SOTSP: Disk center emerging flux, SP
2007-07-29T02:50:59 to 2007-07-29T04:04:29
Science Goal: Emerging flux, super granule
Program: SP 4 cycle, 10", half height for emerging flux
Target: Disk Center
xcen=-94 ycen=8
Instrument: SOTSP
HOP/JOP: 10
Description:
Daily Note and User Entry: Note: The time of the 1st contact (MSP1) is earlier than usual. SOT: Support HOP10 Norikura and HOP24, which observes prominences and filaments at limb. andnbsp
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Coalignment program run (N-limb, E-limb, 2hour for each) to run in weekend plan. XRT: Stop X-ray observation (and perform CCD bakeout).
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: Note: The time of the 1st contact (MSP1) is earlier than usual. SOT: Support HOP10 Norikura and HOP24, which observes prominences and filaments at limb. andnbsp
andnbsp
andnbsp
andnbsp
Coalignment program run (N-limb, E-limb, 2hour for each) to run in weekend plan. XRT: Stop X-ray observation (and perform CCD bakeout).
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.
wavelength: 6302A Continuum Intensity cadence: 0 min fov: 11,81 images: 1087 JavaScript Landing Page
