Varun Sahni
Articles written in Pramana – Journal of Physics
Volume 15 Issue 5 November 1980 pp 423-434 Astrophysics
Massless particles and cosmology
Post recombination density perturbations have been studied in a two-component matter-radiation universe. The study has been carried out for variable matter and radiation densities. The possibility of the existence of different kinds of neutrinos in addition to the electronic, muonic and taonic has been considered and conclusions have been drawn as to the upper limit of the radiation density for different values of Ω_{m}.
Volume 49 Issue 1 July 1997 pp 131-145 Astrophysics
The large scale structure of the universe: Dynamical and statistical aspects
The description of gravitational clustering is essentially statistical but its origin is dynamical. Hence both aspects of clustering: dynamical and statistical, must be understood in order to arrive at a proper appreciation of the subject of gravitational instability and the formation and evolution of the large scale structure of the Universe. Key dynamical aspects of gravitational clustering such as the Zeldovich approximation and its extension — the adhesion model are reviewed. Statistical indicators of clustering such as the correlation function and percolation theory, as applied to the large scale structure of the Universe have also been focussed on.
Volume 51 Issue 1-2 July 1998 pp 27-37
The inflationary Universe — From theory to observations
The inflationary Universe resolves some of the most outstanding issues of standard cosmology including the horizon and flatness problems and the origin of density fluctuations in the Universe. Inflationary models also predict the existence of a relic gravity wave background. Both gravity waves and density fluctuations induce fluctuations in the cosmic microwave background (CMB), the discovery of large angle anisotropies in the CMB having the scale invariant spectrum predicted by inflationary models has fuelled the hope that the inflationary scenario may indeed provide the correct description of the very early Universe. Upcoming large scale galaxy surveys (SDSS & 2dF) and CMB missions (MAP, Planck Surveyor) will further probe the inflationary scenario by throwing light on the origin and evolution of large scale structure in the Universe.
Volume 51 Issue 1-2 July 1998 pp 273-286
Astroparticle physics: Working group report
Subhendra Mohanty Varun Sahni S Chakraborty Ashok Goyal Sukanta Dutta Debajyoti Choudhury Shobhit Mahajan Amitabha Mukherjee Hatem Widyan Urjit Yajnik S Mohanty J A Grifols Uma Mahanta Sarira Sahu Varun Sahni Tarun Souradeep Albert Stebbins Ioav Waga Vikram Soni N Panchapakesan R Brandenberger
The astroparticle physics working group witnessed intense discussion and activity covering a broad range of topics ranging from supergravity and baryogenesis to compact stars and the large scale structure of the Universe. A summary of some of the subject areas in which collaborations were initiated during WHEPP-5 is presented below.
Volume 53 Issue 6 December 1999 pp 937-944 Cosmological Parameters
The cosmological constant revisited
I briefly review the observational evidence for a small cosmological constant at the present epoch. This evidence mainly comes from high redshift observations of Type 1a supernovae, which, when combined with CMB observations strongly support a flat Universe with Ω_{m} + Ω_{A} ⋍ 1. Theoretically a cosmological constant can arise from zero point vacuum fluctuations. In addition ultra-light scalar fields could also give rise to a Universe which is accelerating driven by a time dependent Λ-term induced by the scalar field potential. Finally a Λ dominated Universe also finds support from observations of galaxy clustering and the age of the Universe.
Volume 53 Issue 6 December 1999 pp 995-1000 Large Scale Structure and Gravitational Clustering
Pancakes and filaments in cosmological gravitational clustering
We consider the geometrical properties of a distribution of matter evolving under gravitational clustering. Such a distribution can be studied using standard statistical indicators such as the correlation function as well as geometrical descriptors sensitive to ‘connectedness’ such as percolation analysis and Minkowski functionals. Applying these methods to
Volume 55 Issue 1-2 July 2000 pp 43-52
The case for the cosmological constant
I present a short overview of current observational results and theoretical models for a cosmological constant. The main motivation for invoking a small cosmological constant (or A-term) at the present epoch has to do with observations of high redshift Type Ia supernovae which suggest an accelerating universe. A flat accelerating universe is strongly favoured by combining supernovae observations with observations of CMB anisotropies on degree scales which give the ‘best-fit’ values Θ_{A} ⋍ 0.7 and Θ_{m} ⋍ 0.3. A time dependent cosmological A-term can be generated by scalar field models with exponential and power law potentials. Some of these models can alleviate the ‘fine tuning’ problem which faces the cosmological
Volume 55 Issue 4 October 2000 pp 559-573
This talk presents a brief overview of recent results pertaining to the cosmological constant ‘A’. I summarize the observational situation focussing on observations of high redshift Type Ia supernovae which suggest A > 0. Observations of small angular anisotropies in the cosmic microwave background complement Type Ia supernovae observations and both CMB and Sn can be combined to place strong constraints on the value of A. The presence of a small A-term increases the age of the universe and slows down the formation of large scale structure. I also review recent theoretical attempts to generate a small A-term at the current epoch and a
Volume 94, 2019
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