SOT: HOP 148 (Oscillations)
2009-12-16T10:55:00 to 2009-12-16T15:30:00
Science Goal: High Frequency Oscillations in the Photosphere and Lower Chromosphere
Program: HOP 148 Ca,G,BC, 55"x55", 2x2, Na IVDG 56"x82", 2x2, 3.5 hours
Target: disk center
xcen=-9 ycen=0
Instrument: SOT
HOP/JOP: 148
Description:
Request to SOT HOP Number 0148 In this observing sequence we plan to obtain the imaging observations at the disk center simultaneously with CaII and G-band along with the narrow-band filters at Na and MgII filters. Na and MgII filters will be used in IVDG mode. SOT (BFI): FILTERS: Ca II H, G-band and Blue continuum. FOV: 55"x55" CADENCE: As high cadence as possible. 16 second cadence would be good choice. DURATION: 3-4 hrs SOT (NFI): FILTERS: Na I D or MgbII shuttered IVDG. However, if the signal is not enough and long exposures are necessary, we would request for shutterless IVDG mode. We can sequentially use these filters. ie. First obtain a set of BFI observations with Na filter for about 2 hours and than change to MgII filter. FOV: 55" x 55" (to cover the BFI field of view) CADENCE: 1 minute. DURATION: 3-4 hrs (Same as BFI) Other Instruments: Scientific Objectives: Introduction: No single mechanism has been shown to release enough energy to heat the chromosphere and corona. To understand chromospheric and coronal heating the energy transport processes from the photosphere through higher atmospheric layers must be studied. Recent results show the importance of probing smaller temporal and spatial scales. The data provided by Hinode offers an invaluable opportunity for these types of studies. Primary Objectives: We propose to use time sequences of Hinode/SOT BFI and NFI filtergrams to describe the properties of oscillations and energy transport in the quiet Sun photosphere and lower chromosphere. We plan to study the space and time distributions of high frequency intensity oscillations in sequences of high cadence (30 seconds or less), simultaneous Ca II H-line, G-band and CN images. The propagation of the observed fluctuations will be investigated in different frequency bands roughly in the range 1 mHz f 24 mHz. Spatial patterns corresponding to enhancement or suppression of the oscillation amplitudes or their propagation will be identified and characterized. Observations in the lower chromosphere, obtained with the Na I and/or Mg II filters, will be used to relate the intensity oscillations to Doppler oscillations. They will further be used to determine the magnetic configurations associated with the spatial oscillatory patterns and with the corresponding velocity distributions in Doppler images.
