Utente:Vale maio/Sandbox3: differenze tra le versioni

Versione delle 17:16, 27 giu 2010

Versione delle 17:34, 27 giu 2010

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{{cite book|last=Gamow|first=G.|authorlink=George Gamow|year=2004|origyear=1961|title=Cosmology and Controversy: The Historical Development of Two Theories of the Universe|page=40|publisher=[[Courier Dover Publications]]|url=http://books.google.com/?id=5awirwgmvAoC&pg=PA40|isbn=0486438686}}</ref>, commentando che ".. è in accordo ragionevole con la temperatura reale dello spazio interstellare", ma non fa menzione della radiazione di fondo.

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|align="right">|''1948''||[[Ralph Alpher]] ande [[Robert Herman]] estimatestimano "thela temperaturetemperatura in the Universedell'Universo" ata 5 K. AlthoughAnche theyse donon notmenziona specificallyesplicitamente mentionla microwaveradiazione backgrounddi radiationfondo a microonde, itsi maypuò be inferred.dedurre<ref>Kragh, H. (1999:132). "Alpher and Herman first calculated the present temperature of the decoupled primordial radiation in 1948, when they reported a value of 5 K. Although it was not mentioned either then or in later publications that the radiation is in the microwave region, this follows immediately from the temperature... Alpher and Herman made it clear that what they had called "the temperature in the universe" the previous year referred to a blackbody distributed background radiation quite different from sunliight".</ref>.

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|align="right">|''1950''||Ralph Alpher and Robert Herman re-estimatericalcolano thela temperaturetemperatura ata 28 K.

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|align="right">|''1953''||[[George Gamow]] estimatesstima la temperatura a 7 K.<ref name=Kragh />

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|align="right">|''1955''||Émile Le Roux ofdella the''Radio Nançay Radio Observatory'', in auno skystudio surveydel atcielo a λ = 33 cm, reportedriporta aun near-isotropicradiazione backgrounddi radiationfondo ofquasi isotropa di 3 kelvinskelvin, plus or minus± 2.<ref name=Kragh />.

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|align="right">|''1956''||[[George Gamow]] estimatesstima la temperatura a 6 K.<ref name=Kragh />

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|align="right">|''1957''

|Tigran Shmaonov riporta che "la temperatura assoluta effettiva del fondo di emissione radio ... è di 4 ± 3 K"<ref>{{cite journal|last=Shmaonov|first=T. A.|year=1957|title=Commentary|language=Russian|journal=[[Pribory i Tekhnika Experimenta]]|volume=1|issue=|pages=83|doi=10.1016/S0890-5096(06)60772-3}}</ref>. Va osservato che la "misurazione ha mostrato che l'intensità delle radiazioni è indipendente dal tempo e dalla direzione di osservazione ... è ormai chiaro che Shmaonov aveva osservato la radiazione cosmica di fondo alla lunghezza d'onda di 3,2 cm"<ref>{{cite book|last=Naselsky|first=P. D.|last2=Novikov|first2=D.I.|last3=Novikov|first3=I. D.|year=2006|title=The Physics of the Cosmic Microwave Background|url=http://books.google.com/?id=J2KCisZsWZ0C&pg=RA1-PA1&dq=Shmaonov+cmb|pages=5|publisher=[[Cambridge University Press]]|isbn=0521855500}}</ref>

|Tigran Shmaonov reports that "the absolute effective temperature of the radioemission background ... is 4±3K".<ref>

{{cite journal|last=Shmaonov|first=T. A.|year=1957|title=Commentary|language=Russian|journal=[[Pribory i Tekhnika Experimenta]]|volume=1|issue=|pages=83|doi=10.1016/S0890-5096(06)60772-3}}</ref> It is noted that the "measurements showed that radiation intensity was independent of either time or direction of observation... it is now clear that Shmaonov did observe the cosmic microwave background at a wavelength of 3.2 cm"<ref>

{{cite book|last=Naselsky|first=P. D.|last2=Novikov|first2=D.I.|last3=Novikov|first3=I. D.|year=2006|title=The Physics of the Cosmic Microwave Background|url=http://books.google.com/?id=J2KCisZsWZ0C&pg=RA1-PA1&dq=Shmaonov+cmb|pages=5|publisher=[[Cambridge University Press]]|isbn=0521855500}}</ref>

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|align="right">|''1960sanni 1960''||Robert Dicke re-estimatesstima anuovamente MBRla (microwavetemperatura backgrounddella radiation)CMB temperature ofa 40 K<ref name=Kragh />

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|align="right">|''1964''||[[A. G. Doroshkevich]] ande [[Igor Dmitriyevich Novikov|Igor Novikov]] publishpubblicano auna briefbreve papernota, wheredove theymenzionano namela CMB come fenomeno osservabile<ref>{{cite journal|last=Doroshkevich|first=A. G.|last2=Novikov|first2=I.D.|year=1964|title=Mean Density of Radiation in the CMBMetagalaxy radiationand phenomenonCertain asProblems detectablein Relativistic Cosmology|journal=[[Soviet Physics Doklady]]|volume=9|pages=|doi=|bibcode=1964SPhD....9..111D}}</ref>.

{{cite journal|last=Doroshkevich|first=A. G.|last2=Novikov|first2=I.D.|year=1964|title=Mean Density of Radiation in the Metagalaxy and Certain Problems in Relativistic Cosmology|journal=[[Soviet Physics Doklady]]|volume=9|pages=|doi=|bibcode=1964SPhD....9..111D}}</ref>

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|align="right">|''1964–65''||[[Arno Penzias]] and [[Robert Woodrow Wilson]] measure the temperature to be approximately 3 K. Robert Dicke, [[P. J. E. Peebles]], P. G. Roll, and [[David Todd Wilkinson|D. T. Wilkinson]] interpret this radiation as a signature of the big bang.