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2007-08-08 23:54:38-00:45:09 +1d

HOP12 for Hida

Cooperative Observations between Hida Observatory and; Hinode Satellite - 1. Emerging Flux Regions 2. Cool Jets 3. Ellerman Bombs

x,y:	-94",-189"
Max FOV:	5"x41"
Target:	Active Region
Nearby Events

6302A Continuum Intensity	5"x41"	1500 spectra
6302A Longitudinal Flux Density	5"x41"	1500 spectra
6302A Transverse Flux Density	5"x41"	1500 spectra
6302A Velocity 6301.5A	5"x41"	1500 spectra

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SOTSP: HOP12 for Hida

2007-08-08T23:54:38 to 2007-08-09T00:45:09

Science Goal: Cooperative Observations between Hida Observatory and; Hinode Satellite - 1. Emerging Flux Regions 2. Cool Jets 3. Ellerman Bombs

Program: Dynamic Mode, 30 slits, 50 sec cadence, 30 repeat

Target: Active Region

xcen=-94 ycen=-189

Instrument: SOTSP

HOP/JOP: 12

Description: Daily Note and User Entry: AOCS commands to disable onboard night auto detect (on Wed). HOP29, filament, prominence, cavities (18 -22 UT). HOP12 (22 - 3 UT, can be extended to 6 UT if no conflict). Alignment offset program in today's plan. EIS: 1) EIS would like extended periods of quiet Sun limb pointings for two different programmes andnbsp
a) east limb and west limb pointings for 4 hours at each, within a period of 48 hours for absolute wavelength calibration andnbsp
b) quiet Sun limb pointings (any portion of the limb away from activity or coronal holes) to study the behaviour of line profiles, temperature, and density as a function of radial position 2) HOP 29 (IHY Filaments studies) to run beginning today 3) Will support TOO of a prominence for observations 4) HOP 12 to run once XRT is making observations XRT: CCD Bakeout
Request to SOT: 1a.

* G-band Filtergraph: ???@

Observation of the arch-filaments on the photosphere, ???@

measurement of the horizontal flow (by LCT) around EFR/AFS. ???@

Time cadence: 15 sec ???@

Duration: as long as possible ???@

* Ca Filtergraph: ???@

Observation of the arch-filaments in the chromosphere ???@

Time cadence: about 30 sec ???@

Duration: as long as possible ???@

* SP: ???@

Measurement of the time-evolution of magnetic flux and Doppler ???@

velocity around the EFR/AFS. ???@

Time cadence: 180 sec ???@

Scan step: 0.3 - 0.6 arcsec/step ???@

Scan width: 20 - 60 arcsec (wider than the size of EFR) ???@

Duration: as long as possible 1b. ???@

* Ca Filtergraph: ???@

Observation of the chromospheric gas motion on the footpoint of ???@

magnetic filament. ???@

Time cadence: 8 sec ???@

* G-band Filtergraph: ???@

Detection of the photospheric bright point (G-band bright point). ???@

Time cadence: 8 sec ???@

* SP: ???@

Distinction of the footpoint of magnetic filament. ???@

Time cadence: 30 sec ???@

Scan step: 0.3 - 0.6 arcsec/step ???@

Scan width: about 20 - 30 arcsec 1c. ???@

* G-band Filtergraph: ???@

Detection and distinction of the footpoint of magnetic flux tube, ???@

measurement of the horizontal flow on the photosphere ???@

Time cadence: 8 sec ???@ ???@

* Ca Filtergraph: ???@

Observation of the chromospheric gas motion on the footpoint of ???@

magnetic flux tube ???@

Time cadence: 8 sec ???@ ???@

* SP: ???@

Measurement of the time-evolution of magnetic flux and Doppler ???@

velocity around/in the flux tube. ???@

Time cadence: <
30 sec ???@

Scan step: 0.3 - 0.6 arcsec ???@

Scan width: as wide as possible 2. ???@

Ca and
G-band Filtergraph: ???@

Detection of jets around the photosphere and chromosphere ???@

Time cadence: 10 sec (respectively) ???@

SP: ???@

Observation of the photospheric magnetic field configurations around the jets ???@

