About Science, Myself and Others by V.L. Ginzburg

By V.L. Ginzburg

In approximately technological know-how, Myself and Others, Vitaly Lazarevich Ginzburg, co-recipient of the 2003 Nobel Prize in Physics and Editor of the evaluate magazine Physics-Uspekhi, presents an perception into smooth physics, the lives and works of different well-known physicists he has identified, and perception into his personal lifestyles and perspectives on physics and past.

Divided into 3 components, the e-book starts off with a evaluation of the most important difficulties in modern physics, astrophysics, and cosmology, interpreting their old improvement and why they pose this kind of problem to present day physicists and for society. half One additionally contains info of a few of Professor Ginzburg's paintings, together with superconductivity and superfluidity. half encompasses numerous articles at the lives and works of numerous fashionable physicists, together with the writer. The 3rd half is a set of articles that offer a private view of the writer, describing his own perspectives and reminiscences on a variety of wider themes.

Taken jointly, this choice of articles creates an stress-free evaluation of physics, its philosophy, and key avid gamers in its smooth improvement within the twentieth Century. definitely, it is going to be an stress-free learn for pro physicists and non-scientists alike.

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It is only the problem of the origin of CRs with ultra- or super-high energies that may be ‘particularly important and interesting’, according to the terminology adopted here. For example, the origin of the ‘break’ (‘knee’) in the energy spectrum of CR at ECR ∼ 1015 –1016 eV is not quite clear and especially the situation in the energy range ECR > 1019 eV—such CRs are sometimes called ultrahighCopyright © 2005 IOP Publishing Ltd. Some comments (astrophysics) 35 energy CR (UHECR, see [98, 187, 188]) is enigmatic.

However, after work by Friedmann (1922) and the discovery of the Universe expansion (provisionally in 1929), it became clear that the static model was far from reality and the Λ-term was no longer needed. Moreover, Einstein considered the introduction of the Λ-term to be ‘unsatisfactory from the theoretical point of view’ [79] and discarded it. Pauli, in the appendix to his well-known book published in English in 1958, totally shared Einstein’s opinion (see [65, p 287]). L D Landau hated the idea of the Λ-term but I could not make him give his reasoning.

10) For ΩΛ ∼ 1 and H ∼ H0 ∼ 2 × 10−18 s−1 we have Λ0 ∼ 10−56 cm−2 . The estimates, for our epoch, according to observations, are as follows: Ωb ∼ Copyright © 2005 IOP Publishing Ltd. 015, i. e. there are few baryons. 1 (see comment 9). 8) is questionable. Another equation of state with generally close results is possible: εv = 1 pv w w < 0. 8a) Clearly, the Λ-term corresponds to w = −1. Such ‘dark energy’ is also called ‘quintessence’ [151, 152, 204]. In paper [152], the quintessence is related to the existence of some scalar field Φ.

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