JOINT CDS/TRACE/SUMER/MDI/EIT PROGRAMME JOP118 The Temperature Range of the Sunspot 3-minute Oscillations Per Maltby, Nils Brynildsen, Olav Kjeldseth-Moe, ITA, University of Oslo Richard A. Shine, Lockheed Palo Alto Research Laboratory Klaus Wilhelm, Max-Planck-Institut fur Aeronomie, Germany Received 25 December 1999 Modified 18 April 2001: SUMER not available for solar disk observations Modified 23 July 2001: CDS study O_SPOT_B must not be used. Scientific Justification: This programme builds on the knowledge obtained from JOP018 about the 3-minute oscillations above sunspots, see Brynildsen et al. 1999, ApJ 511, L121, Brynildsen et al. 1999, ApJ 517, L159, Brynildsen et al. 2000, Solar Phys., 191, 129, Maltby et al. 1999, Solar Phys., 190, 437. Briefly, simultaneous SUMER measurements of the intensity and the line-of-sight velocity show that the observations in the chromosphere and the transition region are compatible with the hypothesis that the oscillations are caused by upward-propagating acoustic waves. We have studied the intensity oscillations observed with the TRACE 171 channel above several sunspots. In some sunspots we find that the 171 intensity oscillations show a power spectrum with a maximum close to 6 mHz. These oscillations may be an extension of the sunspot transition region oscillations into the corona. However, this result is uncertain since the oscillations occur in an area where the emission in the 171 channel is weak, most likely because the coronal Fe IX/X emission is weak. Hence, without spectroscopic observations we cannot exclude the possibility that transition region lines, such as O VI at 172.93 Å, 173.08 Å contribute to the oscillations in the 171 channel. We plan to increase our knowledge by observations with: * CDS Normal Incidence Spectrometer * The wavelength bands of the CDS Grazing Incidence Spectrometer (GIS). The intension is to measure the relative contributions of such transition region lines as O VI 172.93 Å, 173.08 Å, Ne VII 465.22 Å, and O V 760.40 Å, to the intensity oscillations. * TRACE observations in the 171 channel with high cadence. * MDI when possible: Doppler velocities and magnetic field measurements, with high spatial resolution and high cadence. The first CDS study is a 120"x120" NIS raster (O_SPOT2), place the centre of this raster 6" west of the western rim of the sunspot umbra. Next, after adjusting for solar rotation, let the slit drift across the sunspot for 4h35m, while the GIS study (O_SPOT10) is run. Then after a second adjustment for solar rotation let the slit drift across the sunspot for 4h9m, while the NIS study (O_SPOT11) is run. Then after a third adjustment for solar rotation the study series ends with a 120"x120" NIS raster (O_SPOT2). NOTE: The GIS study O_SPOT10 MUST have an y-offset of -23". CDS Study Det. X-pos Y-pos # rasters Duration Total duration -------- --- ----- ----- --------- -------- -------------- O_SPOT2 NIS x0 y0 1 25m 24s 25m 24s O_SPOT10 GIS x1 y0-23" 6 45m 50s 4h 35m 0s O_SPOT11 NIS x2 y0 4 1h 2m 10s 4h 8m 40s O_SPOT2 NIS x3 y0 1 25m 24s 25m 24s -------------- 9h 34m 28s NIS Study: O_SPOT2 Spectrometer: Normal Incidence Slit: 2 x 240 arcsec Raster Area: 120 x 120 arcsec Step (DX, DY): 2 arcsec, 0 arcsec Raster Locations: 60 x 1 = 60 Exposure Time: 20 seconds Duration of Raster: 1524 seconds Number of Rasters: 1 Total Duration: 1524 seconds Line Selection: Mg VIII 315.02, Fe XIV 334.17, Fe XVI 360.76, Mg IX 368.06, He I 522.20, O IV 554.52, Ne VI 562.83, He I 584.33, O III 599.59, O V 629.73 Bins Across Line: 21 Telemetry/Compression: truncate to 12 bits Pointing: Sunspot GIS Study: O_SPOT10 Spectrometer: Grazing Incidence Slit: 4 x 4 arcsec Raster Area: 4 x 4 arcsec Step (DX, DY): 