Can a Strong Radio Burst Escape the Magnetosphere of a Magnetar?

We examine the possibility that fast radio bursts (FRBs) are emitted inside the magnetosphere of a magnetar. On its way out, the radio wave must interact with a low-density e ± plasma in the outer magnetosphere at radii R = 109–1010 cm. In this region, the magnetospheric particles have a huge cross section for scattering the wave. As a result, the wave strongly interacts with the magnetosphere and compresses it, depositing the FRB energy into the compressed field and the scattered radiation. The scattered spectrum extends to the γ-ray band and triggers e ± avalanche, further boosting the opacity. These processes choke FRBs, disfavoring scenarios with a radio source confined at R ≪ 1010 cm. Observed FRBs can be emitted by magnetospheric flare ejecta transporting energy to large radii.

Post-Merger Financial Performance of ICICI Bank

India has witnessed Mergers and Acquisitions across sectors and the most talked about mergers are those in the Banking sector. The banking sector attracts more attention because of the wide geographic spread and the scattered spectrum of stakeholders. Post liberalization banking sector has grown by leaps and bounds and has also seen a lot of mergers and acquisitions. ICICI bank is one of the biggest players among the private sector banks, adopted the merger and acquisition route for expansion. It witnessed four mergers and the same have been studied in this paper. Evaluation of the mergers has been done using the CAMEL model. For the study, three years’ pre-merger data and three years’ post-merger data have been taken into consideration. It was found that there was no significant improvement in the financial performance of ICICI Bank post these mergers.

Mitos dan Eksplanasi Ilmiah Lembayung Senja

A Violaceous sky attwilightis a natural phenomenon that occurs at sunset. This phenomenon is characterized by areddish yellow sky appearance. To explain this phenomenon, the community has developed a myth that connects the existence of the occult things such as the decline of the evil ghosts, witchcraft, and the epidemic of the disease. This myth has survived long enough in both sundanesse and Banjarmasin, South Kalimantan. The myth is spread in the community from mouth to mouth and occurs from generation to generation. Development of science and the changing minds of modern society effect myths that are present in society began to be degraded by scientific explanations reinforced by empirical evidences. The explanation used in explaining the twilight phenomenon uses the Hempel-Oppenheim explanation model. The explanationsare considered as general statementsconsidered correct. The Violaceous sky at twilight does not indicate the presence of ghosts, witches, or epidemics but it can be explained by Rayleigh scattering theory. The white light from the sun is dissipated by the atmospheric particles into the monochromatic spectrum. As a result of longer stages, the scattered spectrum has the longest wavelength

Compton Scattering Experiments with Polychromatic Radiation

We show an iterative algorithm that allows to obtain accurate Compton profiles J(q) from Compton scattering spectra I2 (ω2), if the excitation radiation is not strictly monochromatic. It requires knowledge of the spectral distribution of the primary radiation I1(ω1), validity of the impulse approximation and dominance of a monochromatic part in I1(ω1) over the polychromatic rest. Conversely, the primary spectrum is often experimentally not directly accessible. In such a situation it is possible to evaluate the primary spectrum I1(ω1) from the spectrum of scattered photons, I2(ω2), with a similar iterative algorithm. We use a scattering target of high atomic number in order to ensure that the elastically scattered photons dominate the inelastically scattered ones. From the scattered spectrum we get a model for the Compton profile that allows us to separate the inelastic part of the scattered spectrum from the elastic part, which, in turn, is proportional to the spectral distribution of the primary radiation.

Polarization of IRAS Quasars and the Inner Structure of Active Galactic Nuclei

We have found that 4 new, bright IRAS quasars, out of 7 observed, have strong, non-variable, wavelength-dependent polarization. Three show degrees of polarization, pλ, increasing from infrared to UV wavelengths (Fig. 1), which implies a combination of a polarized, scattered spectrum and a much redder, unpolarized spectrum. Detailed IR and optical polarimetry and spectrophotometry of one, IRAS 13349+2438 (Wills et al.), shows a polarized flux spectrum, pλxFλ, (continuum and Pa α, Hα, and Hβ broad hydrogen lines) typical of unreddened, luminous quasars. This suggests that the path of scattered light from a central, luminous quasar is low in dust and that the polarization of the scattered spectrum is wavelength independent. The latter is most easily explained by electron scattering although the data do not exclude dust scattering. When this polarized flux spectrum is subtracted from the total spectrum, we are left with a very reddened line and continuum spectrum, E(B-V) = 0.3 to 0.7, which we attribute to the same luminous quasar seen through a thick dusty torus. The angle of polarization is parallel to the major axis of the r-band image, presumed to be that of the host galaxy. If the torus is in the plane of the galaxy, the axial ratio suggests a viewing angle of 40° to the plane of the torus. Fig. 2 illustrates the geometry. The appearance of the quasar at optical and UV wavelengths will depend strongly on viewing angle, suggesting that present samples of quasars selected by colours, optical flux density, or quasi-stellar appearance, may be seriously biased, with important consequences for studies of the space density and evolution of AGN.

Some Anomalies in the Raman spectrum from laser-produced plasmas

Many experiments show features of the Raman spectrum at variance with the predictions of conventional theory. One persistent discrepancy, the cut-off in the spectrum of scattered light at about 1·5λ0, led Simon and Short to postulate that the scattered spectrum is not Raman light as such, but derives from enhanced Thomson scattering from plasmas in which a population of suprathermal electrons is present. We describe a set of simulations which model the propagation of a light wave through a plasma characterized by two electron temperatures with the hot electron fraction varying between 0 and 0·05. The results show that enhanced Thomson scattering will contribute to the spectra observed in some experiments at least and confirm the contention that the spectrum of the scattered light is not especially sensitive to the width of the suprathermal electron feature. We have also examined the effect of a finite quiver velocity on the enhanced Thomson spectrum as a function of the population of suprathermal electrons, in particular its effect on the wavelength bands.