Degeneration of de Broglie waves

Journal of Fusion Energy

The potential energy of a nuclide is enhanced by about 10 MeV per nucleon from the repulsion between like nucleons, and diminished by about 20 MeV per nucleon from the attraction between unlike nucleons. Nuclear stability results mostly from the interplay of these opposing forces, plus Coulomb repulsion of positive charges. Whereas fusion may be the primary mechanism by which first generation stars produce energy, repulsion between like nucleons may cause neutron emission from the collapsed core (neutron star) produced in a terminal supernova explosion and initiate luminosity in second generation stars that accrete on such objects. As noted earlier [1], the scarcity of solar neutrinos, the enrichment of light isotopes in the solar wind, and the presence of abundant short-lived nuclides and interlinked chemical and isotopic heterogeneities in the early solar system might also be explained if the Sun formed in this manner.

Monthly Notices of the Royal Astronomical Society, 1998

In this article we extend the study performed in our previous article of the collapse of primordial objects. We here analyse the behaviour of the physical parameters for clouds ranging from 10 7 to 10 15 M ᭪. We study the dynamical evolution of these clouds in two ways: as purely baryonic clouds and as clouds with non-baryonic dark matter included. We start the calculations at the beginning of the recombination era, following the evolution of the structure until the collapse (which we defined as the time when the density contrast of the baryonic matter is greater than 10 4). We analyse the behaviour of several physical parameters of the clouds (e.g. the density contrast and the velocities of the baryonic matter and the dark matter) as a function of time and radial position in the cloud. In this study all physical processes that are relevant to the dynamical evolution of the primordial clouds, such as for example photon drag (due to the cosmic background radiation) and hydrogen molecular production, besides the expansion of the Universe, are included in the calculations. In particular we find that the clouds with dark matter collapse at higher redshift when we compare the results with the purely baryonic models. As a general result we find that the distribution of the non-baryonic dark matter is more concentrated than the baryonic one. It is important to stress that we do not take into account the putative virialization of the non-baryonic dark matter; we just follow the time and spatial evolution of the cloud, solving its hydrodynamical equations. We also studied the role of cooling-heating processes in the purely baryonic clouds.

Astrophysics at Ultra-High Energies - Proceedings of the 15th Course of the International School of Cosmic Ray Astrophysics, 2007

Dark matter has been recognized as an essential part of matter for over 70 years now, and many suggestions have been made, what it could be. Most of these ideas have centered on Cold Dark Matter, particles that are expected in extensions of standard particle physics, such as supersymmetry. Here we explore the concept that dark matter is sterile neutrinos, a concept that is commonly referred to as Warm Dark Matter. Such particles have keV masses, and decay over a very long time, much longer than the Hubble time. In their decay they produce X-ray photons which modify the ionization balance in the early universe, increasing the fraction of molecular Hydrogen, and thus help early star formation. Sterile neutrinos may also help to understand the baryonasymmetry, the pulsar kicks, the early growth of black holes, the minimum mass of dwarf spheroidal galaxies, as well as the shape of dark matter halos. As soon as all these tests have been quantitative in its various parameters, we may focus on the creation mechanism of these particles, and could predict the strength of the sharp X-ray emission line, expected from any large dark matter assembly. A measurement of this X-ray emission line would be definitive proof for the existence of may be called weakly interacting neutrinos, or WINs.

positrons, one the main building blocaks of the universe, 2023

A review is made of some experiments on the scattering of electrons and positrons. It is commonly believed that an instant annihilation of both particles takes place, with production of a very large amount of energy. Observation concluded instead that the results of such interactions are much more complex, with the production of both matter and energy. A new electron/positron pair can even be created. It may then be envisaged that "empty" space contains many such pairs. Cycles with creation /annihilation of such pairs may be the main quantum mechanism active in space, and be at the origin of the transmission of gravity. Space may be a medium containing a huge number of positrons, which may be a major component of the undetected dark matter. Such medium would also emit much radiation. But it would absorb also most of this radiation, which would therefore be difficult to detect at distance. It may be a significant amount of the so called dark energy. Complex "normal" matter could be mad from the condensation of components originating in space. This would explain why matter and energy are equivalent.

