2024-09-24T22:21:04.000Z 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 SOTSP Miyoshi Brooks Cruz (RCO) 81 HOP 81 S Pole DSM Day 3 of 3 S Pole LMB LMB 7 20130911_103529 197 218 236 7 26 2046 6 1 1 2 0 52 2010 1016 0.9931573802541545 -13.127 -936.593 322.072 162.304 2013-09-11T10:35:29.000Z 2013-09-11T13:29:03.000Z -13.127 -936.593 CORE (HOP0002) Polar Monitoring Campaign during the Solar Cycle Fast deep mode, 2048 slit position, LIMB ONLY Request to SOT HOP Number 0081 For DSM Day 1 ???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 2 ???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 ???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: 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. Note: set margin factors to 1.4 for FG and SP Day 3 The observation plan for Day 3 is same as Day 2. 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 ???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.;;Request to SOT HOP Number 0081 For DSM Day 1 ???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 2 ???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 ???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: 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. Note: set margin factors to 1.4 for FG and SP Day 3 The observation plan for Day 3 is same as Day 2. 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 ???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. ivo://sot.lmsal.com/VOEvent#2013-09-11T10:34:01Z