SOTSP: HOP 81 North Pole
2010-07-24T10:16:19 to 2010-07-24T11:19:32
Science Goal: CORE (HOP0002) Polar Monitoring Campaign during the Solar Cycle
Program: Fast Map, Full FOV 1 side CCD
Target: N Pole
xcen=-0 ycen=914
Instrument: SOTSP
HOP/JOP: 81
Description:
Request to SOT HOP Number 0081 For DSM Day 1, 2, 4 and 5 ?E BFI G-band: FoV 221"x111", Binning: 2x2, Time resolution: 30 min, JPEG Quality: Q75 Note: One image per one observation period. ?E NFI Na I: IVDG mode, FoV: 328?h x 164?h, Binning: 2x2, Time resolution: 5 min, JPEG Quality: Q75 Note: One image per one observation period. ?E SOT-SP FoV 320?h x 164?h, Pixel size: 0.16?h/pix, Binning: 1x1, Single side mode Exposure: 12.8 sec (16 Cycles), JPEG Quality: Q75, Data rate: 2280Mbits/map Note: If the exposure time may cause the saturation, please decrease it. Note: Since the data size of SP is very huge for the allocation data size of SOT, we can observe only one SP map during two days. It is OK. Note: set margin factors to 1.4 for FG and SP Day 3 ?EBFI G-band: FoV 221"x111", Binning: 2x2, Time resolution: 30 min, JPEG Quality: Q75, Data rate: 9 Mbits/h Note: The G-band images are used for mainly co-alignment. Please insert a G-band image when the observation starts. ?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 ?ESP 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: One map per one day. Note: set margin factors to 1.4 for FG and SP Day 6 The observation plan for Day 6 is same as Day 3. The target is different. In March, the target is the north-polar region. In September, the target is the south-polar region. For FSM ?EBFI G-band: FoV 221"x111", Binning: 2x2, Time resolution: 30 min, JPEG Quality: Q75, Data rate: 9 Mbits/h Note: The G-band images are used for mainly co-alignment. Please insert a G-band image when the observation starts. ?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: 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.
Request to SOT HOP Number 0081 For DSM Day 1, 2, 4 and 5 ?E BFI G-band: FoV 221"x111", Binning: 2x2, Time resolution: 30 min, JPEG Quality: Q75 Note: One image per one observation period. ?E NFI Na I: IVDG mode, FoV: 328?h x 164?h, Binning: 2x2, Time resolution: 5 min, JPEG Quality: Q75 Note: One image per one observation period. ?E SOT-SP FoV 320?h x 164?h, Pixel size: 0.16?h/pix, Binning: 1x1, Single side mode Exposure: 12.8 sec (16 Cycles), JPEG Quality: Q75, Data rate: 2280Mbits/map Note: If the exposure time may cause the saturation, please decrease it. Note: Since the data size of SP is very huge for the allocation data size of SOT, we can observe only one SP map during two days. It is OK. Note: set margin factors to 1.4 for FG and SP Day 3 ?EBFI G-band: FoV 221"x111", Binning: 2x2, Time resolution: 30 min, JPEG Quality: Q75, Data rate: 9 Mbits/h Note: The G-band images are used for mainly co-alignment. Please insert a G-band image when the observation starts. ?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 ?ESP 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: One map per one day. Note: set margin factors to 1.4 for FG and SP Day 6 The observation plan for Day 6 is same as Day 3. The target is different. In March, the target is the north-polar region. In September, the target is the south-polar region. For FSM ?EBFI G-band: FoV 221"x111", Binning: 2x2, Time resolution: 30 min, JPEG Quality: Q75, Data rate: 9 Mbits/h Note: The G-band images are used for mainly co-alignment. Please insert a G-band image when the observation starts. ?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: 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.
wavelength: 6302A Continuum Intensity cadence: 0 min fov: 314,162 images: 997 JavaScript Landing Page
