SOTSP: North Pole magnetic fields
2007-09-22T07:21:33 to 2007-09-22T08:14:33
Science Goal: Polar Region Observation Campaign
Program: 281 slits (one hour), 16 cyles, I scaled
Target: North pole
xcen=-8 ycen=912
Instrument: SOTSP
HOP/JOP: 2
Description:
Daily Note and User Entry: Polar magnetic fields
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
Daily Note and User Entry: Polar magnetic fields
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
wavelength: 6302A Continuum Intensity cadence: -1 min fov: 39,162 images: 243 JavaScript Landing Page
