SOTSP: CORE (HOP0002) Polar Monitoring Campaign during the Solar Cycle
2014-06-05T15:21:47 to 2014-06-05T16:19:45
Science Goal: HOP 81 @ N Pole (Day 1, FSM)
Program: Fast deep mode, HOP81 in the eclipse, WEST +680
Target: N Pole
xcen=93 ycen=873
Instrument: SOTSP
HOP/JOP: 0
Description:
abstract of observational proposal 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. For FSM ???BFI G-band: FoV 221"x111", Binning: 2x2, Time resolution: 30 min, JPEG Quality: Q75, Data rate: 9 Mbits/h ???NFI Na I: IVDG mode, FoV: 328??? x 164???, Binning: 2x2, Time resolution: 5 min, JPEG Quality: Q75, Data rate: 102 Mbits/h ??? SP FoV 320??? x 164???, Pixel size: 0.32???/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.
abstract of observational proposal 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. For FSM ???BFI G-band: FoV 221"x111", Binning: 2x2, Time resolution: 30 min, JPEG Quality: Q75, Data rate: 9 Mbits/h ???NFI Na I: IVDG mode, FoV: 328??? x 164???, Binning: 2x2, Time resolution: 5 min, JPEG Quality: Q75, Data rate: 102 Mbits/h ??? SP FoV 320??? x 164???, Pixel size: 0.32???/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.
wavelength: 6302A Continuum Intensity cadence: 0 min fov: 106,162 images: 337 JavaScript Landing Page
