|Author||Vats, H. O. ♦ Deshpande, M. R. ♦ Mehta, M. ♦ Shah, C. R. ♦ Shah, K. J.|
|Source||Indian Institute of Astrophysics|
|Subject Domain (in DDC)||Natural sciences & mathematics ♦ Physics|
|Subject Keyword||Radio emission ♦ Solar radio emission ♦ Coronal rotation|
|Description||The time series of solar radio emission at 2.8 GHz is analysed using correlation methods. The analysis showed that this type of time series can be used to infer the rotation period of the source (in this case solar corona). It is found that the correlograms have a very strong persistence of rotational modulation. These values are significantly lower than those reported earlier by other methods. The reasons for this difference are unknown.|
|Education Level||UG and PG|
|Learning Resource Type||Article|
|Publisher Institution||Astronomical Society of India|
|Size (in Bytes)||250.73 kB|
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