Arxiv preprint astro-ph/ …, 2006

Centre d'Etude Spatiale des Rayonnements Low-mass protostars form from condensations inside molecular clouds when gravity overwhelms thermal and magnetic supporting forces. The first phases of the formation of a solar-type star are characterized by dramatic changes not only in the physical structure but also in the chemical composition. Since PPIV (e.g., Langer et al.), exciting new developments have occurred in our understanding of the processes driving this chemical evolution. These developments include two new discoveries : 1) extremely enhanced molecular deuteration, which is caused by the freeze-out of heavy-element-bearing molecules onto grain mantles during the Prestellar Core and Class 0 source phases; and 2) hot corinos, which are warm and dense regions at the center of Class 0 source envelopes and which are characterized by a multitude of complex organic molecules. In this chapter we will review these two new topics, and will show how they contribute to our understanding of the first phases of solar-type stars.

2005

The finding of an unexpectedly large source of energy from repulsive interactions between neutrons in the 2,850 known nuclides has challenged the assumption that H-fusion is the main source of energy that powers the Sun and other stars. Neutron repulsion in compact objects produced by the collapse of stars and collisions between galaxies may power more energetic cosmological events (quasars, gamma ray bursts, and active galactic centers) that had been attributed to black holes before neutron repulsion was recognized. On a cosmological scale, nuclear matter cycles between fusion, gravitational collapse, and dissociation (including neutronemission) rather than evolve in one direction by fusion. The similarity Bohr noted between atomic and planetary structures may extend to a similarity between nuclear and stellar structures.

Physical Review D, 2020

The present article investigates the impact of muons on core-collapse supernovae, with particular focus on the early muon neutrino emission. While the presence of muons is well understood in the context of neutron stars, until the recent study by Bollig et al. [Phys. Rev. Lett. 119, 242702 (2017)] the role of muons in core-collapse supernovae had been neglected-electrons and neutrinos were the only leptons considered. In their study, Bollig et al. disentangled the muon and tau neutrinos and antineutrinos and included a variety of muonic weak reactions, all of which the present paper follows closely. Only then does it becomes possible to quantify the appearance of muons shortly before stellar core bounce and how the post-bounce prompt neutrino emission is modified.

Nuclear Physics A, 1991

This report was preparedas an accountof worksponsoredby an agencyof the UnitedStates _'_ f__,'_,',,7 ,_ Government, Neither the United States Governmentnor any agencythereof, nor any of their employees, makes any warranty,expressor implied,or assumesany legal liabilityor responsibility for the accuracy,completeness, or usefulnessof any information,apparatus,product, or processdisclosed,or representsthat its use wouldnot infringe privatelyowned rights. Reference herein to any specificcommercialproduct, process,or serviceby trade name, trademark, manufacturer,or otherwisedoes not necessarilyconstitute or imply its endorsement,recommendation,or favoringby the United States Governmentor any agencythereof. The views / and opinions of authors expressed herein do not n_s_iity _tatc,or reflee',those of th_ .... .I UnitedStatesGovernmentor any agencythereof. (. r,.-li stant temperature and density. This is the pre-processing phase. As the shock wave passes ,

Nature Astronomy, 2017

Author Contributions J.d.S. has conducted the historical research, conducted the interviews, and prepared the manuscript. G.B. and J.v.D. defined the project, supervised the research, gave technical and conceptual advice, and contributed to the writing of the manuscript.

Arxiv preprint astro-ph/0205170, 2002

There is increasing observational evidence for the existence of strange stars: ultra-compact objects whose interior consists entirely of deconfined quark matter. If confirmed, their existence places constraints on the rate of formation of microscopic black holes in models which invoke a TeV-scale Planck mass. In such models, black holes can form with ∼ TeV masses through nuclear interactions of particles with PeV and greater energies. Once formed, these black hole states are unstable to Hawking radiation, and rapidly decay. However, if such a black hole forms in the interior of a strange star, the density is high enough that the decay may be counterbalanced by accretion, and the black hole can grow, leading to subsequent catastropic collapse of the star. A guaranteed source of ultra-high energy particles is provided by the cosmogenic Greisen neutrinos, as well as by ultra-high energy cosmic rays, and the implied lifetimes for strange stars are extremely short, contrary to observations. The observed lifetimes of strange star candidates thus effectively exclude Planck mass scales of less than ∼ 2 TeV with comparable black hole masses, for up to 2 extra dimensions. Seeding of strange star collapse in scenarios with a larger number of extra-dimensions or with higher mass black holes remains a possibility, and may provide another channel for the origin of gamma-ray bursts.

