Study of inhomogeneties in the solar atmosphere a thesis submitted for the degree of Doctor of Philosophy in the faculty of science, Bangalore University, Bangalore R. Kariappa [Ph.D Thesis]
Material type:
TextPublication details: Bangalore Indian Institute of Astrophysics 1992Description: 99pSubject(s): Online resources: Dissertation note: Doctor of Philosophy Indian Institute of Astrophysics, Bangalore 1992 Summary: It has been recognised that the two resonance lines of singly ionized calcium viz. the Hand K lines (3968A and 3934A) can be used as the most reliable diagnostic indicators in the visible region of the spectrum to identify regions of chromospheric activity 'in the solar atmosphere. Since then~have been used extensively as a tool to study both the spatial and dynamical properties of the inhomogeneities in the solar chromosphere. Among the chromospheric inhomogeneities, the network, the bright points and the regions in between them characterize the quiet solar chromosphere. These regions are seen in emission and
they have a one to one correspondence with the underlying photospheric magnetic fields.
In this thesis work a study of the dynamical evolution of the Call H line profiles both at the sites of the arc sec structures namely
the bright points and the network boundary regions and the main role of 3-min oscillations in the heating of the quiet. solar chromosphere has been made. The basic data for this study is the time series spectra of 35 minute duration in the Cal I H line. This sequence spectra was obtained at the Vacuum Tower Telescope (VTT) of the Sacramento Peak Observatory,New Mexico on September 13, 1971 under exceptionally good seeing conditions, on a quiet region around the centre of the solar
disc. The spectra are of high spatial, spectral and temporal resolution.
| Item type | Current library | Shelving location | Call number | Status | Date due | Barcode |
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Thesis & Dissertations
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IIA Library-Bangalore | General Stacks | 043:52/ KAR (Browse shelf(Opens below)) | Available | 15401 |
Thesis Supervisors K. R. Sivaraman and M. N. Anandaram
Doctor of Philosophy Indian Institute of Astrophysics, Bangalore 1992
It has been recognised that the two resonance lines of singly ionized calcium viz. the Hand K lines (3968A and 3934A) can be used as the most reliable diagnostic indicators in the visible region of the spectrum to identify regions of chromospheric activity 'in the solar atmosphere. Since then~have been used extensively as a tool to study both the spatial and dynamical properties of the inhomogeneities in the solar chromosphere. Among the chromospheric inhomogeneities, the network, the bright points and the regions in between them characterize the quiet solar chromosphere. These regions are seen in emission and
they have a one to one correspondence with the underlying photospheric magnetic fields.
In this thesis work a study of the dynamical evolution of the Call H line profiles both at the sites of the arc sec structures namely
the bright points and the network boundary regions and the main role of 3-min oscillations in the heating of the quiet. solar chromosphere has been made. The basic data for this study is the time series spectra of 35 minute duration in the Cal I H line. This sequence spectra was obtained at the Vacuum Tower Telescope (VTT) of the Sacramento Peak Observatory,New Mexico on September 13, 1971 under exceptionally good seeing conditions, on a quiet region around the centre of the solar
disc. The spectra are of high spatial, spectral and temporal resolution.
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