Observation

Observation Details

XRT: Inter ARs loops

2007-07-07T07:04:54 to 2007-07-07T10:19:54

Science Goal: Joint Observation of the Solar Corona between Hinode EIS and NAOJ Norikura Observatory for nonthermal line broadening in the coronal emission

Program: Inter_ARs_loops

Target: QR

xcen=876 ycen=-202

Instrument: XRT

HOP/JOP: 0

Description: Tim File-OBS_DEC: Synoptics Open+Al/Mesh (181/4096) - Backup Period
Daily Note: none
Request to XRT HOP Number 0010: The sequence that was run previously is used. No strong request.
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: andlt
This is the most important for EIS team.andgt
: 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.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines Daily Note: none
Request to XRT HOP Number 0010: The sequence that was run previously is used. No strong request.
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: andlt
This is the most important for EIS team.andgt
: 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.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines Daily Note: none
Request to XRT HOP Number 0010: The sequence that was run previously is used. No strong request.
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: andlt
This is the most important for EIS team.andgt
: 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.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines Daily Note: none
Request to XRT HOP Number 0010: The sequence that was run previously is used. No strong request.
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: andlt
This is the most important for EIS team.andgt
: 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.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines Daily Note: none
Request to XRT HOP Number 0010: The sequence that was run previously is used. No strong request.
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: andlt
This is the most important for EIS team.andgt
: 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.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines Daily Note: none
Request to XRT HOP Number 0010: The sequence that was run previously is used. No strong request.
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: andlt
This is the most important for EIS team.andgt
: 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.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines Daily Note: none
Request to XRT HOP Number 0010: The sequence that was run previously is used. No strong request.
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: andlt
This is the most important for EIS team.andgt
: 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.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines Daily Note: none
Request to XRT HOP Number 0010: The sequence that was run previously is used. No strong request.
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: andlt
This is the most important for EIS team.andgt
: 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.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines Daily Note: none
Request to XRT HOP Number 0010: The sequence that was run previously is used. No strong request.
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: andlt
This is the most important for EIS team.andgt
: 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.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines Daily Note: none
Request to XRT HOP Number 0010: The sequence that was run previously is used. No strong request.
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: andlt
This is the most important for EIS team.andgt
: 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.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines Daily Note: none
Request to XRT HOP Number 0010: The sequence that was run previously is used. No strong request.
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: andlt
This is the most important for EIS team.andgt
: 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.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines

Annotations:

Chief Observer

Masumi Shimojo/Noriyuki Narukage