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Observation Details
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2014-12-11 13:04:23-15:57:57
HOP 81 N Pole Fast Scan Mode
CORE (HOP0002) Polar Monitoring Campaign during the Solar Cycle
x,y:-24",892"
Max FOV:321"x162"
Target:N Pole
Nearby Events
6302A Continuum Intensity321"x162"1019 spectra
6302A Longitudinal Flux Density321"x162"1019 spectra
6302A Transverse Flux Density321"x162"1019 spectra
6302A Velocity 6301.5A321"x162"1019 spectra
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SP Cubes 16 MB
SOTSP: HOP 81 N Pole Fast Scan Mode
2014-12-11T13:04:23 to 2014-12-11T15:57:57
Science Goal: CORE (HOP0002) Polar Monitoring Campaign during the Solar Cycle
Program: Fast deep mode, 2048 slit position, LIMB ONLY
Target: N Pole
xcen=-24 ycen=892
Instrument: SOTSP
HOP/JOP: 81
Description: Request to SOT HOP Number 0081 For FSM ?EBFI G-band: FoV 221"x111", Binning: 2x2, Time resolution: 30 min, JPEG Quality: Q75, Data rate: 9 Mbits/h ?ENFI Na I: IVDG mode, FoV: 328?h x 164?h, Binning: 2x2, Time resolution: 5 min, JPEG Quality: Q75, Data rate: 102 Mbits/h ?E SP FoV 320?h x 164?h, Pixel size: 0.32?h/pix, Binning: 2x2, Single side mode Exposure: 4.8 sec (6 Cycles), JPEG Quality: Q75, Data rate: 600Mbits/map Note: The G-band images are used for mainly co-alignment. Please insert a G-band image when the observation starts. Note: One map per one day. Other Instruments: Scientific Objectives: Objectives: 1: To observe the evolution of the magnetic field distribution around the poles during the solar cycle. 2: To understand the relationship between photospheric magnetic field and the coronal structures (include the solar wind) around the poles. Scientific Background: The polar observations by SOT/SP revealed that there are many strong patchy magnetic poles around the poles. Such strong magnetic fields in the polar region may strongly relate with the dynamo and it is very important to observe the evolution of the magnetic field distribution for understanding the dynamo. The strong patchy magnetic poles have the trumpet-like vertical magnetic structure. Although we think that the trumpet structures may relate with the fast solar wind, there are no coronal (X-ray/EUV) structures on most of the magnetic structures. To understand the fast solar wind, the relationship between photospheric magnetic fields and coronal structures in the polar coronal hole is very essential. During the polarity reversal, the opposite polarity magnetic field invade the polar region. At the time, the relationship between coronal activities/structures and photospheric magnetic field is very interesting for understanding the solar wind.

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Hits: 23
Chief Observer
Cruz (RCO) --> de Wijn (RCO)
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Cites: HOP 81 N Pole Fast Scan Mode     
Timeline: gif use
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wavelength: 6302A Continuum Intensity cadence: -1 min fov: 321,162 images: 1019 JavaScript Landing Page
wavelength: 6302A Velocity 6301.5A cadence: -1 min fov: 321,162 images: 1019 JavaScript Landing Page
wavelength: 6302A Transverse Flux Density cadence: -1 min fov: 321,162 images: 1019 JavaScript Landing Page
wavelength: 6302A Longitudinal Flux Density cadence: -1 min fov: 321,162 images: 1019 JavaScript Landing Page
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