2007-09-17T22:26:22.000Z http://sot.lmsal.com Mr. Sam Freeland Lockheed Martin Solar and Astrophysics Laboratory (LMSAL) http://www.lmsal.com Lockheed Martin Advanced Tech Center, 3251 Hanover Rd, O/ADBS, B/252, Palo Alto, CA 94304 null null HINODE SOT Hara Sterling Shine and Ishikawa 2 North Pole magnetic fields North pole PCH PCH 1 141 905 0 162 2007-09-16T01:23:34.000Z 2007-09-16T06:52:53.000Z 141 905 Polar Region Observation Campaign SP Deep Map full range Daily Note and User Entry: Daily Note and User Entry:North Pole deep magnetic field measurements Request to SOT: G-band and Ca-H at high cadence full resolution with vector magnetograms. ??????4.8 x 4 seconds integration time needed in SP to increase the SNR a factor of 2 on the limb Time evolution of granular structures are ~ 1 min. 80""x120"" maps will take 4 hours in total 5 positions (North, South, East, West, disc center) with no active regions. West limb have been only once observed and East limb never !!! At least high resolution G-band maps (1x1) to identify magnetic features. Scientific Objectives: ??????Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request. ??????Motivation: ???ENorth and south limb HINODE/SP data have shown a conspicuous presence of small magnetic fields structures that has not been detected up to now.???EThere is a strong interest in determining the magnetic structure and origin of these magnetic features, besides their relationship among the four cardinal points. ???EDisk center SP data have also shown a opulence of small scale flux tube concentrations with may be connected to north and south poles magnetic activity. Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements???@with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and WL in context. LASCO: TBD ??????inner Hinode; Request to SOT: G-band and Ca-H at high cadence full resolution with vector magnetograms. ??????4.8 x 4 seconds integration time needed in SP to increase the SNR a factor of 2 on the limb Time evolution of granular structures are ~ 1 min. 80""x120"" maps will take 4 hours in total 5 positions (North, South, East, West, disc center) with no active regions. West limb have been only once observed and East limb never !!! At least high resolution G-band maps (1x1) to identify magnetic features.; Scientific Objectives: ??????Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection; produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request. ??????Motivation: ???ENorth and south limb HINODE/SP data have shown a conspicuous presence of small magnetic fields structures that has not been detected up to now.???EThere is a strong interest in determining the magnetic structure and origin of these magnetic features, besides their relationship among the four cardinal points. ???EDisk center SP data have also shown a opulence of small scale flux tube concentrations with may be connected to north and south poles magnetic activity.; Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements???@with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same ;slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and; WL in context. LASCO: TBD ??????inner Hinode ivo://sot.lmsal.com/VOEvent#2007-09-16T01:21:30Z