After the First Three Minutes: The Story of Our Universe - download pdf or read online
By T. Padmanabhan
The evolution of our Universe and the formation of stars and galaxies are mysteries that experience lengthy questioned scientists. contemporary years have introduced new medical realizing of those profound and basic matters. In vigorous prose, Professor Padmanabhan paints an image of latest cosmology for the overall reader. not like different renowned books on cosmology, After the 1st 3 mins doesn't gloss over info, or draw back from explaining the underlying thoughts. as a substitute, with a lucid and casual sort, the writer introduces all of the suitable heritage after which conscientiously items jointly an attractive tale of the evolution of our Universe. Padmanabhan leaves the reader with a cutting-edge photo of scientists' present knowing in cosmology and a willing style of the buzz of this fast-moving technological know-how. all through, no arithmetic is used and all technical jargon is obviously brought and bolstered in a convenient thesaurus on the finish of the booklet. For normal readers who are looking to come to grips with what we actually do and do not find out about our Universe, this ebook presents 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 various 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 a couple of hundred well known technological know-how articles, a comic book strip serial and several other ordinary columns on astronomy, leisure arithmetic, and the background of technological know-how.
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Extra resources for After the First Three Minutes: The Story of Our Universe
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. Of course, in order to fuse two nuclei together, we have to overcome the electrostatic repulsion, and hence such a process can take place only at very high tern pera tures.
It turns out that particles like the electron, proton, etc. not only carry charge but also have another intrinsic property called the 'spin'. The spin has the effect of making the electron and proton behave like very tiny bar magnets. The force of interaction between the electron and proton is not only due to the electrical attraction but also because of the tiny magnetic force arising from the spins. The magnetic force is very small compared to the electrical force; but this tiny force does contribute to the energy of the electron in the hydrogen atom.
Bodies a1 room 1emperarure (300 K) emir mosl of 1he ndiation in the infnred. Bodies a1 higher remperalures, say, bcr"een 5000 K 10 7000 K (as in stars) emil a large amoun1 of 'isible ndiarion. It is also possible to reverse the above processes. Just as a particle and antiparticle can annihilate each other and produce photons, we can also produce particle-antiparticle pairs out of sufficiently energetic photons. 5 MeV, every once in a while a pair of photons will convert themselves into electron-positron pairs.
After the First Three Minutes: The Story of Our Universe by T. Padmanabhan