SOTSP: HOP 212 Support @ Disk Center
2012-06-22T10:14:35 to 2012-06-22T10:38:51
Science Goal: HOP 212 Support @ Disk Center
Program: Fast map, 123"x123", 1-side CCD
Target: Quiet Sun
xcen=12 ycen=8
Instrument: SOTSP
HOP/JOP: 212
Description:
Request to SOT HOP Number 0212 No request Other Instruments: Scientific Objectives: The connection of the coronal magnetic field with the solar surface through the chromosphere leads to interesting dynamics in the chromospheric structure. It is highly likely that the origin of the fast wind/stream of outflowing plasma lies within small-scale dynamic processes which appear continuously and frequently in the chromosphere of coronal holes and the quiet Sun, namely, spicules and swirls. Over the past decade there has been a resurgence in the study of spicules. Recent observations have lead us to conclude that there are two distinct varieties of spicule, namely, slower type-I (i.e. mottles, dynamic fibrils, Halpha spicules etc.) and faster type-II (RBEs: Rapid Blue-shift Excursions on-disk). RBEs are observed in both Halpha 6563 A and Ca ii 8542 A wavelength channels. Such events dominate the dynamics of the chromosphere in coronal holes and quiet Sun. Joint SDO (Solar Dynamics Observatory: 2010) and Hinode observations have revealed that fast spicules are the source of hot plasma channelling into the corona. Understanding these small-scale jet-like structures of the chromosphere allows us to address the heating of the corona and the acceleration of the fast solar wind in coronal holes. A statistical approach to RBE studies can tell how much much energy they contribute to coronal heating which remains an open question. With a statistical approach to RBEs we can place constraints upon the mass outflow rate with respect to their contribution to the fast solar wind. Recently, vortex-driven swirl structures have been discovered in the solar chromosphere. Chromospheric swirls are believed to be formed by rapidly rotating magnetic flux structures whichform as a direct result of the vortex flows in the photosphere. We consider that these structures may, also, be efficiently channelling energy from the photosphere through to the solar corona. These swirl structures may have a corresponding response in the atmospheric layers above. Not a lot is currently known about swirls in the scientific literature. More statistics concerning disk centre swirls (i.e. avoiding any projection issues) in the Quiet Sun (i.e. ideal for observing swirls and to minimize any line blending issues with Hinode/EIS) are required.
wavelength: 6302A Continuum Intensity cadence: 0 min fov: 121,122 images: 382 JavaScript Landing Page
