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Browsing IIAP Publications by Title

Browsing IIAP Publications by Title

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  • Solar activity 
    Das, A. K (Royal Astronomical Society, 1956)
  • Solar activity 
    Laurie, P. S; Bappu, M. K. V (Royal Astronomical Society, 1970-12)
  • Solar activity 
    Gokhale, M. H (Indian Institute of Astrophysics, Bangalore, 1988)
    Sun could have had a nice and perfect spherical symmetry in its atmosphere and probably no variations on time scales smaller than hundreds of thousands of years if (i) the energy produced in its core could be transported ...
  • Solar activity (Report on progress of astronomy) 
    Das, A. K (Royal Astronomical Society, 1954)
  • Solar activity (Report on progress of astronomy) 
    Das, A. K (Royal Astronomical Society, 1951)
  • The Solar Activity Monitor Network – SAMNet 
    Erdelyi, Robertus; Korsos, Marianna B; Huang, Xin; Yang, Yong; Pizzey, Danielle; Wrathmall, Steven A; Hughes, Ifan G; Dyer, Martin J; Dhillon, Vikram S; Belucz, Bernadett; Brajsa, Roman; Chatterjee, Piyali; Cheng, Xuewu; Deng, Yuanyong; Dominguez, Santiago Vargas; Joya, Raul; Gömöry, Peter; Gyenge, Norbert G; Hanslmeier, Arnold; Kucera, Ales; Kuridze, David; Li, Faquan; Liu, Zhong; Xu, Long; Mathioudakis, Mihalis; Matthews, Sarah; McAteer, James R.T; Pevtsov, Alexei A; Pötzi, Werner; Romano, Paolo; Shen, Jinhua; Temesvary, Janos; Tlatov, Andrey G; Triana, Charles; Utz, Dominik; Veronig, Astrid M; Wang, Yuming; Yan, Yihua; Zaqarashvili, Teimuraz; Zuccarello, Francesca (EDP Sciences, 2022-06)
    The Solar Activity Magnetic Monitor (SAMM) Network (SAMNet) is a future UK-led international network of ground-based solar telescope stations. SAMNet, at its full capacity, will continuously monitor the Sun’s intensity, ...
  • Solar Activity-Prominences 
    Bappu, M. K. V (Royal Astronomical Society, 1963-09)
  • Solar Activity-Prominences 
    Bappu, M. K. V (1964-09)
  • Solar and Stellar Convection 
    Narasimha, D (Indian Institute of Astrophysics, Bangalore, 1988)
    The flow field in stellar convection zones, characterised by high Rayleigh number, low Prandtl number and large Reynolds number, is time dependent and turbulent, consisting of eddies having a range of scale-lengths upto ...
  • Solar astronomy at high altitude 
    Hasan, S. S; Bagare, S. P; Rangarajan, K. E (Indian National Science Academy, 2014-11)
    A major project called the National Large Solar Telescope (NLST) has been proposed for pursuing Solar Astronomy at High Altitude. The project envisages the development of a state-of-the-art 2-m class telescope to carry ...
  • Solar asymmetry and sun-earth connections 
    Georgieva, K; Kirov, B; Javaraiah, J (European Space Agency, 2003-09)
    The effect of solar activity on climate depends on the North-South solar activity asymmetry: the correlation between solar activity and a number of meteorological elements has opposite signs for predominantly more active ...
  • Solar Convection and Oscillations 
    Chitre, S. M (Indian Institute of Astrophysics, Bangalore, 1986)
    A wide variety of gravity and acoustic wave motions have been detected at the surface of the Sun as Doppler shifts of spectral lines. These velocity field provide a valuable probe for studying the internal solar structure ...
  • The solar corona in the He II line 
    Shylaja, B. S (Indian Institute of Astrophysics, 1997)
    The corona of the sun was photographed with the filters centered at 4686Å, 4921 Å and 5812 Å, on 24th October 1995, during totality at Nim Ka Thana The PDS scans of these Images were presented The differences In the contours ...
  • The Solar Corona of July 20, 1963 
    Bappu, M. K. V; Bhatnagar, A (Kodaikanal Observatory, 1969-01)
    The total solar eclipse of July 20, 1963 was observed at the AAVSO site near Wilton, Malne, U.S.A, where totality lasted for 58 seconds. Pictures of the corona were obtained with a camera of focal length 57 cm on Kodak ...
  • Solar coronal bright points observed with the VLA 
    Habbal, S. R; Ronan, R. S; Withbroe, G. L; Shevgaonkar, R. K; Kundu, M. R (The American Astronomical Society, 1986-07)
    The first observations of solar coronal bright points made at 20-cm wavelength with the VLA are reported. The brightness temperature of the sources observed varies between 1 and 5 x 10 to the 5th K. The observations indicate ...
  • Solar Coronal Density Turbulence and Magnetic Field Strength at the Source Regions of Two Successive Metric Type II Radio Bursts 
    Ramesh, R; Kathiravan, C; Anshu Kumari (American Astronomical Society, 2023-01-20)
    We report spectral and polarimeter observations of two weak, low-frequency (≈85–60 MHz) solar coronal type II radio bursts that occurred on 2020 May 29 within a time interval ≈2 minutes. The bursts had fine structures, ...
  • Solar coronal magnetic fields and sensitivity requirements for spectropolarimetry channel of VELC onboard Aditya-L1 
    Sasikumar Raja, K; Venkata Suresh, Narra; Singh, J; Prasad, B. R (Elsevier, 2022-01-01)
    Understanding solar coronal magnetic fields is crucial to address the long-standing mysteries of the solar corona and solar wind. Although routine photospheric magnetic fields (MFs) are available for decades, coronal MFs ...
  • Solar coronal magnetic fields derived using seismology techniques applied to omnipresent sunspot waves 
    Jess, D. B; Reznikova, V. E; Ryans, R. S. I; Christian, D. J; Keys, P. H; Mathioudakis, M; Mackay, D. H; Krishna Prasad, S; Banerjee, D; Grant, S. D. T; Yau, S; Diamond, C (Nature Publishing Group, 2016-02)
    Sunspots on the surface of the Sun are the observational signatures of intense manifestations of tightly packed magnetic field lines, with near-vertical field strengths exceeding 6,000 G in extreme cases. It is well accepted ...
  • Solar coronal rotation determined by X-ray bright points in Hinode/XRT and Yohkoh/SXT full-disc images 
    Kariyappa, R (EDP Sciences, 2008-09)
    Aims. Our aim is to identify and trace the X-ray bright points (XBPs) over the disc and use them as tracers to determine the coronal rotation. This investigation will help to clarify and understand several issues: (i) ...
  • The solar cycle 
    Javaraiah, J; Rozelot, J. P; Bertello, L (Hindawi Publishing Corporation, 2012-06)
    The Sun provides variable energetic and magnetic field input to the conditions in the heliosphere which directly affect the magnetosphere. In particular, the Sun's variable magnetic fields constitute a rich source for ...

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