Quark Matter 1987: Concluding remarks

This year marked the beginning of the experimental program at BNL and CERN to probe the properties of ultra dense hadronic matter and to search for the quark-gluon plasma phase of matter. Possible implications of the preliminary findings are discussed. Problems needing further theoretical and experimental study are pointed out.     

About neutrino signals from SN 1987A

Summary The properties of neutrino signals from SN 1987A are unexpected, namely, two pulses occurred with a 4 h 43 min interval and the total energy carried away by neutrinos is too high (E ₅₄≥3) for either of the pulses,i.e. an order as high as the maximum value ensuing from the neutron star mass defect. If the function of neutrino energy distribution is assumed to be equilibrium and of Fermi form, the data obtained from different equipments are in a poor agreement with each other. The general relativity and the geometry as a whole were used earlier to demonstrate that, in case of a sufficiently high mass when any equilibrium static solution is absent, there exists a dynamic oscillatory solution, namely, matter moves periodically to under the gravitational radius and emerges from under the latter to enter the same physical space. The mass defect for the dynamic configuration is 60%, thereby eliminating all the troubles involved by energy considerations. A feasible scenario of the SN 1987A explosion is discussed considering the function of neutrino energy distribution to differ from an equilibrium function.

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Riassunto Le proprietà dei segnali neutrinici dalla SN 1987A sono impreviste, cioè due impulsi si sono verificati con un intervallo di 4 h 43 min e l'energia totale portata via dai neutrini è troppo elevata (E ₅₄≥3) per ciascuno degli impulsi, cioè è dello stesso ordine del valore massimo che deriva dal difetto di massa della stella di neutroni. Se la funzione della distribuzione dell'energia dei neutrini è ipotizzata in equilibrio e della forma di Fermi, i dati ottenuti con diverse apparecchiature sono in scarso accordo tra loro. La relatività generale e la geometria nel complesso sono state usate precedentemente per dimostrare che, nel caso di una massa sufficientemente grande, quando manca una soluzione di equilibrio statico, esiste una soluzione oscillatoria dinamica, cioè la materia si muove periodicamente fino a sotto il raggio gravitazionale e emerge da sotto quest'ultimo per entrare nello stesso spazio fisico. Il diffetto di massa per la configurazione dinamica è il 60%, eliminando perciò tutti i problemi che le considerazioni sull'energia implicano. Si discute uno scenario fattibile dell'esplosione della SN 1987A assumendo che la funzione di distribuzione dell'energia neutrinica differisca dalla funzione di equilibrio.

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Резюме Свойства нейтринных сигналов от SN 1987A неожиданны: были два имульса с интервалом 4 h 43 min: полная энергия, унесенная нейтрино, слишком велика (E ₅₄>3 для каждого из импульсов, что на порядок превышает максимальное значение, вытекающее из дефекта массы нейтронной звезды. Если предположить, что функция распределения нейтрино по энергии равновесная фермиевская, то данные установок плохо согласуются между собой. Ранее, строго в рамках общей теории относительности и геометрии в целом, было показано, что при достаточно большой массе, когда не существует равновесного статического решения, есть динамическое колебательное решение-материя периодически заходит под гравиатционный радиус и выходит из под него в тоже самое физическое пространство. Дефект массы для динамической конфигурации равен 60%, что снимает все трудности с энергетикой. Обсуждается возможный сценарий взрыва SN 1987A, при этои функция распределения нейтрино по энергии отличается от равновесной.

     

Neutrino astrophysics and SN 1987 A(*)(**)

Summary In this paper we summarize the Mont Blanc observation of the Large Magellanic Cloud supernova, exploded on February 23, 1987. The problem of two bursts, recorded in different underground detectors and separated in time by 4.7 hours, is also discussed. Since the different observations are not contradictory from the experimental point of view, some changements are required in the current predictions of the theoretical models of a gravitational stellar collapse in order to fit all the experimental data. Finally, the combined analysis of the data, recorded in all the neutrino and gravitational wave detectors running at the time of the supernova, clearly indicates a long duration of the phenomenon. Thus, any serious (even if difficult) tentative to explain how a star ends its life as a supernova should be based on all the experimental data available, recorded in different, independent experiments running at intercontinental distances at the time of supernova 1987 A. To speed up publication, the proofs were not sent to the authors and were supervised by the Scientific Committee.     

Supernova 1987A, 30 Years Later

Most supernova theories state that this phenomenon lasts for a few seconds and ends with a big final explosion. However, these theories do not take into account several experimental results obtained with neutrino and gravitational wave detectors during the explosion of SN 1987A, the only supernova observed in a nearby galaxy in modern age. According to these experimental results the phenomenon is much more complex that envisaged by current theories, and has a duration of several hours. Since recent data of the X-ray NASA Satellite NuSTAR show a clear evidence of an asymmetric collapse, we have revisited the experimental data recorded by some underground and gravitational wave detectors running at the time of SN 1987A. New evidence is shown that confirms the previous results, namely that the data recorded by the gravitational wave detectors running in Rome and in Maryland are strongly correlated with the data of both the LSD (Mont Blanc) and the Kamiokande detectors, and that the correlation extends over a long period of time (one or two hours) centered at the Mont Blanc time. In addition, the signals of the GW detectors preceded the signals of the underground detectors by a time of order of one second. This result, obtained by comparing six independent files of data recorded by four different experiments located at intercontinental distances, indicates that also Kamiokande detected neutrinos at theMont Blanc time, but these interactions were not identified because not grouped in a burst. A similar correlation was also found in the data of the underground experiments in Mont Blanc and Baksan.