| Overview | Where | Groups: Mode, FOV, # spectra in map | Data Links |
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2007-07-21 19:20:50-20:00:20
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filament filament evolution |
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| 6302A Continuum Intensity | 197"x162" | 621 spectra | | 6302A Longitudinal Flux Density | 197"x162" | 621 spectra | | 6302A Transverse Flux Density | 197"x162" | 621 spectra | | 6302A Velocity 6301.5A | 197"x162" | 621 spectra |
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Level 1 Summary
Level 2 Summary
Level 1 Monthly
Level 2 Monthly
SP Cubes 10 MB |
SOTSP: filament
2007-07-21T19:20:50 to 2007-07-21T20:00:20
Science Goal: filament evolution
Program: Fast map 200 arcsec, ROI 2
Target: Filament
xcen=432 ycen=581
Instrument: SOTSP
HOP/JOP: 24
Description:
Daily Note and User Entry: SOT: Track AR and observe filament or prominence HOP15 will be tested from 07/18 to 07/22. HOP10 prominence observation. HOP24 filament observation. EIS: HOP10 Norikura 4hour per day if whether is fine in Norikura. (Limb fix) XRT: Support HOP10 if possible. Mike Marsh's AR evolution program (coordinated with TRACE) may be run if possible.
Request to SOT: Observation of Ca H spicules. The sequence that was run previously is used. Widest FOV in the NS direction is desired.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines
Other Instruments: Norikura: High dispersion spectra of Fe X6374 and Fe XIV5303 are obtained. High-acuracy Doppler velocity and line width are given. Independent Fe XIV 5303 imaging observations provide high-cadence imaging and Doppler informaiton. Bi-products: <
This is the most important for EIS team.>
: By the simultaneous observations with Norikura Solar Observatory, EIS line width of instrumental origin is absolutely calibrated. In EIS bandpass there are Fe X lines in the short wavelength band and Fe XIV lines in the long wavelength band. These are calibrated with Fe X 6374 and Fe XIV 5303 emission lines. Norikura Solar Observatory is going to support this campaign observation with a high priority.
Daily Note and User Entry: SOT: Track AR and observe filament or prominence HOP15 will be tested from 07/18 to 07/22. HOP10 prominence observation. HOP24 filament observation. EIS: HOP10 Norikura 4hour per day if whether is fine in Norikura. (Limb fix) XRT: Support HOP10 if possible. Mike Marsh's AR evolution program (coordinated with TRACE) may be run if possible.
Request to SOT: Observation of Ca H spicules. The sequence that was run previously is used. Widest FOV in the NS direction is desired.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines
Other Instruments: Norikura: High dispersion spectra of Fe X6374 and Fe XIV5303 are obtained. High-acuracy Doppler velocity and line width are given. Independent Fe XIV 5303 imaging observations provide high-cadence imaging and Doppler informaiton. Bi-products: <
This is the most important for EIS team.>
: By the simultaneous observations with Norikura Solar Observatory, EIS line width of instrumental origin is absolutely calibrated. In EIS bandpass there are Fe X lines in the short wavelength band and Fe XIV lines in the long wavelength band. These are calibrated with Fe X 6374 and Fe XIV 5303 emission lines. Norikura Solar Observatory is going to support this campaign observation with a high priority.
Annotations:
Hits: 67
Chief Observer
Sekii, Watanabe and Shine
Related Links
Cites:
filament See also
Get All Data
saaIntervals
hiIntervals
Time Series (SP Datacubes)
wavelength: 6302A Continuum Intensity cadence: 0 min fov: 197,162 images: 621 JavaScript Landing Page
