Heliophysics Events Knowledgebase Coverage Registry (HCR)
Observation Details
Overview Where Groups: Mode, FOV, # spectra in map Data Links
2019-06-07 12:08:23-13:06:21
HOP81 S pole
HOP81 Polar Monitoring Campaign
x,y:-120",-946"
Max FOV:106"x162"
Target:S. Pole
Nearby Events
6302A Continuum Intensity106"x162"339 spectra
6302A Longitudinal Flux Density106"x162"339 spectra
6302A Transverse Flux Density106"x162"339 spectra
6302A Velocity 6301.5A106"x162"339 spectra
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SP Cubes 5 MB
SOTSP: HOP81 S pole
2019-06-07T12:08:23 to 2019-06-07T13:06:21
Science Goal: HOP81 Polar Monitoring Campaign
Program: Fast deep mode, HOP81 in the eclipse, EAST -680
Target: S. Pole
xcen=-120 ycen=-946
Instrument: SOTSP
HOP/JOP: 81
Description: 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.

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: 37
Chief Observer
De Rosa
Related Links
Cites: HOP81 S pole     
Timeline: gif use
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wavelength: 6302A Continuum Intensity cadence: 0 min fov: 106,162 images: 339 JavaScript Landing Page
wavelength: 6302A Velocity 6301.5A cadence: 0 min fov: 106,162 images: 339 JavaScript Landing Page
wavelength: 6302A Transverse Flux Density cadence: 0 min fov: 106,162 images: 339 JavaScript Landing Page
wavelength: 6302A Longitudinal Flux Density cadence: 0 min fov: 106,162 images: 339 JavaScript Landing Page
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