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  • Giridhar, S; Arellano Ferro, A; Mathias, P (Astronomical Society of India, 2001)
    Our abundance analysis of this post-AGB candidate star confirms that the HD 172481 is indeed a post-AGB star. It belongs to an important, but relatively rare class of post-AGB stars showing Li I features in their spectra. ...
  • Anilkumar, Nishtha; Birdie, C (2014)
  • Birdie, C (PETRONAS, in Collaboration with Librarians Association of Malaysia (PPM), 2005-05)
    Library Consortia evolved as a group activity over the years to empower the collective bargaining with publishers. The libraries felt the urge to collaborate not only for viable economics, but also for enhanced information ...
  • Moreno, H. W. B (Astronomical Society of India, 1920)
  • Moreno, H. W. B (Astronomical Society of India, 1918)
  • Moreno, H. W. B (Astronomical Society of India, 1919)
  • Indian Institute of Astrophysics (Indian Institute of Astrophysics, 1992-05)
  • Lee, W. A (Astronomical Society of India, 1915)
  • Shylaja, B. S (Astronomical Society of India, 1997)
  • Raju, K. P; Srikanth, R; Singh, J (Astronomical Society of India, 1999)
    Supergranulation is the surface manifestation of large scale solar convection. Since there is a strong correspondence between supergranulation pattern and Ca K chromospheric network, lifetimes and sizes may be obtained ...
  • Sahoo, B. K; Md. Islam, R; Das, B. P; Chaudhuri, R. K; Mukherjee, D (The American Physical Society, 2006-12)
    Atomic properties involving the low-lying excited D3/2,5/22 states in alkaline-earth-metal ions are of current interest in many different applications ranging from tests of physics beyond the standard model to astrophysics. ...
  • Antokhina, E. A; Srinivasa Rao, M; Parthasarathy, M (Elsevier B.V, 2011-04)
    Hipparcos photometric data for the massive O-type binary UW CMa were analysed within the framework of the Roche model. Photometric solutions were obtained for five mass ratios in the q = M2/M1 = 0.5–1.5 range. The system ...
  • Kumar, Brajesh; Pandey, S. B; Sahu, D. K; Vinko, J; Moskvitin, A. S; Anupama, G. C; Bhatt, V. K; Ordasi, A; Nagy, A; Sokolov, V. V; Sokolova, T. N; Komarova, V. N; Kumar, Brijesh; Bose, S; Roy, R; Sagar, R (Oxford University Press on behalf of the Royal Astronomical Society, 2013-05-01)
    We present the low-resolution spectroscopic and UBVRI broad-band photometric investigations of the Type IIb supernova (SN) 2011fu, discovered in UGC 01626. The photometric follow-up of this event was initiated a few days ...
  • Gangopadhyay, A; Misra, K; Pastorello, A; Sahu, D. K; Singh, M; Dastidar, R; Anapuma, G. C; Kumar, B; Pandey, S. B (Societe Royale des Sciences de Liege, 2018-04)
    Stripped-Envelope Supernovae constitute the sub-class of core-collapse supernovae that strip off their outer hydrogen envelope due to high stellar winds or due to interaction with a binary companion where mass transfer ...
  • Narayana, J. V; Viswanadham, P (Government Observatory, Madras, 1965-11)
  • Ivanov, V. P; Kjurkchieva, D. P; Srinivasa Rao, M (Astronomical Society of India, 2010-09)
    We propose a procedure for light-curve solutions of eclipsing binary stars in the Small Magellanic Cloud (SMC) for which photometric data have been obtained in the framework of the OGLE project. We also present a way of ...
  • Kulkarni, A. G; Abhyankar, K. D (Astronomical Society of India, 1977-12)
  • Chatterjee, S (Institute of Physics and IOP Publishing Limited, 2003-03)
    We study the scattering of light by a dielectric film with a periodic gradation of the refractive index along its thickness. The intensity of the scattered light is calculated in the scalar wave approximation, in which the ...
  • Venkata Suresh, Narra; Prasad, B. R (SPIE, 2021-07)
    To meet the proposed science goals of the Visible Emission Line Coronagraph on board the Aditya-L1 mission, the total scattered light should be less than 5 ppm (parts per million) of solar disk brightness over the field ...
  • Raveendran, A. V (D. Reidel Publishing Company, 1984-02)
    Photometry of the spectroscopic binary BD +25°2511 obtained during the 1981, 1982, and 1983 observing seasons shows that it is a variable with a period of about 3.5 days.

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