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1
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0001904929
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T. Gehrels, M. S. Matthews, Eds. Univ. of Ariz. Press, Tucson, AZ
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A. W. Schardt et al., Saturn, T. Gehrels, M. S. Matthews, Eds. (Univ. of Ariz. Press, Tucson, AZ, 1984), pp. 417-459.
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(1984)
Saturn
, pp. 417-459
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Schardt, A.W.1
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2
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18644382903
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note
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This velocity was measured by Voyager 1 (3). Ideal corotation would imply a velocity of 200 km/s in Titan's restframe.
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3
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0001405511
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T. Gehrels, M. S. Matthews, Eds. Univ. of Ariz. Press, Tucson, AZ
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F. M. Neubauer, D. A. Gurnett, J. D. Scudder, R. E. Hartle, Saturn, T. Gehrels, M. S. Matthews, Eds. (Univ. of Ariz. Press, Tucson, AZ, 1984), pp. 760-787.
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(1984)
Saturn
, pp. 760-787
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Neubauer, F.M.1
Gurnett, D.A.2
Scudder, J.D.3
Hartle, R.E.4
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4
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18644367207
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note
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Plasma-β: ratio of thermal and magnetic pressure.
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6
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18644381408
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note
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Space Craft Event Time (SCET) in the universal time frame (UTC). All times given here are in this time frame.
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8
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18644374268
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note
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The coordinate system used is the Titan interaction system (TIIS) defined in Fig. 1.
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9
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0002598305
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H. Alfvén, Tellus 9, 92 (1957).
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(1957)
Tellus
, vol.9
, pp. 92
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Alfvén, H.1
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10
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0003186750
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N. F. Ness, M. H. Acuña, K. W. Behannon, F. M. Neubauer, J. Geophys. Res. 87, 1369 (1982).
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(1982)
J. Geophys. Res.
, vol.87
, pp. 1369
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Ness, N.F.1
Acuña, M.H.2
Behannon, K.W.3
Neubauer, F.M.4
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11
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18644376100
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thesis, Institut für Geophysik und Meteorologie, University of Cologne, Germany
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H. Backes, thesis, Institut für Geophysik und Meteorologie, University of Cologne, Germany (2004).
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(2004)
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Backes, H.1
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12
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18644370480
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note
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Several models have been developed to explain Titan's interaction with the saturnian plasma (20, 21, 23-27), which all differ in certain respects.
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15
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2142803437
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Materials and methods are available as supporting material on Science Online.
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Science Online
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16
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18644367961
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note
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A: CA time, 26 October 2004, 15:30:05 UTC; CA altitude, 1174 km; 5LT = 10.6; solar declination, -23.23°; angle between ideal corotation direction and Sun-Titan line, 109.2°; flyby through northern tail.
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22
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18644382531
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note
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The layer between the northern and the southern lobe can have two configurations: In the first, the magnetic field is at a minimum. In this case, it is called a "neutral sheet." In the second, the magnetic field rotates continuously from the field direction in the northern lobe to the field direction in the southern lobe, while the field magnitude is constant. In this case, the expression "neutral sheet" is not appropriate and we call it "polarity reversal layer" instead.
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25
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0003293574
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K. Kabin, T. I. Gombosi, D. L. D. Zeeuw, K. G. Powell, P. L. Israelevich, J. Geophys. Res. 104, 2451 (1999).
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(1999)
J. Geophys. Res.
, vol.104
, pp. 2451
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Kabin, K.1
Gombosi, T.I.2
Zeeuw, D.L.D.3
Powell, K.G.4
Israelevich, P.L.5
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28
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18644365275
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note
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We acknowledge the superb work done by the technical and data processing staff of the MAG team. H.B., F.M.N., and A.W. are supported by the DLR (Germany). M.K.D., C.B., C.S.A., and N. Achilleos are supported by PPARC (UK). N. André is supported by CNES (France). This research was performed while G.H.J. held a National Research Council Research Associateship at the Jet Propulsion Laboratory (JPL). The research at the University of California, Los Angeles, was supported by NASA under a grant administered by JPL.
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