Time cadence: 60 sec ???@

Scan step: 0.3 - 0.6 arcsec ???@

Scan width: as wide as possible 3. ???@

* SP: ???@

Obtaining photospheric magnetic field and Doppler velocity ???@

around/at Ellerman bomb ???@

Time cadence: 60 sec ???@

Scan step: 0.3 - 0.6 arcsec ???@

Scan width: as wide as possible ???@

* Ca H Filtergram: ???@

Observing shape and time evolution of the Ellerman bomb ???@

Time cadence: 8 sec
Scientific Objectives: 1a. Rise velocity of emerging loops 1b. Shock waves just below the arch filaments in emerging flux regions 1c. Evolution of magnetic element at the footpoint of emerging flux region 2. Detection of Alfven wave generation 3. Observation of reconnection jets and X-ray signatures in the corona
Other Instruments:

Daily Note and User Entry: AOCS commands to disable onboard night auto detect (on Wed). HOP29, filament, prominence, cavities (18 -22 UT). HOP12 (22 - 3 UT, can be extended to 6 UT if no conflict). Alignment offset program in today's plan. EIS: 1) EIS would like extended periods of quiet Sun limb pointings for two different programmes andnbsp
a) east limb and west limb pointings for 4 hours at each, within a period of 48 hours for absolute wavelength calibration andnbsp
b) quiet Sun limb pointings (any portion of the limb away from activity or coronal holes) to study the behaviour of line profiles, temperature, and density as a function of radial position 2) HOP 29 (IHY Filaments studies) to run beginning today 3) Will support TOO of a prominence for observations 4) HOP 12 to run once XRT is making observations XRT: CCD Bakeout
Request to SOT: 1a.

* G-band Filtergraph: ???@

Observation of the arch-filaments on the photosphere, ???@

measurement of the horizontal flow (by LCT) around EFR/AFS. ???@

Time cadence: 15 sec ???@

Duration: as long as possible ???@

* Ca Filtergraph: ???@

Observation of the arch-filaments in the chromosphere ???@

Time cadence: about 30 sec ???@

Duration: as long as possible ???@

* SP: ???@

Measurement of the time-evolution of magnetic flux and Doppler ???@

velocity around the EFR/AFS. ???@

Time cadence: 180 sec ???@

Scan step: 0.3 - 0.6 arcsec/step ???@

Scan width: 20 - 60 arcsec (wider than the size of EFR) ???@

Duration: as long as possible 1b. ???@

* Ca Filtergraph: ???@

Observation of the chromospheric gas motion on the footpoint of ???@

magnetic filament. ???@

Time cadence: 8 sec ???@

* G-band Filtergraph: ???@

Detection of the photospheric bright point (G-band bright point). ???@

Time cadence: 8 sec ???@

* SP: ???@

Distinction of the footpoint of magnetic filament. ???@

Time cadence: 30 sec ???@

Scan step: 0.3 - 0.6 arcsec/step ???@

Scan width: about 20 - 30 arcsec 1c. ???@

* G-band Filtergraph: ???@

Detection and distinction of the footpoint of magnetic flux tube, ???@

measurement of the horizontal flow on the photosphere ???@

Time cadence: 8 sec ???@ ???@

* Ca Filtergraph: ???@

Observation of the chromospheric gas motion on the footpoint of ???@

magnetic flux tube ???@

Time cadence: 8 sec ???@ ???@

* SP: ???@

Measurement of the time-evolution of magnetic flux and Doppler ???@

velocity around/in the flux tube. ???@

Time cadence: <
30 sec ???@

Scan step: 0.3 - 0.6 arcsec ???@

Scan width: as wide as possible 2. ???@

Ca and
G-band Filtergraph: ???@

Detection of jets around the photosphere and chromosphere ???@

Time cadence: 10 sec (respectively) ???@

SP: ???@

Observation of the photospheric magnetic field configurations around the jets ???@

Time cadence: 60 sec ???@

Scan step: 0.3 - 0.6 arcsec ???@

Scan width: as wide as possible 3. ???@

* SP: ???@

Obtaining photospheric magnetic field and Doppler velocity ???@

around/at Ellerman bomb ???@

Time cadence: 60 sec ???@

Scan step: 0.3 - 0.6 arcsec ???@

Scan width: as wide as possible ???@

* Ca H Filtergram: ???@

Observing shape and time evolution of the Ellerman bomb ???@

Time cadence: 8 sec
Scientific Objectives: 1a. Rise velocity of emerging loops 1b. Shock waves just below the arch filaments in emerging flux regions 1c. Evolution of magnetic element at the footpoint of emerging flux region 2. Detection of Alfven wave generation 3. Observation of reconnection jets and X-ray signatures in the corona
Other Instruments:

Annotations:

Chief Observer

Nagata, Tarbell