Physical Review Letters, 2008

A mechanism is identified whereby dark matter (DM) in protostellar halos dramatically alters the current theoretical framework for the formation of the first stars. Heat from neutralino DM annihilation is shown to overwhelm any cooling mechanism, consequently impeding the star formation process and possibly leading to a new stellar phase. A "dark star" may result: a giant ( ∼ > 1 AU) hydrogen-helium star powered by DM annihilation instead of nuclear fusion. Observational consequences are discussed.

Nuclear Physics B - Proceedings Supplements, 2002

It is described the astrophysical model of a short-lived and very powerful hidden source of high-energy neutrinos. This source is formed as a result of dynamical evolution of a galactic nucleus prior to its collapse into the massive black hole. A dense central stellar cluster in the galactic nucleus onthe late stage of evolution consists of neutron stars and stellar mass black holes deep inside the massive gas envelope produced by destructive collisions of a primary stellar population. Frequent collisions of neutron stars result in a creation of an expanding rarefied cavity in the envelope. Particles are effectively accelerated in the cavity and, due to pp-collisions in the gas envelope, they produce high-energy neutrinos. High-energy neutrino signal can be detected by underground neutrino telescope with effective area S ~ 1 km 2.

2018

Even though the combined laboratory, astrophysical and cosmological evidence implies that neutrinos have masses, neutrinos provide only a small cosmic dark matter component. The study of solar neutrinos provides important information on nuclear processes inside the Sun as well as on matter densities. Moreover, supernova neutrinos provide sensitive probes for studying supernova explosions, neutrino properties and stellar collapse mechanisms. Neutrino-nucleus reactions at energies below 100MeV play essential roles in core-collapse supernovae, explosive and r-process nucleosynthesis, as well as observation of solar and supernova neutrinos by earthbound detectors. On the other hand, recent experimental data of high-energy extragalactic neutrinos at 1 PeV open a new window to probe non-standard neutrino properties, such as resonant effects in the oscillation probability.

Physical Review D, 1975

Comments and Addenda The Comments and Addenda sectiotl is for short comm~rnicatrons which are not o f such urgencj as to justrjy pttblrcatiorz in Physical Review Letters and are nor approprlute for regular Articles It rncludes only the followrng types of communrcations-(1) comments on papers previously publrshed r r~ The Physical Review or Physical Review Letters; 117laddenda to papers previously published in The Physical Review or Physical Review Letters, in whrch the additronal itlformation can be presented without the need for writing a complete article Manuscripts intended fur t h i~ secriun should be accompanied by a brief ab~tract fur infornwtiun-rerrieval purposes Accepted manuscripts will follow the same publicatiorr schedule as arricles in this journal, and galleys wrll be sent to authors Neutrino production in stellar matter by photons in a renormalizable scalar-boson-exchange model of weak interactions S. N. isw was:

Dark Matter in Astro- and Particle Physics, 2001

I discuss in this talk mainly three topics related with dark matter motivated neutrino mass spectrum and a generic issue of mass pattern, the normal versus the inverted mass hierarchies. In the first part, by describing failure of a nontrivial potential counter example, I argue that the standard 3 ν mixing scheme with the solar and the atmospheric ∆m 2 's is robust. In the second part, I discuss the almost degenerate neutrino (ADN) scenario as the unique possibility of accommodating dark matter mass neutrinos into the 3 ν scheme. I review a cosmological bound and then reanalyze the constraints imposed on the ADN scenario with the new data of double beta decay experiment. In the last part, I discuss the 3 ν flavor transformation in supernova (SN) and point out the possibility that neutrinos from SN may distinguish the normal versus inverted hierarchies of neutrino masses. By analyzing the neutrino data from SN1987A, I argue that the inverted mass hierarchy is disfavored by the data.