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1.
The effect of particle-particle interaction on the adiabatic index γ for an electron-positron plasma is considered. An improved method for numerically calculating the Hartree-Fock exchange integral is presented and its relativistic asymptotics is determined. An approximation formula is derived for the correlation part of the interaction in the low-density limit. This formula includes degeneracy and the positron component. 相似文献
2.
A series of hydrodynamical models of type-II supernova outbursts (SNII) has been calculated. Approximate relations connecting the total outburst energy ε, the mass of envelope ejectedM, the presupernova radiusR, and the amount of ionizing quanta radiated by the supernovaeN H with such values as the duration of the light curve plateau Δt, and absolute magnitude in the wavelength bandV and photospheric velocityU PH observed near the middle of the plateau have been established. Advantage has been taken of the relations to obtain a preliminary evaluation for the characteristics of the average SN II: ε=7×1050 erg,M=6M ⊙,R=500R ⊙,N H=2×1058. The SNIIs with plateau-like light curves seem to be accounted for by thermonuclear explosions of degenerate cores of red giant stars and result in a total disruption of the star without any stellar remnant. To the contrary, SNIIs with linear light curves have substantially different properties (in particular, they throw considerably less massive envelopes off). These SNII must signify the birth of collapsed objects—neutron stars (pulsars) or black holes. 相似文献
3.
A catalog of massive (⩾10 M
⊙) stars in binary and multiple systems with well-known masses and luminosities has been compiled. The catalog is analyzed
using a theoretical mass-luminosity relation. This relation allows both normal main-sequence stars and stars with peculiarities:
with clear manifestations of mass transfer, mass accretion, and axial rotation, to be identified. Least-squares fitting of
the observational data in the range of stellar masses 10M
⊙ ⩽ M ≲ 50 M
⊙ yields the relation L ∼ M
2.76.
An erratum to this article is available at . 相似文献
4.
We propose an iterative algorithm for computing the synthesis of heavy elements through the rapid capture of neutrons (r-process) and, at sufficiently high temperatures, protons by simultaneously using two distinct computer codes. One of the codes describes the kinetics of nuclear reactions between light and intermediate chemical elements, which are the source of free neutrons and protons used by the second code to synthesize heavy elements from seed nuclides (isotopes near the iron peak of the cosmic abundance curve). The two codes interact through the neutron and proton reaction channels. We demonstrate the efficiency of our method with an example of the nucleosynthesis in a supernova’s helium shell triggered by the evaporation of neutrons and protons from α particles exposed to the neutrino flux from a collapsing stellar core. In this case, three or four iterations are enough to obtain an almost exact self-consistent solution. 相似文献
5.
We investigate a three-parameter equation of state for stellar matter under nuclear statistical equilibrium conditions in the ranges of temperatures 3×109–1011 K and densities 104–1013 g cm?3 and for various ratios of the total number of neutrons to the total number of protons within the range 1–1.5. These conditions correspond to the initial stages of the gravitational collapse of iron stellar cores that are accompanied by nonequilibrium matter neutronization. We analyze the effect of the excited levels of atomic nuclei on the thermodynamic properties of the matter. We show that this effect is insignificant at low densities, ρ?1010 g cm?3, but it leads to an expansion of the instability region, γ<4/3, at higher densities. The incorporated effects of the Fermi degeneracy of free nucleons prove to be insignificant, because their concentrations are low at low temperatures. In the future, we plan to investigate the effects of Coulomb interactions and neutron-rich nuclei on the thermodynamic properties of the matter. 相似文献
6.
In the domain of thermodynamic parameters characteristic of the initial collapse of iron stellar cores, we studied the influence of Coulomb interaction on the thermodynamic functions of a plasma under nuclear statistical equilibrium conditions. Our attention was focused on the nuclear component of the matter. We established that including the interaction shifts the equilibrium toward the nuclei with larger charges. However, this effect and the changes in thermodynamic quantities are noticeable only at high densities (ρ ? 1011 g cm?3), i.e., at an advanced stage of gravitational collapse. We also showed that the mean ion model is inadequate in regions with a coupling parameter Γ ～ 1. We point out a method for modifying the linear mixing model to properly pass to the Debye limit and discuss other multicomponent plasma models. 相似文献
7.
Dependence of the acceleration of the outer edge of a stellar envelope on supernova explosion energy
Based on numerical simulations of a supernova explosion, we investigate the shock-wave breakout through the stellar surface. The computations have been performed in a wide range of explosion energies and presupernova masses. The results are compared with the classical Gandelman-Frank-Kamenetsky self-similar solution. We have determined the dependence of an arbitrary coefficient in the self-similar solution on the explosion energy and presupernova structure. The derived analytical approximation formula for this coefficient can be used to estimate the supernova explosion energy from such parameters of the ejected envelope determined from astronomical observations as its maximum expansion velocity and the density distribution along its outer edge. The formula may prove to be also useful in studying the X-ray and gamma-ray bursts that accompany the shock-wave breakout through the surface of compact presupernovae. 相似文献
8.
We have developed an algorithm for taking into account the neutrino scattering in the approximation of neutrino heat conduction. We show that in the case of incoherent neutrino scattering (e.g., by electrons), the coefficients of the temperature and chemical potential gradients are averaged over the neutrino energy using functions that can be found by numerically solving integral equations. The coherent scattering by free nucleons and atomic nuclei can be described by introducing a transport cross section. We suggest a new method for calculating the neutrino—electron scattering functions that is based on Fermi—Dirac functions of integer indices. 相似文献
9.
The similarity theory of stellar models is used to study the properties of very massive stars when all the opacity sources, except the Thomson scattering, can be disregarded. The dimensionless internal structure of such stars is essentially independent of the energy generation law. It is shown that the mass-luminosity relation can be fitted by an analytical expression that is virtually universal with regard to the chemical composition and the energy generation law. A detailed comparison with the Eddington standard model is made. The application of the results obtained to the observations of massive stars is briefly discussed. 相似文献
10.