She-Sheng Xue

On the Interpretation of the Burst Structure of Gamma-Ray Bursts

Given the very accurate data from the BATSE experiment and RXTE and Chandra satellites, we use the GRB 991216 as a prototypical case to test the EMBH theory linking the origin of the energy of GRBs to the electromagnetic energy of black holes. The fit of the afterglow fixes the only two free parameters of the model and leads to a new paradigm for the interpretation of the burst structure, the IBS paradigm. It leads as well to a reconsideration of the relative roles of the afterglow and burst in GRBs by defining two new phases in this complex phenomenon: a) the injector phase, giving rise to the proper-GRB (P-GRB), and b) the beam-target phase, giving rise to the extended afterglow peak emission (E-APE) and to the afterglow. Such differentiation leads to a natural possible explanation of the bimodal distribution of GRBs observed by BATSE. The agreement with the observational data in regions extending from the horizon of the EMBH all the way out to the distant observer confirms the uniqueness of the model. Subject headings: black holes, gamma ray bursts, supernovae The most decisive tool in the identification of the energetics of GRBs has been the discovery by Beppo SAX of the afterglow phenomenon. We show in this letter how the afterglow data can be fit using the theory which relates the GRB energy to the extraction process of the electromagnetic energy of a black hole endowed with electromagnetic structure (an EMBH). This energy extraction process occurs via vacuum polarization pair creation and approaches almost perfect reversibility in the sense of black hole physics (Christodoulou & Ruffini 1971; Damour & Ruffini 1975; Preparata et al. 1998). In addition to yielding excellent agreement between the theory and the data, a new paradigm will be introduced here for the interpretation of the burst structure which we call the IBS paradigm. ruffini@icra.it Because of the unique accuracy of its data, we use the GRB 991216 as a prototype for a description which may then be generalized to other GRBs. The relevant data for GRB 991216 are reproduced in Fig. 1, namely the data on the burst as recorded by BATSE (BATSE Rapid Burst Response 1999) and the data on the afterglow from the RXTE satellite (Corbet & Smith 2000) and the Chandra satellite (Piro et al. 2000) (see also Halpern et al. 2000). We have modeled the afterglow assuming that the ultra-high energy baryons (the ABM pulse of Ruffini et al. (2001a), Letter 1), accelerated in the pair-electromagneticbaryonic pulse (PEMB pulse) following a black hole collapse process (see Letter 1), after reaching transparency interact with the interstellar medium (ISM), assumed to have an average density nism of 1 proton/cm. All internal energy developed in the collision is assumed to be radiated away in a

Neutron star equilibrium configurations within a fully relativistic theory with strong, weak, electromagnetic, and gravitational interactions

Abstract We formulate the equations of equilibrium of neutron stars taking into account strong, weak, electromagnetic, and gravitational interactions within the framework of general relativity. The nuclear interactions are described by the exchange of the σ, ω, and ρ virtual mesons. The equilibrium conditions are given by our recently developed theoretical framework based on the Einstein–Maxwell–Thomas–Fermi equations along with the constancy of the general relativistic Fermi energies of particles, the “Klein potentials”, throughout the configuration. The equations are solved numerically in the case of zero temperatures and for selected parameterizations of the nuclear models. The solutions lead to a new structure of the star: a positively charged core at supranuclear densities surrounded by an electronic distribution of thickness ∼ ℏ / ( m e c ) ∼ 10 2 ℏ / ( m π c ) of opposite charge, as well as a neutral crust at lower densities. Inside the core there is a Coulomb potential well of depth ∼ m π c 2 / e . The constancy of the Klein potentials in the transition from the core to the crust, imposes the presence of an overcritical electric field ∼ ( m π / m e ) 2 E c , the critical field being E c = m e 2 c 3 / ( e ℏ ) . The electron chemical potential and the density decrease, in the boundary interface, until values μ e crust μ e core and ρ crust ρ core . For each central density, an entire family of core–crust interface boundaries and, correspondingly, an entire family of crusts with different mass and thickness, exist. The configuration with ρ crust = ρ drip ∼ 4.3 × 10 11 g cm − 3 separates neutron stars with and without inner crust. We present here the novel neutron star mass–radius for the especial case ρ crust = ρ drip and compare and contrast it with the one obtained from the traditional Tolman–Oppenheimer–Volkoff treatment.

On a Possible Gamma-Ray Burst-Supernova Time Sequence

The data from the Chandra satellite on the iron emission lines in the afterglow of GRB 991216 are used to give further support to the theory that links the origin of the energy of gamma-ray bursts (GRBs) to the extractable energy of electromagnetic black holes (EMBHs), leading to an interpretation of the GRB-supernova correlation. Following the relative spacetime transformation paradigm and the interpretation of the burst structure paradigm, we introduce a paradigm for the correlation between GRBs and supernovae. The following sequence of events is shown as kinematically possible and consistent with the available data: (1) the GRB-progenitor star P1 first collapses into an EMBH; (2) the proper GRB and the peak of the afterglow (the extended afterglow peak emission) propagate in interstellar space until the impact on a supernova-progenitor star P2 at a distance ≤2.69 × 1017 cm, and they induce the supernova explosion; and (3) the accelerated baryonic matter pulse, originating the afterglow, reaches the supernova remnants 18.5 hr after the supernova explosion and gives rise to the iron emission lines. Some considerations of the dynamical implementation of the paradigm are presented. The concept of an induced supernova explosion, introduced here specifically for the GRB-supernova correlation, may have a more general application in relativistic astrophysics.

