By R.D. Blandford, H. Netzer, L. Woltjer, T.J.-L. Courvoisier, M. Mayor
Beginning with this quantity, the Lecture Notes of the popular complex classes of the Swiss Society for Astrophysics and Astronomy can be released each year. In each one direction, 3 huge lectures given through prime specialists of their respective fields conceal diverse and crucial facets of the topic. the 20 th path, held at Les Diablerets in April 1990, handled present study on energetic galactic nuclei; it represents the main up to date perspectives at the topic, awarded with specific regard for readability. the former classes thought of a large choice of matters, starting with "Theory of Stellar Athmospheres" in 1971 and finishing with "The Milky method as a Galaxy" in 1989. The Lecture Notes of those Saas-Fee classes seemed as guides of the Geneva Observatory, from which they could nonetheless be ordered (chemin des Maillettes fifty one, CH-1290 Sauverny, Switzerland).
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Il risultato finale fu un articolo unito tra Penrose ed io, in 1970, che alla fine provò che ha dovuto avere una singolarità come quella del big bang, con l'unica condizione che la relatività generale sia corretta e che l'universo contenga tanta materia come osserviamo. Ci fu una forte opposizione al nostro lavoro, da parte dei russi, dovuto alla sua credenza marxista nel determinismo scientifico, e da parte della gente che credeva che l'idea in sé delle singolarità era ripugnante e rovinava la bellezza della teoria di Einstein.
Magari allora l'universo in espansione attuale non sarebbe derivato da una singolarità come il big bang, bensì di, una fase previa in contrazione. Quando l'universo collassò, le particelle che lo formassero non avrebbero potuto urtare tutte tra sé, ma si sarebbero incrociati e separato dopo, producendo l'espansione attuale dell'universo. Come potremmo distinguere allora se l'universo reale ha cominciato con un big bang o no? Quello che Lifshitz e Khalatnikov fecero fu studiare modelli dell'universo che erano approssimativamente come quelli di Friedmann, ma che avevano in conto le irregolarità e le velocità aleatorie delle galassie nell'universo reale.
Benché Friedmann trovasse solo uno, esistono in realtà tre tipi di modelli che ubbidiscono alle due supposizioni fondamentali di Friedmann. Nel primo tipo (quello che trovò Friedmann, l'universo si espande il sufficientemente lento come affinché l'attrazione gravitazionale tra le differenti galassie sia capace di frenare e finalmente fermare l'espansione. Allora le galassie si incominciano ad avvicinare le alcune alle altre e l'universo si contrarsi. 2 dimostrazione come cambia, come aumenta in due il tempo, la distanza galassie vicine.
