2010-02-11T16:45:24.000Z http://sot.lmsal.com Ted Tarbell LMSAL http://lmsal.com 3251 Hanover Rd, O/ADBS, B/252, Palo Alto, CA, 94304 +1-650-424-2400 tarbell@lmsal.com Hinode SOT Arikawa Sterling Shine(RCO) 117 117 null HOP 117, IBIS POR POR Pore 6 436 -47 0 0 2009-05-06T14:00:00.000Z 2009-05-06T16:01:00.000Z 436 -47 Stokes polarimetry of photosphere and chromosphere. III (DST/IBIS) HOP 117 : Na IVDG and G/Ca 100"x100", 2x2, 32 sec Request to SOT HOP Number 0117 The Hinode Spectro Polarimeter will scan the same region. Hinode???fs narrow and broad band instruments (NFI and BFI respectively) will obtain longitudinal magnetograms and imaging data at a cadence of a tens of seconds, as we did in May 2008. Other Instruments: IBIS, TRACE Scientific Objectives: Science Justification: The justification for our continued work is rooted in the need to examine the free energy in the magnetic field in the Sun's atmosphere. In particular, we wish to try to define the magnetic structure at the coronal base - the upper chromosphere - together with coronal plasma measurements themselves. The need to make measurements now is motivated not only by the availability of IBIS as a new spectropolarimeter but also because we wish to take advantage of the unique Hinode and TRACE observatories while they are still operating well. Justification for additional time: We request a further 14 days of time with the DST/IBIS, combined with Hinode and TRACE, in each of the next two quarters. Of two allocated times for observations (May and December 2008), we were fortunate to obtain excellent quality data on just one day,20 May 2008, owing to atmospheric limitations. Unfortunately the overlap with the Hinode SOT data was only partial (50%), sampling only a small fraction of the region of activity and insufficient to examine reliably the magnetic fields. In this attempt, we hope to reach several new goals: - First, to obtain complete overlap with the Hinode SOT and XRT instruments, - second, to obtain vector magnetic field data of a small region of activity (small spot or pore) sufficient to capture most of the connections of magnetic field lines locally, - third, and only under conditions of excellent seeing, to observe near or at the solar limb, - fourth, to obtain at least one time series at fast (20s or faster) cadence in Halpha to explore further the dynamics of fibrils and their possibility to trace out magnetic lines of force, - fifth, to assess the origin and mitigation of cross-talk between Stokes parameters observed with IBIS.