2024-09-24T22:21:28.000Z http://sot.lmsal.com Mr. Sam Freeland Lockheed Martin Solar and Astrophysics Laboratory (LMSAL) http://www.lmsal.com Lockheed Martin Advanced Tech Center, 3251 Hanover Rd, O/ADBS, B/252, Palo Alto, CA 94304 null null HINODE SOTSP Kotoku Sterling Cruz 47 HOP47 Moss Obs Quiet Sun, Moss NET NET 15 20071114_124305 128 103 101 8 98 312 2 2 1 2 0 22 2032 156 1 118.3 -92.831 8.242 162.304 2007-11-14T12:43:05.000Z 2007-11-14T12:52:56.000Z 118.3 -92.831 SUMER campaign - Moss Observation Na IV 3.5kx2k GB 3.5kx2k, 90sec --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. ivo://sot.lmsal.com/VOEvent#2007-11-14T12:13:00Z