solar astrophysics
I am interested to understand the solar rotation and its differential nature with respect to altitude and latitude using data of different nature and source. I do want to inspect any link between the solar rotation and solar activity cycle which ultimately leads to influence the Geo-Space whether.
The Sun can be viewed through many wavelengths, giving a picture of its various features. Images are obtained from a network of ground-based and space-based observatories that enable a comprehensive solar analysis. Detailed analyses of these images provide critical information for forecasting solar activity.
I have carried out a long term study of the coronal solar rotation using the disc integrated radio flux at 2.8 GHz data (observed at Dominion Radio Astrophysical Observatory, Penticton, British Columbia, Canada) of last 63 years (more than five solar cycles). The seven years data obtained from a ground-based observatory, known as Nobeyama Radio Observatory situated at Nobeyama, Japan, were also analyzed to investigate the differential rotation of lower corona. The almost rigid rotation across latitude of the mid corona were also examined and verified by analyzing Yohkoh (a Japanese space observatory, launched in Aug 1991 and lasted up to Dec 2001) data of its whole mission period.
I am now interested to study the differential rotation of transition region of solar atmosphere, a region intermediate between the chromosphere and corona. The ultraviolet images observed through the SOHO space observatory at four different wavelengths can be used for this purpose. Our initial result with EIT 171 nm images confirms our previous finding that at this height the rate of rotation is less differential than the Sun’s lower atmosphere but more than the corona.
Last summer, I visited the High Altitude Observatory, Boulder, CO, USA as visiting scientist for three weeks. During my scientific visit, I participated in collaborations with Dr. Steven Tomczyk, Assistant Director, High Altitude Observatory, Boulder, CO on the determination of coronal differential rotation using Mk3 and Mk4 data. This 30 years long data, taken almost continuously through coronagraph, are helpful to predict some long term oscillation in the solar rotation at different heights of the solar corona.
Such data provides the information about the outer corona. So far, I studied the solar rotation of the lower corona with the data available to me from different sources. The coronagraph data will give a new insight about the higher corona. This will surely helps us to prepare a complete model for the solar rotation of corona.
The Sun can be viewed through many wavelengths, giving a picture of its various features. Images are obtained from a network of ground-based and space-based observatories that enable a comprehensive solar analysis. Detailed analyses of these images provide critical information for forecasting solar activity.
I have carried out a long term study of the coronal solar rotation using the disc integrated radio flux at 2.8 GHz data (observed at Dominion Radio Astrophysical Observatory, Penticton, British Columbia, Canada) of last 63 years (more than five solar cycles). The seven years data obtained from a ground-based observatory, known as Nobeyama Radio Observatory situated at Nobeyama, Japan, were also analyzed to investigate the differential rotation of lower corona. The almost rigid rotation across latitude of the mid corona were also examined and verified by analyzing Yohkoh (a Japanese space observatory, launched in Aug 1991 and lasted up to Dec 2001) data of its whole mission period.
I am now interested to study the differential rotation of transition region of solar atmosphere, a region intermediate between the chromosphere and corona. The ultraviolet images observed through the SOHO space observatory at four different wavelengths can be used for this purpose. Our initial result with EIT 171 nm images confirms our previous finding that at this height the rate of rotation is less differential than the Sun’s lower atmosphere but more than the corona.
Last summer, I visited the High Altitude Observatory, Boulder, CO, USA as visiting scientist for three weeks. During my scientific visit, I participated in collaborations with Dr. Steven Tomczyk, Assistant Director, High Altitude Observatory, Boulder, CO on the determination of coronal differential rotation using Mk3 and Mk4 data. This 30 years long data, taken almost continuously through coronagraph, are helpful to predict some long term oscillation in the solar rotation at different heights of the solar corona.
Such data provides the information about the outer corona. So far, I studied the solar rotation of the lower corona with the data available to me from different sources. The coronagraph data will give a new insight about the higher corona. This will surely helps us to prepare a complete model for the solar rotation of corona.