By T. Padmanabhan
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 figuring out of those profound and primary matters. In energetic prose, Professor Padmanabhan paints an image of up to date 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 recommendations. as a substitute, with a lucid and casual kind, the writer introduces all of the correct history after which rigorously items jointly an enticing tale of the evolution of our Universe. Padmanabhan leaves the reader with a cutting-edge photograph of scientists' present knowing in cosmology and a willing flavor of the thrill 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 word list on the finish of the booklet. For basic readers who are looking to come to grips with what we actually do and do not learn about our Universe, this ebook 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 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 general columns on astronomy, leisure arithmetic, and the background of technological know-how.
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Extra info for After the First Three Minutes: The Story of Our Universe
We shall see, in later chapters, that the 21 em radiation turns out to be a boon to astronomers. There is another important piece of information which the spectrum can provide. We mentioned earlier that the wavelength of radiation (as detected by us) could change if the source is moving towards or away from us. Suppose we have a source of gaseous hydrogen emitting radiation at two different wavelengths, say, A. 1 and A. 2 . For example, the transition of electrons from the first excited level to the ground state will lead to the emission of photons with wavelength A.
The first one is called the 'wavelength', which is the distance between two crests of the wave at any given time. The second quantity is the 'frequency' of the wave, which tells us how many times the wave vibrates in one second at any given location. The third is the 'amplitude' of the wave, which is an indication of how big a disturbance the wave is creating on the surface of the water. Finally, one can also associate a 'speed of propagation' with the wave. This decides how fast the disturbance moves from one point to another along the surface of the water.
5 Interaction of matter and light The same physical process is responsible for the emission of radiation in almost all cases. Different atoms will have different sets of energy levels, and the transitions of electrons between these levels will lead to the emission of radiation at different frequencies. In fact, the process is not restricted to atoms. Molecules, for example, have their own energy levels (in addition to the energy levels of the atoms which make up the molecule) and hence can emit radiation by making a transition between two such levels.