SOTSP: HOP 74 QS Magnetic Field
2008-09-04T09:00:05 to 2008-09-04T09:23:02
Science Goal: Search for photospheric/chromospheric drivers of chromospheric penumbral micro-jets
Program: Normal map, 2.9"x82", no sum, HOP74
Target: Quiet Sun
xcen=-10 ycen=-1
Instrument: SOTSP
HOP/JOP: 0
Description:
HINODE SOT found sub-arcsec chromospheric activities, penumbral microjets, in sunspot penumbrae. Their very dynamical nature suggests that they are possibly driven by magnetic reconnection in the uncombed magnetic field configuration of penumbral filaments. The purpose of this observation is to detect a possible signature of sudden change of photospheric magnetic fields using Hinode SOT and the Fabry-Perot imaging spectro-polarimeter newly installed to SST at La Palma. So far, their temporal evolution and apparent velocity have been studied only using image sequences taken through the CaII H filter. It is important to directly measure velocities with Dopplergrams of chromospheric spectral lines. For this purpose, SOT can provide Dopplergrams in Na D with CaII H imaging. Diagnostic by SP is also important to know magnetic configuration around the footpoints of penumbral microjets. Another important question is what the transition region and coronal response to the penumbral microjets is. EIS and XRT observations together with SOT are essential to know the coronal and transition region response. (ref. Katsukawa et al. 2007, Science 318 (5856), 1594-1597)
HINODE SOT found sub-arcsec chromospheric activities, penumbral microjets, in sunspot penumbrae. Their very dynamical nature suggests that they are possibly driven by magnetic reconnection in the uncombed magnetic field configuration of penumbral filaments. The purpose of this observation is to detect a possible signature of sudden change of photospheric magnetic fields using Hinode SOT and the Fabry-Perot imaging spectro-polarimeter newly installed to SST at La Palma. So far, their temporal evolution and apparent velocity have been studied only using image sequences taken through the CaII H filter. It is important to directly measure velocities with Dopplergrams of chromospheric spectral lines. For this purpose, SOT can provide Dopplergrams in Na D with CaII H imaging. Diagnostic by SP is also important to know magnetic configuration around the footpoints of penumbral microjets. Another important question is what the transition region and coronal response to the penumbral microjets is. EIS and XRT observations together with SOT are essential to know the coronal and transition region response. (ref. Katsukawa et al. 2007, Science 318 (5856), 1594-1597)
wavelength: 6302A Continuum Intensity cadence: 0.01 min fov: 3,81 images: 263 JavaScript Landing Page