0 arcsec, 0 arcsec Raster Locations: 145 Exposure Time: 17 seconds Duration of Raster: 2750 seconds Number of Rasters: 6 Total Duration: 16500 seconds Line Selection: Full GIS output Pointing: Sunspot NIS Study: O_SPOT11 Spectrometer: Normal Incidence Slit: 2 x 240 arcsec Raster Area: 2 x 120 arcsec Step (DX, DY): 0 arcsec, 0 arcsec Raster Locations: 250 x 1 = 250 Exposure Time: 10 seconds Duration of Raster: 3730 seconds Number of Rasters: 4 Total Duration: 14920 seconds Line Selection: Fe XVI 360.76, Mg IX 368.06, O IV 554.52, Ne VI 562.83, He I 584.33, O V 629.73 Bins Across Line: 25 Telemetry/Compression: truncate to 12 bits Pointing: Sunspot NIS Study: O_SPOT2 Spectrometer: Normal Incidence Slit: 2 x 240 arcsec Raster Area: 120 x 120 arcsec Step (DX, DY): 2 arcsec, 0 arcsec Raster Locations: 60 x 1 = 60 Exposure Time: 20 seconds Duration of Raster: 1524 seconds Number of Rasters: 1 Total Duration: 1524 seconds Line Selection: Mg VIII 315.02, Fe XIV 334.17, Fe XVI 360.76, Mg IX 368.06, He I 522.20, O IV 554.52, Ne VI 562.83, He I 584.33, O III 599.59, O V 629.73 Bins Across Line: 21 Telemetry/Compression: truncate to 12 bits Pointing: Sunspot TRACE Phase A: Channel: WL Exposure Time: 0.0032 seconds ? Image Area: 768 pixels x 768 pixels Pixel size: 0.5 arcsec Number of images: ~10 Pointing: Sunspot Phase B: Channel: 171 Exposure Time: 17 seconds Image Area: 768 pixels x 768 pixels Pixel size: 0.5 arcsec Number of images: ~2000 Duration: ~34200 seconds Pointing: Sunspot Phase A: Channel: WL Exposure Time: 0.0032 seconds ? Image Area: 768 pixels x 768 pixels Pixel size: 0.5 arcsec Number of images: ~10 Pointing: Sunspot MDI When possible: Doppler velocities and longitudinal magnetic field with high cadence EIT For a limited data set 171 channel observations with high cadence. JOINT CDS/TRACE/SUMER/MDI/EIT PROGRAMME JOP118 The Temperature Range of the Sunspot 3-minute Oscillations Per Maltby, Nils Brynildsen, Olav Kjeldseth-Moe, ITA, University of Oslo Richard A. Shine, Lockheed Palo Alto Research Laboratory Klaus Wilhelm, Max-Planck-Institut fur Aeronomie, Germany Received 25 December 1999 Modified 18 April 2001 In this update of JOP118 it is assumed that SUMER will not be available for observations on the solar disk. Scientific Justification: This programme builds on the knowledge obtained from JOP018 about the 3-minute oscillations above sunspots, see Brynildsen et al. 1999, ApJ 511, L121, Brynildsen et al. 1999, ApJ 517, L159, Brynildsen et al. 2000, Solar Phys., 191, 129, Maltby et al. 1999, Solar Phys., 190, 437. Briefly, simultaneous SUMER measurements of the intensity and the line-of-sight velocity show that the observations in the chromosphere and the transition region are compatible with the hypothesis that the oscillations are caused by upward-propagating acoustic waves. We have studied the intensity oscillations observed with the TRACE 171 channel above several sunspots. In some sunspots we find that the 171 intensity oscillations show a power spectrum with a maximum close to 6 mHz. These oscillations may be an extension of the sunspot transition region oscillations into the corona. However, this result is uncertain since the oscillations occur in an area where the emission in the 171 channel is weak, most likely because the coronal Fe IX/X emission is weak. Hence, without spectroscopic observations we cannot exclude the possibility that transition region lines, such as O VI at 172.93Å and 173.08Å contribute to the oscillations in the 171 channel. We plan to increase our knowledge by observations with: * CDS Normal Incidence Spectrometer * The wavelength bands of the CDS Grazing Incidence Spectrometer (GIS). The intension is to measure the relative contributions