On the extension of the sensitive area of an extensive air shower surface array

A large distance between true and reconstructed core locations of an extensive air shower (EAS) may result in great systematic mis-estimation of EAS parameters. The reconstruction of those EASs whose core locations are outside the boundary of a surface array (outside EAS (OEAS)) results in a large distance of the reconstructed core location from the true one, especially when the true core is far outside the array. Although it may not be mentioned, the rejection of OEASs is a necessary and important step in the reconstruction procedure of an EAS. In this paper, an existing technique is optimized for the rejection of OEASs. The simultaneous use of this technique and a recently developed approach for reconstructing the core location of an EAS can significantly increase the sensitive area of a surface array.     

Bayesian Methods for Reconstructing Sunspot Numbers Before and During the Maunder Minimum

The Maunder Minimum (MM) was an extended period of reduced solar activity in terms of yearly sunspot numbers (SSN) during 1610?–?1715. The reality of this “grand minimum” is generally accepted in the scientific community, but the statistics of the SSN record suggest a need for data reconstruction. The MM data show a nonstandard distribution compared with the entire SSN signal (1610?–?2014). The pattern does not satisfy the weakly stationary solar dynamo approximation, which characterizes many natural events spanning centuries or even millennia, including the Sun and the stars. Over the entire observation period (1610?–?2014), the reported SSN exhibits statistically significant regime switches, departures from autoregressive stationarity, and growing trends. Reconstruction of the SSN during the pre-MM and MM periods is performed using five novel statistical procedures in support of signal analysis. A Bayesian–Monte Carlo backcast technique is found to be most reliable and produces an SSN signal that meets the weak-stationarity requirement. The computed MM signal for this reconstruction does not show a “grand” minimum or even a “semi-grand” minimum.     

An Infra-Red model of the zodiacal emission

The Infra-Red Astronomical Satellite (IRAS) observations of the zodiacal dust emission are used to fit the dust grain composition and distribution in the ecliptical plane. We obtain a good fit to the data for a density distribution of black-body grains given by p = pr ^{0.66/log(1.7r/R)} for r < 0.87R and r < 3oR     

On the Evolution of Bands in the Dynamic Spectra of Solar Type II Radio Bursts

Astronomy Letters - Based on an analysis of the dynamic spectra for solar flares in the meter wavelength range obtained with the ground-based Radio Solar Telescope Network, we consider the...     

Main sequence for rotating stars of intermediate mass

We have investigated the evolutionary behaviour of intermediate mass (2, 3, 4, 5, and 7M ) Population I stars, assuming two different rates of rotation at the threshold of stability.In the first part of the study, stars are assumed to start with a critical rotation (fast rotation model) and to progress to the point of rotational instability. The stars evolve by losing mass and become rotationally unstable before they reach the zero-age Main Sequence. It is argued that multiple star systems might be formed through the evolution of rapidly rotating stars. An expression for the rotational mass loss rate is derived as a function of the physical parameters of stars.In the second part of the study, stars are assumed to rotate at a rate below the critical value (slow rotation model). The evolution of slowly rotating stars is followed as far as zero-age Main Sequence on the theoretical Hertzsprung-Russell diagram and compared with that of normal stars. The evolutionary paths are found to be more or less similar to those of normal stars; but their positions on the Main Sequence are characterized by effective temperatures and luminosities lower than those of normal stars. The zero-age Main-Sequence times of these stars are longer than those of normal stars. The rotational rates obtained for the zero-age Main Sequence are in good agreement with observed values.     

The effect of spatial smearing on solar Doppler measurements

A general mathematical formulation of the effect of spatial smearing on solar velocity measurements is presented. The variations of the straylight induced error with wavelength and line parameters are discussed. The spatial and time dependence of the error will influence the measurement of solar limb effect and may introduce fictitious large scale velocity fields with amplitudes of the order of a few m/s.Present address: Space Science Department of ESA, ESTEC, Noordwijk, The Netherlands.     

On the spectrum of a gaseous nebula of pure hydrogen,I

The emissivity for the two photons decay from the metastable level 2s has been computed in the case of a gaseous nebula of pure hydrogen, with both radiative and collisional excitation of the states.The populations of 2s and 2p levels are deduced from the condition of equilibrium with other levels. Electron temperatures between 10⁴ and 4×10⁴K and electron densities between 10⁴ and 10⁶ cm^–3 have been investigated.For the optically thin case Ly intensity has also been computed.In the case of collisional excitation a much greater efficiency for the two photons process is found, which profoundly affects the appearance of the continuous spectrum.     

Catalog of X-Ray Active Galactic Nuclei Based on ROSAT BSC and FSC Sources

Astrophysics - A general catalog of active galactic nuclei (AGN) has been created from identified optical sources of X-ray data from the Hamburg-ROSAT Catalog (HRC) and the Byurakan-Hamburg ROSAT...     

On the formation of metal-poor stars

The expulsion of metal-rich grains from collapsing protostars is considered, and it is concluded that stars of mass greater than 21M could be significantly depleted in heavy metals during their formation.