Il Nuovo Cimento B (1971-1996)

, Volume 34, Issue 2, pp 245–255 | Cite as

The role of strong interactions in cosmology

  • M. Dersarkissian


A cosmological model is constructed which is a Friedmann model, but with a finite ultimate temperature (TF). The model predicts the temperature of the cosmic-microwave background in terms of 4 parameters: the present energy density of matter in the Universe and the parameters which may have characterized hot, dense, hadronic matter during the early Universe (A, TF, B). The latter are defined by the level density for hadronic matter:\(\sigma (m)\underrightarrow {m \to \infty } Am^{ - B} exp [m/T_F ]\). The calculation of the microwave temperature gives similar results for Hagedorn (B=5/2) and Frautschi (B=3) models. Both models clearly favour a low cosmic density ((10−31÷10−33) g/cm3) over a high density (10−29 g/cm3). This result suggests that hot, dense, hadronic matter in thermal contact with radiation in the early Universe conspired to produce the open Universe of today.

Роль сильных вааимодействий в космологии


Конструируется космологическая модель, которая представляет модель Фридмана, но с конечной температурой (TF). Предложенная модель предсказывает температуру космического микроволнового фона в терминах четырех параметров: современная плотность энергии во Вселенной и параметры, которые характеризуют горячее, плотное, адронное вещество на ранних стадиях развития Вселенной (A, TF, B). Последние параметры определяют уровень плотности адронного вещества:\(\sigma (m)\underrightarrow {m \to \infty } Am^{ - B} exp [m/T_F ]\). Вычисление микроволновой температуры дает одинаковый результат для моделей Хагедорна (B=5/2) и Фраутчи (B=3). Обе эти модели отдают предпочтение низкой космической плотности ((10−31÷10−33) г/см3) по сравнению с высокой плотностяю (10−29 г/см3). Этот результат подтверждает, что горячее, плотное, адронное вещество в тепловом контакте с излучением на ранней стадии развития Вселенной способствовало бы образованию открытой Вселенной в настоящее время.


Si costruisce un modello cosmologico che è un modello di Friedmann, ma con una temperatura finale finita (TF). Il modello predice la temperatura del fondo della microonda cosmica in termini di 4 parametri: l'attuale densità di energia della materia nell'Universo e i parametri che possono aver caratterizzato la materia calda, densa e adronica durante il primo Universo (A, TF, B). Questi ultimi sono definiti dalla densità dei livelli per la materia adronica:\(\sigma (m)\underrightarrow {m \to \infty } Am^{ - B} exp [m/T_F ]\). Il calcolo della temperatura della microonda dà risultati analoghi per i modelli di Hagedorn (B=5/2) e di Frautschi (B=3). Entrambi i modelli favoriscono chiaramente una bassa densità cosmica ((10−31÷10−33) g/cm3) rispetto ad un'alta densità (10−29 g/cm3). Questo risultato suggerisce che la materia calda, densa, adronica in contatto termico con la radiazione nel primo Universo cooperò nel produrre l'odierno Universo aperto.


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Copyright information

© Società Italiana di Fisica 1976

Authors and Affiliations

  • M. Dersarkissian
    • 1
  1. 1.Department of PhysicsTemple UniversityPhiladelphia

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