SOTSP: HOP363 w/BBSO
2018-10-06T15:04:38 to 2018-10-06T15:58:58
Science Goal: High Resolution Multi-Wavelength Study of Solar Pores
Program: Normal Map, 100"x164", 1-side, Q75
Target: Plage
xcen=596 ycen=-18
Instrument: SOTSP
HOP/JOP: 363
Description:
The main objective of this observing proposal is to compare small-scale magnetic and flow fields in the vicinity of pores in different environments and at various stages of evolution. The need to understand the different mechanisms responsible for the formation of quiet-Sun and active region pores motivates this work. The thin, dark lines, so-called ?hairs? are often seen extending from the pores to the closest neighboring granules (Scharmer et al. 2002, Nature 420, 151). What are the implications of such corrugated boundaries for the stability of flux tubes? Are they a first indication of penumbra formation? The 1.6 m Godde Solar Telescope (GST) at Big Bear Solar Observatory will be furnishing high-resolution images in G-band (Broad-band Filter Imager, BFI) with the spectra in H? and Ca II NIR from Fast Imaging Solar Spectrograph (FISS) covering chromospheric layers. The photospheric magnetic field information would be obtained using 1565 nm spectropolarimetric spectra from Near-infrared Imaging Spectro-polarimeter (NIRIS). From Hinode we will be requesting SOT/SP Sepctropolarimetric data in 6302.05 nm line.
The main objective of this observing proposal is to compare small-scale magnetic and flow fields in the vicinity of pores in different environments and at various stages of evolution. The need to understand the different mechanisms responsible for the formation of quiet-Sun and active region pores motivates this work. The thin, dark lines, so-called ?hairs? are often seen extending from the pores to the closest neighboring granules (Scharmer et al. 2002, Nature 420, 151). What are the implications of such corrugated boundaries for the stability of flux tubes? Are they a first indication of penumbra formation? The 1.6 m Godde Solar Telescope (GST) at Big Bear Solar Observatory will be furnishing high-resolution images in G-band (Broad-band Filter Imager, BFI) with the spectra in H? and Ca II NIR from Fast Imaging Solar Spectrograph (FISS) covering chromospheric layers. The photospheric magnetic field information would be obtained using 1565 nm spectropolarimetric spectra from Near-infrared Imaging Spectro-polarimeter (NIRIS). From Hinode we will be requesting SOT/SP Sepctropolarimetric data in 6302.05 nm line.
wavelength: 6302A Continuum Intensity cadence: 0 min fov: 92,162 images: 601 JavaScript Landing Page
