Observation

Observation Details

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Groups: Mode, FOV, # spectra in map

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2007-11-14 14:13:05-14:22:56

HOP47 Moss Obs

SUMER campaign - Moss Observation

x,y:	132",-93"
Max FOV:	8"x162"
Target:	Quiet Sun, Moss
Nearby Events

6302A Continuum Intensity	8"x162"	7 spectra
6302A Longitudinal Flux Density	8"x162"	7 spectra
6302A Transverse Flux Density	8"x162"	7 spectra
6302A Velocity 6301.5A	8"x162"	7 spectra

Level 1 Summary
Level 2 Summary
Level 1 Monthly
Level 2 Monthly
SP Cubes 2 MB

SOTSP: HOP47 Moss Obs

2007-11-14T14:13:05 to 2007-11-14T14:22:56

Science Goal: SUMER campaign - Moss Observation

Program: Na IV 3.5kx2k GB 3.5kx2k, 90sec

Target: Quiet Sun, Moss

xcen=132 ycen=-93

Instrument: SOTSP

HOP/JOP: 47

Description: --SUMER Campaign--- HOP47: Moss Observations (WED 11/14: 1213 - 1801) HOP47 Moss Obs 2007/11/14 12:13:00 - 2007/11/14 18:01:05 pointing: (118,-99) FG15 (0x017a) Na IV 3.5kx2k GB 3.5kx2k, 90sec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec Request to SOT HOP Number 0047 BFI: G-band, Ca H-line 105x105"" FOV, 2x2 summed NFI: 1. H-alpha -300mA blue wing filtergrams 2. Fe I 6301.5 magnetograms 160x160"" FOV, 2x2 summed SP: Fast Map, 50"" scan over the AR, repeat every 30 minutes Programs 1 and
2 in the NFI can't be run at the same time so we'd run H-alpha for 2 hours and then switch to the Fe I magnetograms for another 2 hours. A cadence of 10 - 30 s for the BFI and NFI filtegrams would be adequate. AR moss is believed to correspond tothe ~ 1 MK footpoints of hot (3 MK) SXR loops and represents a sensitive monitor of coronal heating and conditions. Coronal loop models can run under certain circumstances into trouble when trying to reproduce the moss in that the predicted intensities are much larger than what is observed. Absorption of moss emission by cool and dense spicule plasma is a proposed mechanism for bringing observations and modeling into a better agreement.

--SUMER Campaign--- HOP47: Moss Observations (WED 11/14: 1213 - 1801) HOP47 Moss Obs 2007/11/14 12:13:00 - 2007/11/14 18:01:05 pointing: (118,-99) FG15 (0x017a) Na IV 3.5kx2k GB 3.5kx2k, 90sec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec SP08 (0x0080) Fast map 50 arcsec Request to SOT HOP Number 0047 BFI: G-band, Ca H-line 105x105"" FOV, 2x2 summed NFI: 1. H-alpha -300mA blue wing filtergrams 2. Fe I 6301.5 magnetograms 160x160"" FOV, 2x2 summed SP: Fast Map, 50"" scan over the AR, repeat every 30 minutes Programs 1 and
2 in the NFI can't be run at the same time so we'd run H-alpha for 2 hours and then switch to the Fe I magnetograms for another 2 hours. A cadence of 10 - 30 s for the BFI and NFI filtegrams would be adequate. AR moss is believed to correspond tothe ~ 1 MK footpoints of hot (3 MK) SXR loops and represents a sensitive monitor of coronal heating and conditions. Coronal loop models can run under certain circumstances into trouble when trying to reproduce the moss in that the predicted intensities are much larger than what is observed. Absorption of moss emission by cool and dense spicule plasma is a proposed mechanism for bringing observations and modeling into a better agreement.

Annotations:

Chief Observer

Cruz