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The SEGMA array: current status M. Vellante Physics Department, University of L’Aquila, Italy

The SEGMA array: current status M. Vellante Physics Department, University of L’Aquila, Italy. ULTIMA Meeting Tsukuba, Japan 14 November 2008. 1. SEGMA: South Europe GeoMagnetic Array. Cooperating institutions: University of L’Aquila, Italy

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The SEGMA array: current status M. Vellante Physics Department, University of L’Aquila, Italy

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  1. The SEGMA array: current status M. Vellante Physics Department, University of L’Aquila, Italy ULTIMA Meeting Tsukuba, Japan 14 November 2008 1

  2. SEGMA: South Europe GeoMagnetic Array • Cooperating institutions: • University of L’Aquila, Italy • Space Research Institute (IWF), Graz, Austria • Geodetic and Geophysical Research Institute, Sopron, Hungary • Geophysical Institute, Sofia, Bulgaria 2

  3. NCK CST RNC PAG AQU Map of the recording stations of the SEGMA array 3

  4. SEGMA array, coordinates of the recording stations 4

  5. Main features of the fluxgate instrument and data acquisition: • 0.01 nT resolution • Max. data rate 64 vectors/sec • Standard final sampling rate: 1Hz • Absolute time via GPS receiver • Check operations and data recovery made frequently at AQU, NCK and PAG. Once every 1-2 months at CST and RNC. 5

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  8. From the WEB site of SEGMA it is possible to get: • user defined magnetograms: http://sole-terra.aquila.infn.it/dati.asp?lang=en • example plot • cross-phase spectra (daily and monthly vision): • http://sole-terra.aquila.infn.it/cross-phase-spectra.asp?lang=en • example 8

  9. Scientific objectives • General purpose: • Investigation of the dynamical features of the solar wind – magnetosphere interaction. • Ground support to space missions. • Specific objectives: • Understanding of generation mechanisms of ULF waves in the magnetosphere, • relation with solar wind conditions. • Understanding of propagation characteristics of ULF waves, • transformation they undergo in the magnetosphere (resonances) and • in the transmission through the ionosphere. • Study of connection between Pi2 pulsations and geomagnetic substorms. • Monitoring of plasma mass density in the plasmasphere and ionosphere by means of • detection of field line resonances. 9

  10. Thank you for your attention 10

  11. back 11

  12. back 12

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