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 clinical figuring out of those profound and basic matters. In full of life prose, Professor Padmanabhan paints an image of latest cosmology for the final reader. not like different renowned books on cosmology, After the 1st 3 mins doesn't gloss over information, or shrink back from explaining the underlying thoughts. as an alternative, with a lucid and casual kind, the writer introduces all of the suitable historical past after which rigorously items jointly an interesting tale of the evolution of our Universe. Padmanabhan leaves the reader with a cutting-edge photograph of scientists' present figuring out in cosmology and a willing flavor of the buzz of this fast-moving technology. all through, no arithmetic is used and all technical jargon is obviously brought and bolstered in a convenient thesaurus on the finish of the e-book. For normal readers who are looking to come to grips with what we actually do and do not learn about our Universe, this e-book 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 a number of other common columns on astronomy, leisure arithmetic, and the background of technological know-how.
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Additional info for After the First Three Minutes: The Story of Our Universe
All of them are vibrations in the electromagnetic field; the higher the frequency, the more rapid these vibrations are. There are, however, several other properties of the electromagnetic radiation which vary drastically as the wavelength is changed. In particular, the way radiation interacts with matter depends very much on the wavelength. Consequently, the emission and absorption of radiation by matter depends on the wavelength. You know from experience that visible light cannot pass through human flesh while X-rays can.
During such a motion, the particle is constantly accelerated and will radiate energy. Astrophysical systems invariably contain magnetic fields which could influence the motion of the charged particles. As a result, synchrotron radiation is of primary importance in astrophysics and usually occurs in a wave band stretching from centimeters to meters. This is the wavelength below standard AM (around 300 meters wavelength) and FM (around 3 meters wavelength) used in radio transmissions. Radio astronomers have very effectively used synchrotron radiation as a probe of astrophysical systems.
The radiation with wavelengths outside the visible band is called by different names, like gamma rays, X-rays, ultraviolet, infrared and radio waves; we shall discuss these bands in detail in the next chapter. In discussing properties like wavelength or frequency of radiation, there is a tacit assumption that the source of radiation and the observer are at rest with respect to each other. In general, this need not be true; for example, we may receive radiation from a star or a galaxy which is moving with respect to us.