Summary
The thermodynamical picture of a hot lump of hadronic matter («clusters», high-density gluonic clouds and especially suitable cases of hydrodynamical theories of Heisenberg and Landau) naturally leads to direct production of gamma quanta («black-body radiation») and—in the next order ine 2—of lepton pairs. At largep T their spectra reproduce the main features of the pionic spectrum. The intensity of γ’s exceedse 2 times that of the π’s, due to the relatively large volume of the radiating system and to the long duration of its expansions. However, since the dynamics of the heated hadronic vacuum is not known, pre-exponential factors cannot be safely calculated. All this is expected to hold for the overall c.m.s. energy\(\sqrt 8 \sim \left( {10 \div 10^2 } \right)\) GeV. For even higher energies with a correspondingly increasing mass of the lump (if such lumps exist), probably at\(\sqrt 8 > 10^3 \) GeV, γ quanta (and for even larger lumps,\(\sqrt 8 \sim 10^4 \) GeV, leptons as well) may become equal partners to hadrons in thermodynamical equilibrium. Almost all the results were published by the present author about 15 years ago in Russian (and only briefly mentioned in some of his review papers in English). In this paper they are somewhat extended and discussed in more detail in the light of new experiments on large-p T leptons and of the quark-gluon ideas.
Riassunto
Il quadro termodinamico di un blocco caldo di materia adronica («ammassi», nubi gluoniche di alta densità e specialmente casi adatti di teorie idrodinamiche di Heisenberg e Landau) conduce in modo naturale alla produzione diretta dei quanti gamma («radiazione del corpo nero») e—nell’ordine successivo ine 2—di coppie di leptoni. Per grandep T i loro spettri riproducono le caratteristiche principali dello spettro pionico. L’intensità dei γ superae 2 volte quella dei π, a causa del volume relativamente grande del sistema radiante e della lunga durata del suo sviluppo. Comunque, poiché non si conosce la dinamica del vuoto adronico riscaldato, i fattori preesponenziali non possono essere calcolati in modo sicuro. Ci si aspetta che tutto questo valga per l’energia totale s.c.m.\(\sqrt 8 \sim \left( {10 \div 10^2 } \right)\) GeV. Per energie ancora maggiori con massa del blocco crescente corrispondentemente (se questi blocchi esistono), probabilmente a\(\sqrt 8 > 10^3 \){ GeV, i quanti γ (e per blocchi ancora maggiori,\(\sqrt 8 \sim 10^4 \) GeV, anche i leptoni) possono partecipare come gli adroni all’equilibrio termodinamico. Quasi tutti i risultati furono pubblicati da questo autore una quindicina di anni fa in russo (e menzionati solo brevemente in alcuni dei suoi lavori di rassegna in inglese). In questo lavoro questi risultati sono in qualche modo estesi e discussi più dettagliatamente alla luce di nuovi esperimenti sui leptoni con grandep T e delle idee sul quark-gluone.
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Feinberg, E.L. Direct production of photons and dileptons in thermodynamical models of multiple hadron production. Nuov Cim A 34, 391–412 (1976). https://doi.org/10.1007/BF02783618
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DOI: https://doi.org/10.1007/BF02783618