of such transition region lines as O VI 172.93Å, 173.08Å, Ne VII 465.22Å, and O V 760.40Å, to the intensity oscillations. * TRACE observations in the 171Å channel with high cadence. * MDI when possible: Doppler velocities and magnetic field measurements, with high spatial resolution and high cadence. CDS uses O_SPOT_B (var 1) series. Place the western rim of the sunspot umbra at the centre of the raster. The first study is a 120"x120" NIS raster (O_SPOT2). Next, after adjusting for solar rotation, let the slit drift across the sunspot for 4h35m, while the GIS study (O_SPOT10) is run. Then after a second adjustment for solar rotation let the slit drift across the sunspot for 4h9m, while the NIS study (O_SPOT11) is run. Then after a third adjustment for solar rotation the study series ends with a 120"x120" NIS raster (O_SPOT2). NOTE: The repeats of the rasters in mk_plan MUST NOT be modified. The GIS study O_SPOT10 has an y-offset that MUST NOT be modified. CDS (O_SPOT_B) Study Det. X-pos Y-pos # rasters Duration Total duration -------- --- ----- ----- --------- -------- -------------- O_SPOT2 NIS x0 y0 1 25m 24s 25m 24s O_SPOT10 GIS x0 y0-23" 6 45m 50s 4h 35m 0s O_SPOT11 NIS x0 y0 4 1h 2m 10s 4h 8m 40s O_SPOT2 NIS x0 y0 1 25m 24s 25m 24s ---------- 9h 34m 28s NIS Study: O_SPOT2 Spectrometer: Normal Incidence Slit: 2x240 arcsec Raster Area: 120x120 arcsec Step (DX, DY): 2 arcsec, 0 arcsec Raster Locations: 60 x 1 = 60 Exposure Time: 20 seconds Duration of Raster: 1524 seconds Number of Rasters: 1 Total Duration: 1524 seconds Line Selection: Mg VIII 315.02, Fe XIV 334.17, Fe XVI 360.76, Mg IX 368.06, He I 522.20, O IV 554.52, Ne VI 562.83, He I 584.33, O III 599.59, O V 629.73 Bins Across Line: 21 Telemetry/Compression: truncate to 12 bits Pointing: Sunspot GIS Study: O_SPOT10 Spectrometer: Grazing Incidence Slit: 4x4 arcsec Raster Area: 4x4 arcsec Step (DX, DY): 0 arcsec, 0 arcsec Raster Locations: 145 Exposure Time: 17 seconds Duration of Raster: 2750 seconds Number of Rasters: 6 Total Duration: 16500 seconds Line Selection: Full GIS output Pointing: Sunspot NIS Study: O_SPOT11 Spectrometer: Normal Incidence Slit: 2x240 arcsec Raster Area: 2x120 arcsec Step (DX, DY): 0 arcsec, 0 arcsec Raster Locations: 250 x 1 = 250 Exposure Time: 10 seconds Duration of Raster: 3730 seconds Number of Rasters: 4 Total Duration: 14920 seconds Line Selection: Fe XVI 360.76, Mg IX 368.06, O IV 554.52, Ne VI 562.83, He I 584.33, O V 629.73 Bins Across Line: 25 Telemetry/Compression: truncate to 12 bits Pointing: Sunspot NIS Study: O_SPOT2 Spectrometer: Normal Incidence Slit: 2x240 arcsec Raster Area: 120x120 arcsec Step (DX, DY): 2 arcsec, 0 arcsec Raster Locations: 60 x 1 = 60 Exposure Time: 20 seconds Duration of Raster: 1524 seconds Number of Rasters: 1 Total Duration: 1524 seconds Line Selection: Mg VIII 315.02, Fe XIV 334.17, Fe XVI 360.76, Mg IX 368.06, He I 522.20, O IV 554.52, Ne VI 562.83, He I 584.33, O III 599.59, O V 629.73 Bins Across Line: 21 Telemetry/Compression: truncate to 12 bits Pointing: Sunspot TRACE Phase A: Channel: WL Exposure Time: 0.0032 seconds ? Image Area: 768 pixels x 768 pixels Pixel size: 0.5 arcsec Number of images: 1 Duration: 0.0032 seconds Pointing: Sunspot Phase B: Channel: 171 Exposure Time: 17 seconds Image Area: 768 pixels x 768 pixels Pixel size: 0.5 arcsec Number of images: 160 Duration: ~34200 seconds Pointing: Sunspot Phase A: Channel: WL Exposure Time: 0.0032 seconds ? Image Area: 768 pixels x 768 pixels Pixel size: 0.5 arcsec Number of images: 1 Duration: 0.0032 seconds Pointing: Sunspot MDI When possible: Doppler velocities and longitudinal magnetic field with high cadence EIT For a limited data set 171 channel observations with high cadence.