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SUMMARY:Mysteries of the solar chromosphere explored using the high-resolu
 tion observations - Juie Shetye (University of Warwick)
DTSTART:20180205T140000Z
DTEND:20180205T150000Z
UID:TALK96187@talks.cam.ac.uk
CONTACT:Dr. Yufeng Lin
DESCRIPTION:The solar chromosphere serves as a bridging layer between the 
 photosphere and the corona and is often neglected. This dynamic layer is f
 illed with a plethora of features that vary at small time and space scales
 . With the advent of new and improved methods of observations we are not o
 nly able to unveil new features but also understand the physical propertie
 s of others. Here I present a statistical study of spicules obtained from 
 spectral images\, taken from the CRISP instrument at the Swedish 1-m Solar
  Telescope in H-alpha 656.28 nm wavelength. Remarkably\, many of these fas
 t spicules display apparent unphysical velocities above 5000 km/s\, very s
 hort lifetimes of up to 20 s combined with width or thickness of 100 km an
 d apparent lengths of around 3500 km. We interpret the observations as mas
 s motions (of flux tubes\, maybe sheets) that appear in the field-of-view 
 of CRISP’s 0.0060 nm filters in the line of sight\, along with their pro
 jection as we scan. Furthermore\, such spicules exhibited transverse motio
 n associated with these structures\, which in some cases could be related 
 to high-frequency magneto-hydrodynamic (MHD) kink-waves. Can these high-fr
 equency waves be transferred to the solar corona and contribute to coronal
  heating? MHD waves are not only responsible for the generation and evolut
 ion of these events but also are responsible for energy and mass transport
 . At present\, MHD LareXd simulations to be carried at CFSA\, hope to prov
 ide some insight into the dynamics of such events. Are spicules the only e
 vents in the chromosphere? I will show dynamic events that swirl and can f
 urther explain aspects of chromospheric dynamics never understood before. 
  \n\nObservations of small-scale events in the chromosphere further highli
 ght the need to understand the plasma environment associated with the even
 ts. We still don’t know where the Hydrogen lines are formed\, or if a fe
 ature observed in the Calcium line\, occurs at the corona or the chromosph
 ere.  This raises the need to develop a thorough radiative transfer code (
 e.g expansion of CHIANTI) for the chromosphere. In addition\, the current 
 work presented already tests the limits of current telescopes in terms of 
 the temporal and spatial resolution. The answer to exploring the depth of 
 chromosphere lies in building next-generation solar physics observatories 
 such as DKIST that have 3 times more spatial resolution than CRISP and muc
 h higher temporal resolution.
LOCATION:MR14\,  Centre for Mathematical Sciences\, Wilberforce Road\, Cam
 bridge
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