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We study the dependence of Saturn's magnetospheric\udmagnetic field structure on the interplanetary magnetic field (IMF),\udtogether with the corresponding variations of the open-closed field line\udboundary in the ionosphere. Specifically we investigate the interval from 8\udto 30 January 2004, when UV images of Saturn's southern aurora were obtained\udby the Hubble Space Telescope (HST), and simultaneous interplanetary\udmeasurements were provided by the Cassini spacecraft located near the\udecliptic ~0.2 AU upstream of Saturn and ~0.5 AU off the\udplanet-Sun line towards dawn. Using the paraboloid model of Saturn's\udmagnetosphere, we calculate the magnetospheric magnetic field structure for\udseveral values of the IMF vector representative of interplanetary\udcompression regions. Variations in the magnetic structure lead to different\udshapes and areas of the open field line region in the ionosphere. Comparison\udwith the HST auroral images shows that the area of the computed open flux\udregion is generally comparable to that enclosed by the auroral oval, and\udsometimes agrees in detail with its poleward boundary, though more typically\udbeing displaced by a few degrees in the tailward direction

annales geophysicae

IMF dependence of the open-closed field line boundary in Saturn's ionosphere, and its relation to the UV auroral oval observed by the Hubble Space Telescope