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Browsing by Author "Krishnakumar, V"

Browsing by Author "Krishnakumar, V"

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  • Krishnakumar, V; Venkatakrishnan, P (European Southern Observatory, 1997-12)
    The result of blind deconvolution is a reconstructed image that has non positive intensities. The number of these non positive pixels has been used as an estimator for the departure from a perfect reconstruction. Simulations ...
  • van Ballegooijen, A. A; Nisenson, P; Noyes, R. W; Löfdahl, M. G; Stein, R. F; Nordlund, Å; Krishnakumar, V (The American Astronomical Society, 1998-12)
    The interaction of magnetic fields and convection is investigated in the context of the coronal heating problem. We study the motions of photospheric magnetic elements using a time series of high-resolution G-band and ...
  • Krishnakumar, V (Indian Institute of Astrophysics, 1998-08)
  • Krishnakumar, V (Indian Institute of Astrophysics, Bangalore, 1998-08)
  • Krishnakumar, V; Venkatakrishnan, P (Astronomical Society of the Pacific, 1998)
    The functional form of the long exposure OTF P(u,v) is known (Fried 1966; Kirshnakumar & Venkatakrishnan 1997a) and i(x,y) is what we record. The knowledge of P(u,v) is complete once ro is estimated. Our aim is to recover ...
  • Krishnakumar, V; Venkatakrishnan, P; Srikanth, R (Astronomical Society of India, 2000)
    We present the results of a preliminary analysis of a time series of a sequence of Ca II K bright points and G band bright points observed co-spatially and co-temporally. Inspection of these images shows that the larger ...
  • Krishnakumar, V; Venkatakrishnan, P (Indian Institute of Astrophysics, Bangalore, 1997)
    The photoheliograms obtained at Kodaikanal during the partial eclipse of the Sun on October 24, 1995 were digitised on a PDS microdensitometer. The lunar limb was used as a standard source for the digital reconstruction ...
  • Krishnakumar, V; Venkatakrishnan, P (Kluwer Academic Publishers, 1999-05)
    Periodic shaking or buffeting of magnetic flux tubes could generate magnetohydrodynamic waves which propagate along the flux tubes and dissipate energy in the chromosphere and/or corona. If we make an assumption that the ...

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