SOTSP: HOP 63 at E Limb
2008-01-27T13:10:35 to 2008-01-27T13:36:54
Science Goal: Magneto-acoustic shocks in the chromosphere and UV variability+Hinode Observations in Support of MOTH-II South Pole Observations
Program: Fast map, half height 12 sec cadence
Target: E Limb
xcen=-951 ycen=7
Instrument: SOTSP
HOP/JOP: 63
Description:
Scientific Objectives: We propose to establish a physical connection between photospheric magnetic fields and the variability of solar UV intensity based on magneto-acoustic shocks produced by leaking p modes in magnetic regions. Motivating Science: The Magneto-Optical filter at Two Heights (MOTH) experiment has played an crucial role in our understanding of magnetoatmospheric (MA) waves and their interaction with the ever changing magnetic field (e.g., Jefferies et al. 2006, ApJL, 648, 151) by simultaneously observing Doppler signals at two ""heights"" in the solar chromosphere. Joint Hinode/SOT observations will provide fantastic observational detail for MOTH-II - allowing the potential combination of wave and magnetic field evolution at granular and supergranular scales. By choosing a limb and disk target with modest length timeseries (~4hrs in length) we will be able to address a broad range of chromospheric wave phenomena (including those mentioned above) and get a new (more accurate) multi-point estimate of the wave energy flux in and through the quiet chromosphere. Solar Optical Telecope 1. NFI: [2x2 pixel binning (~0.3"" resolution) using 1kx1k of detector] - Halpha 6562.8 Dopplergrams at approx. (+- 204 mA) at 20s cadence [on disk - wave phenomena typically have ~3-5min periods] - Halpha 6562.8 Dopplergrams at approx. (+- 408 mA) at 20s cadence [for limb study - horizontal coupling, straws and spicules] - Na I D 5890.6 Dopplergrams at approx. (+- 156 mA) at 20s cadence - Mg I b Dopplergrams at approx. (+- 114 mA) at 20s cadence - Each sequence should be started and finished with both a Mg Ib and Na ID magnetogram note: SOT Na ID magnetograms can be ""calibrated"" by MOTH II magnetograms of the same line]. 2. BFI: [2x2 pixel binning (~0.3"" resolution) using 1kx1k of detector] - Ca II H imaging with relatively long exposure (~300ms) to enhance appearance of dynamic ""straws"" at a cadence of ~10s. - Would like one sequence of Ca IIH [at the limb]. - Removal of this element for on disk will give better NFI cadence [by ~3s] and be able to run sequences longer. 3. SP: Fast Maps [0.32"" spatial resolution]. The SP map will be used to infer the field topology through inversions and extrapolations. - Repeated rapid rastering of target region at ~0.32"" spatial resolution with step size of (0.32""). *NFI - obtain one disk center sequence with at least two positions in the wings of Mg I B (+- TBD), and or Na 1 D (+- TBD), for more accurate determination of wave energy flux through chromosphere. This alone would be a truly unique observation.
