By T. Padmanabhan
ISBN-10: 0521620392
ISBN-13: 9780521620390
The evolution of our Universe and the formation of stars and galaxies are mysteries that experience lengthy wondered scientists. fresh years have introduced new clinical realizing of those profound and basic matters. In full of life prose, Professor Padmanabhan paints an image of latest cosmology for the final reader. in contrast to different well known books on cosmology, After the 1st 3 mins doesn't gloss over information, or shrink back from explaining the underlying ideas. in its place, with a lucid and casual sort, the writer introduces all of the suitable heritage after which rigorously items jointly an enticing tale of the evolution of our Universe. Padmanabhan leaves the reader with a cutting-edge photo of scientists' present figuring out in cosmology and a prepared flavor of the buzz of this fast-moving technological know-how. all through, no arithmetic is used and all technical jargon is obviously brought and strengthened in a convenient thesaurus on the finish of the ebook. For basic readers who are looking to come to grips with what we actually do and do not learn about our Universe, this publication offers an exhilarating and uncompromising learn. Thanu Padmanabhan is a Professor at Inter-University Centre for Astronomy and Astrophysics in Pune, India. he's the recipient of diverse awards and writer of 3 books, constitution Formation within the Universe (Cambridge, 1994), Cosmology and Astrophysics via difficulties (Cambridge, 1996), and, including J.V. Narlikar, Gravity, Gauge Theories and Quantum Cosmology. he's additionally the writer of multiple hundred renowned technology articles, a comic book strip serial and a number of other general columns on astronomy, leisure arithmetic, and the heritage of technological know-how.
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Extra info for After the First Three Minutes: The Story of Our Universe
Example text
Such a process is preferred by nature, and elements heavier than iron - in general - release energy when split up. The situation is reversed for elements which are lighter than iron. Here we can increase the binding energy by fusing two light elements together. Once again such a process is preferred, and energy will be released in the nuclear fusion oflighter elements. In summary, we may say that heavier elements like uranium will release energy when undergoing fission while lighter elements like hydrogen will release energy during fusion.
This suggests that elements heavier than iron will behave differently, compared to those lighter than iron, as far as nuclear processes are concerned. In addition to this average behaviour, one can also see significant spikes at some particular elements. For example, helium has an extremely stable nuclear structure, with a fairly high binding energy. Since the nuclear forces provide the binding for the constituents of the atomic nucleus, we can split the atomic nucleus by overcoming these forces.
But you will recall from the above discussion that, at any given temperature, there will always be some radiation present which we called the thermal radiation.
After the First Three Minutes: The Story of Our Universe by T. Padmanabhan
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