5846. [Google Scholar]
  • Nemeth Z, Burch J, Goetz C, Goldstein R, Henri P, et al. 2016. Charged particle signatures of the diamagnetic cavity of comet 67P/Churyumov–Gerasimenko. MNRAS 462(Suppl_1): S415–S421. DOI: 10.1093/mnras/stw3028. [Google Scholar]
  • Neubauer FM, Glassmeier KH, Pohl M, Raeder J, Acuna MH, et al. 1986. First results from the Giotto magnetometer experiment at comet Halley. Nature 321: 352. [NASA ADS] [CrossRef] [Google Scholar]
  • Opitz A, Karrer R, Wurz P, Galvin AB, Bochsler P, et al. 2009. Temporal evolution of the solar wind bulk velocity at solar minimum by correlating the STEREO A and B plastic measurements. Sol Phys 256: 365. DOI: 10.1007/s11207-008-9304-7. [Google Scholar]
  • Richter I, Koenders C, Auster HU, Goetz C, et al. 2015. Observation of a new type of low-frequency waves at comet 67P/Churyumov-Gerasimenko. Ann Geophys 33: 1031–1036. DOI: 10.5194/angeo-33-1031-2015. [CrossRef] [Google Scholar]
  • Sibeck DG, Lopez RE, Roelof EC. 1991. Solar wind control of the magnetopause shape, location, and motion. J Geophys Res 96(A4): 5489–5495. DOI: 10.1029/90JA02464. [CrossRef] [Google Scholar]
  • Timar A, Nemeth Z, Szego K, Dosa M, Opitz A, et al. 2017. Modelling the size of the very dynamic diamagnetic cavity of comet 67P/Churyumov–Gerasimenko. MNRAS 469(Suppl_2): S723–S730. DOI: 10.1093/mnras/stx2628. [Google Scholar]
  • Vennerstrom S, Olsen N, Purucker M, Acuña MH, Cain JC. 2003. The magnetic field in the pile-up region at Mars, and its variation with the solar wind. Geophys Res Lett 30: 1369. DOI: 10.1029/2003GL016883. [CrossRef] [Google Scholar]
  • Vigren E, Altwegg K, Edberg NJT, Eriksson AI, Galand M, et al. 2016. Model-observation comparisons of electron number densities in the coma of 67P/Churyumov-Gerasimenko during 2015 January. Astron J 152: 59 (8 pp). DOI: 10.3847/0004-6256/152/3/59. [CrossRef] [Google Scholar]
  • Vigren E, Eriksson AI. 2017. A 1D model of radial ion motion interrupted by ion-neutral interactions in a cometary coma. Astron J 153: 4. [Google Scholar]
  • Wedlund CS, Alho M, Gronoff G, Kallio E, Gunell H, et al. 2017. Hybrid modelling of cometary plasma environments: I. Impact of photoionisation, charge exchange, and electron ionisation on bow shock and cometopause at 67P/Churyumov-Gerasimenko. A&A 604: A73. DOI: 10.1051/0004-6361/201730514. [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  • Wu ZJ. 1987. Calculation of the shape of the contact surface at comet Halley. In: ESA proceedings of the International Symposium on the Diversity and Similarity of Comets 6–9 April 1987, Brussels, Belgium, 69–73. [Google Scholar]
  • Zieger B, Hansen KC. 2008. Statistical validation of a solar wind propagation model from 1 to 10 AU. J Geophys Res, 113, A08107. DOI: 10.1029/2008JA013046. [NASA ADS] [CrossRef] [Google Scholar]

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