SOTSP: HOP 302 Pores @ AR12526
2016-03-29T17:49:10 to 2016-03-29T18:59:58
Science Goal: Target of Opportunity observations of a pore
Program: HOP 302 9x81", 72 sec, centered, repeats
Target: Active Region
xcen=-160 ycen=9
Instrument: SOTSP
HOP/JOP: 302
Description:
Request to SOT HOP Number 0302 *Target of Opportunity observations of a pore. * Very Fast Map observing mode (similar to HOP 243 with 9 arcsec wide FOV and 73 sec cadence) using both sides of CCD. SP 0x15b *DURATION: 1 hours *REPEATS: 3 x with +/- 5 arcsec offset of X in order to have a better chance of pointing at small pore *Height along the slit should be 82 arcsec minimum to allow accurate removal of drifts. *Perhaps reset correlation tracker every hour or two as the stability might be worth the 1.5 minute data gap? Other Instruments: IRIS Requests: Yes, we would like co-temporal observations with IRIS if possible. What was run with HOP 272 (similar to this but with sunspots as targets) was an OBS of 3620257130 or 3820257177 (?). A large 8 step sparse raster (1" steps, i.e., not a full spatial coverage) with 4s exposure times. That would lead to a raster scan that covers 8" x 120" with a raster cadence of 43 seconds. To boost the signal-to-noise of the FUV spectra, we could sum those by 2 in the spectral dimension. This will give C II, Si IV and Mg II h/k slit jaw images with a cadence of 21 seconds for each of the filters. Scientific Objectives: Main Objective: I'd like to acquire a time series of a small- to medium- sized pore with SP data to see if there are any oscillations of the magnetic field strength, inclination, intensity or area that could be indicative of MHD waves in the photosphere. Scientific Justification: MHD waves are thought to be a likely candidate for transporting heat in the solar atmosphere. The layer in which we can most successfully observe, ie, the photosphere, is also the layer in which the MHD wave amplitudes are small and mode-mixing and conversion of different types of waves makes observations messy. Nevertheless, it is important to utilize what is our best spectropolarimeter (SOT SP) available to the solar physics community to determine if the amplitudes of the MHD waves in the photosphere really are too small to be detected, as predicted by theory. We have acquired two nice data sets for time series (15 step fast map rasters) in sunspots in the last year and half using HOP 272. It would be excellent to run this type of observation with pores as targets since the weaker field strengths and smaller wave guides of pores will provide a distinctly different environment for wave propagation.
Request to SOT HOP Number 0302 *Target of Opportunity observations of a pore. * Very Fast Map observing mode (similar to HOP 243 with 9 arcsec wide FOV and 73 sec cadence) using both sides of CCD. SP 0x15b *DURATION: 1 hours *REPEATS: 3 x with +/- 5 arcsec offset of X in order to have a better chance of pointing at small pore *Height along the slit should be 82 arcsec minimum to allow accurate removal of drifts. *Perhaps reset correlation tracker every hour or two as the stability might be worth the 1.5 minute data gap? Other Instruments: IRIS Requests: Yes, we would like co-temporal observations with IRIS if possible. What was run with HOP 272 (similar to this but with sunspots as targets) was an OBS of 3620257130 or 3820257177 (?). A large 8 step sparse raster (1" steps, i.e., not a full spatial coverage) with 4s exposure times. That would lead to a raster scan that covers 8" x 120" with a raster cadence of 43 seconds. To boost the signal-to-noise of the FUV spectra, we could sum those by 2 in the spectral dimension. This will give C II, Si IV and Mg II h/k slit jaw images with a cadence of 21 seconds for each of the filters. Scientific Objectives: Main Objective: I'd like to acquire a time series of a small- to medium- sized pore with SP data to see if there are any oscillations of the magnetic field strength, inclination, intensity or area that could be indicative of MHD waves in the photosphere. Scientific Justification: MHD waves are thought to be a likely candidate for transporting heat in the solar atmosphere. The layer in which we can most successfully observe, ie, the photosphere, is also the layer in which the MHD wave amplitudes are small and mode-mixing and conversion of different types of waves makes observations messy. Nevertheless, it is important to utilize what is our best spectropolarimeter (SOT SP) available to the solar physics community to determine if the amplitudes of the MHD waves in the photosphere really are too small to be detected, as predicted by theory. We have acquired two nice data sets for time series (15 step fast map rasters) in sunspots in the last year and half using HOP 272. It would be excellent to run this type of observation with pores as targets since the weaker field strengths and smaller wave guides of pores will provide a distinctly different environment for wave propagation.
wavelength: 6302A Continuum Intensity cadence: 0.01 min fov: 9,81 images: 1744 JavaScript Landing Page
