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After the First Three Minutes: The Story of Our Universe by T. Padmanabhan PDF

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. contemporary years have introduced new medical figuring out of those profound and primary concerns. In energetic prose, Professor Padmanabhan paints an image of latest cosmology for the overall reader. not like different well known books on cosmology, After the 1st 3 mins doesn't gloss over info, or draw back from explaining the underlying techniques. as an alternative, with a lucid and casual kind, the writer introduces all of the suitable historical past 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 prepared 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 strengthened in a convenient thesaurus on the finish of the e-book. For basic readers who are looking to come to grips with what we actually do and do not find out about our Universe, this ebook offers a thrilling 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 well known technology articles, a comic book strip serial and a number of other standard columns on astronomy, leisure arithmetic, and the background of technological know-how.

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If the energy of the photon is different, then it will not be absorbed by the hydrogen atom. spectrum. By studying an absorption spectrum we can determine the composition of elements in regions through which radiation has been passing. 6 eV. What happens if we shine photons with higher energy, say 15 eV, on the hydrogen atom? To answer this question we must remember that a free electron which is not moving has zero energy and a free electron moving with some speed has positive energy. 6 eV on a hydrogen atom, then the electron can absorb one such photon and reach the zero energy level.

When a charged particle and its antiparticle collide with each other, their total energy can be converted into radiation. For example, when an electron and positron collide, they annihilate each other, and their total energy is emitted as radiation in the form of two photons. S MeV. A photon with this energy will have a frequency of 10 20 Hz and thus will be in the gamma ray band. ,t 105 { 80001< 10, I( 2 10 K .. , ____ ........ 11ure emirs a chanctcrisric pec1rum of ndiation called the Planck spectrum.

5 eV etc. 6. 6 eV. 5 eV! We say that the energy of the electron is 'quantized'; it can take only specific values. Equivalently, we may say that the electron can exist in only certain definite energy levels. This is one of the key predictions of quantum theory, which is, of course, confirmed in laboratory experiments. It is possible for an electron to jump from a higher energy level to a lower energy level on its own, changing its energy. 2 eV, which is the difference in these energies. 5 x 10 15 Hz and a wavelength of about 1216 A.

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After the First Three Minutes: The Story of Our Universe by T. Padmanabhan


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