Scientific Objectives: We propose to establish a physical connection between photospheric magnetic fields and the variability of solar UV intensity based on magneto-acoustic shocks produced by leaking p modes in magnetic regions. Motivating Science: The Magneto-Optical filter at Two Heights (MOTH) experiment has played an crucial role in our understanding of magnetoatmospheric (MA) waves and their interaction with the ever changing magnetic field (e.g., Jefferies et al. 2006, ApJL, 648, 151) by simultaneously observing Doppler signals at two "heights" in the solar chromosphere. Joint Hinode/SOT observations will provide fantastic observational detail for MOTH-II - allowing the potential combination of wave and magnetic field evolution at granular and supergranular scales. By choosing a limb and disk target with modest length timeseries (~4hrs in length) we will be able to address a broad range of chromospheric wave phenomena (including those mentioned above) and get a new (more accurate) multi-point estimate of the wave energy flux in and through the quiet chromosphere. Solar Optical Telecope 1. NFI: [2x2 pixel binning (~0.3" resolution) using 1kx1k of detector] - Halpha 6562.8 Dopplergrams at approx. (+- 204 mA) at 20s cadence [on disk - wave phenomena typically have ~3-5min periods] - Halpha 6562.8 Dopplergrams at approx. (+- 408 mA) at 20s cadence [for limb study - horizontal coupling, straws and spicules] - Na I D 5890.6 Dopplergrams at approx. (+- 156 mA) at 20s cadence - Mg I b Dopplergrams at approx. (+- 114 mA) at 20s cadence - Each sequence should be started and finished with both a Mg Ib and Na ID magnetogram note: SOT Na ID magnetograms can be "calibrated" by MOTH II magnetograms of the same line]. 2. BFI: [2x2 pixel binning (~0.3" resolution) using 1kx1k of detector] - Ca II H imaging with relatively long exposure (~300ms) to enhance appearance of dynamic "straws" at a cadence of ~10s. - Would like one sequence of Ca IIH [at the limb]. - Removal of this element for on disk will give better NFI cadence [by ~3s] and be able to run sequences longer. 3. SP: Fast Maps [0.32" spatial resolution]. The SP map will be used to infer the field topology through inversions and extrapolations. - Repeated rapid rastering of target region at ~0.32" spatial resolution with step size of (0.32"). *NFI - obtain one disk center sequence with at least two positions in the wings of Mg I B (+- TBD), and or Na 1 D (+- TBD), for more accurate determination of wave energy flux through chromosphere. This alone would be a truly unique observation.
Scientific Objectives: We propose to establish a physical connection between photospheric magnetic fields and the variability of solar UV intensity based on magneto-acoustic shocks produced by leaking p modes in magnetic regions. Motivating Science: The Magneto-Optical filter at Two Heights (MOTH) experiment has played an crucial role in our understanding of magnetoatmospheric (MA) waves and their interaction with the ever changing magnetic field (e.g., Jefferies et al. 2006, ApJL, 648, 151) by simultaneously observing Doppler signals at two "heights" in the solar chromosphere. Joint Hinode/SOT observations will provide fantastic observational detail for MOTH-II - allowing the potential combination of wave and magnetic field evolution at granular and supergranular scales. By choosing a limb and disk target with modest length timeseries (~4hrs in length) we will be able to address a broad range of chromospheric wave phenomena (including those mentioned above) and get a new (more accurate) multi-point estimate of the wave energy flux in and through the quiet chromosphere. Solar Optical Telecope 1. NFI: [2x2 pixel binning (~0.3" resolution) using 1kx1k of detector] - Halpha 6562.8 Dopplergrams at approx. (+- 204 mA) at 20s cadence [on disk - wave phenomena typically have ~3-5min periods] - Halpha 6562.8 Dopplergrams at approx. (+- 408 mA) at 20s cadence [for limb study - horizontal coupling, straws and spicules] - Na I D 5890.6 Dopplergrams at approx. (+- 156 mA) at 20s cadence - Mg I b Dopplergrams at approx. (+- 114 mA) at 20s cadence - Each sequence should be started and finished with both a Mg Ib and Na ID magnetogram note: SOT Na ID magnetograms can be "calibrated" by MOTH II magnetograms of the same line]. 2. BFI: [2x2 pixel binning (~0.3" resolution) using 1kx1k of detector] - Ca II H imaging with relatively long exposure (~300ms) to enhance appearance of dynamic "straws" at a cadence of ~10s. - Would like one sequence of Ca IIH [at the limb]. - Removal of this element for on disk will give better NFI cadence [by ~3s] and be able to run sequences longer. 3. SP: Fast Maps [0.32" spatial resolution]. The SP map will be used to infer the field topology through inversions and extrapolations. - Repeated rapid rastering of target region at ~0.32" spatial resolution with step size of (0.32"). *NFI - obtain one disk center sequence with at least two positions in the wings of Mg I B (+- TBD), and or Na 1 D (+- TBD), for more accurate determination of wave energy flux through chromosphere. This alone would be a truly unique observation.
wavelength: 6302A Continuum Intensity cadence: 0.08 min fov: 1,81 images: 403 JavaScript Landing Page
