Articles written in Resonance – Journal of Science Education
Volume 6 Issue 1 January 2001 pp 70-72 Classroom
Volume 11 Issue 4 April 2006 pp 91-99 Classroom
Volume 21 Issue 1 January 2016 pp 89-92 Book Review
Volume 22 Issue 1 January 2017 pp 91-93 Book Review
Volume 22 Issue 3 March 2017 pp 225-235 General Article
Gravitation, the universal attractive force, acts upon all matter(and radiation) relentlessly. Left to itself, gravity wouldpull everything together, and the Universe would be nothingbut a gigantic black hole. Nature throws almost every bit ofphysics – rotation, magnetic field, heat, quantum effects andso on, at gravity to escape such a fate. In this series of articles,we shall explore systems where the eternal pull of gravity hasbeen held off by one or another such means.
Volume 22 Issue 4 April 2017 pp 389-398 General Article
Gravitation, the universal attractive force, acts upon all matter(and radiation) relentlessly. Stable extended structurescan exist only when gravity is held off by other forces of nature.This series of articles explores this interplay, looking atobjects that just missed being stars in this particular installment.
Volume 22 Issue 5 May 2017 pp 475-484 General Article
During its active lifetime, a star burns its nuclear fuel, andgravitation is held off by the pressure of the heated gas. Gravityshould take over once this fuel is exhausted unless someother agency saves the star from such a fate. Low mass starsfind peace as ‘white dwarfs’ when the electrons settle intoa Fermi degenerate phase where the pressure of degenerateelectrons balance the gravitational pressure.
Volume 22 Issue 6 June 2017 pp 597-610 General Article
A star burns its nuclear fuel and balances gravitation by thepressure of the heated gas, during its active lifetime. Afterthe exhaustion of the nuclear fuel, a low mass star findspeace as a ‘white dwarf’, where the pressure support againstgravitation is provided by Fermi-degenerate electrons. However,for massive stars, the gravitational squeeze becomes sosevere that in the final phase of evolution, the average densityapproximately equals the nuclear density. At such densities,most of the protons combine with electrons to convertthemselves into neutrons. A `neutron star', composed of suchneutron-rich material, is host to some fascinating physics arisingout of its amazingly compact state of matter (where a solarmass is packed inside a sphere of radius ∼ 10Km).