Relative Spacetime Transformations in Gamma-Ray Bursts

GRB 991216 and its relevant data acquired from the BATSE and the Rossi X-Ray Timing Explorer and Chandra satellites are used as a prototypical case to test the theory linking the origin of gamma-ray bursts (GRBs) to the process of vacuum polarization occurring during the formation phase of a black hole endowed with electromagnetic structure. The relative spacetime transformation paradigm is presented. It relates the observed signals of GRBs to their past light cones, defining the events on the worldline of the source that is essential for the interpretation of the data. Since GRBs present regimes with unprecedentedly large Lorentz factors, and also sharply varying with time, particular attention is given to the constitutive equations relating the four time variables: the comoving time, the laboratory time, the arrival time, and the arrival time at the detector corrected by the cosmological effects. This paradigm is at the very foundation of any possible interpretation of the data of GRBs.

Electron-positron pair production in space- or time-dependent electric fields

Treating the production of electron and positron pairs by a strong electric field from the vacuum as a quantum tunneling process we derive, in semiclassical approximation, a general expression for the pairproduction rate in a z-dependent electric field EðzÞ pointing in the z direction. We also allow for a smoothly varying magnetic field parallel to EðzÞ. The result is applied to a confined field EðzÞ � 0 for jzj & ‘, a semiconfined field EðzÞ � 0 for z * 0, and a linearly increasing field Eðz Þ� z. The boundary effects of the confined fields on pair-production rates are exhibited. A simple variable change in all formulas leads to results for electric fields depending on time rather than space. In addition, we discuss tunneling processes in which empty atomic bound states are spontaneously filled by negative-energy electrons from the vacuum under positron emission. In particular, we calculate the rate at which the atomic levels of a bare nucleus of finite-size rn and large Z � 1 are filled by spontaneous pair creation.

The self-consistent general relativistic solution for a system of degenerate neutrons, protons and electrons in β-equilibrium

Abstract We present the self-consistent treatment of the simplest, nontrivial, self-gravitating system of degenerate neutrons, protons and electrons in β -equilibrium within relativistic quantum statistics and the Einstein–Maxwell equations. The impossibility of imposing the condition of local charge neutrality on such systems is proved, consequently overcoming the traditional Tolman–Oppenheimer–Volkoff treatment. We emphasize the crucial role of imposing the constancy of the generalized Fermi energies. A new approach based on the coupled system of the general relativistic Thomas–Fermi–Einstein–Maxwell equations is presented and solved. We obtain an explicit solution fulfilling global and not local charge neutrality by solving a sophisticated eigenvalue problem of the general relativistic Thomas–Fermi equation. The value of the Coulomb potential at the center of the configuration is e V ( 0 ) ≃ m π c 2 and the system is intrinsically stable against Coulomb repulsion in the proton component. This approach is necessary, but not sufficient, when strong interactions are introduced.

The Klein first integrals in an equilibrium system with electromagnetic, weak, strong and gravitational interactions

Abstract The isothermal Tolman condition and the constancy of the Klein potentials originally expressed for the sole gravitational interaction in a single fluid are here generalized to the case of a three quantum fermion fluid duly taking into account the strong, electromagnetic, weak and gravitational interactions. The set of constitutive equations including the Einstein–Maxwell–Thomas–Fermi equations as well as the ones corresponding to the strong interaction description are here presented in the most general relativistic isothermal case. This treatment represents an essential step to correctly formulate a self-consistent relativistic field theoretical approach of neutron stars.

New perspectives in physics and astrophysics from the theoretical understanding of Gamma‐Ray Bursts

If due attention is given in formulating the basic equations for the Gamma‐Ray Burst (GRB) phenomenon and in performing the corresponding quantitative analysis, GRBs open a main avenue of inquiring on totally new physical and astrophysical regimes. This program is very likely one of the greatest computational efforts in physics and astrophysics and cannot be actuated using shortcuts. A systematic approach is needed which has been highlighted in three basic new paradigms: the relative space‐time transformation (RSTT) paradigm (Ruffini et al. [143]), the interpretation of the burst structure (IBS) paradigm (Ruffini et al. [144]), the GRB‐supernova time sequence (GSTS) paradigm (Ruffini et al. [145]). From the point of view of fundamental physics new regimes are explored: (1) the process of energy extraction from black holes; (2) the quantum and general relativistic effects of matter‐antimatter creation near the black hole horizon; (3) the physics of ultrarelativisitc shock waves with Lorentz gamma factor γ ...

Do we live on a lattice? Fermion masses from the Planck mass

Abstract The “no-go” theorem of Nielsen and Ninomiya, forbidding a sensible formulation of the usual electroweak action on a lattice, has been revisited proceeding from the hypothesis that space-time, as a result of the dynamics of quantum gravity, is a four-dimensional random lattice with constant a ≅ O ( r Pl ), the Planck length. We find that a sensible electroweak theory at long wavelengths is recovered by adding a chiral-gauge-invariant quadrilinear fermionic term. Dynamical symmetry breaking of Nambu-Jona-Lasinio type is shown to be crucial for making contact with known phenomenology. The relation of this approach with similar recent proposals is briefly discussed.

The elementary spike produced by a pure e+e- pair-electromagnetic pulse from a Black Hole: The PEM Pulse

In the framework of the model that uses black holes endowed with electromagnetic structure (EMBH) as the energy source, we study how an elementary spike appears to the detectors. We consider the simplest possible case of a pulse produced by a pure