Volume 37, Issue 1
March 2016
Article ID 0009369 March 2016
A. A. Yeghiazaryan T. A. Nazaryan A. A. Hakobyan
The quartet of galaxies NGC 7769, 7770, 7771 and 7771A is a system of interacting galaxies. Close interaction between galaxies caused characteristic morphological features: tidal arms and bars, as well as an induced star formation. In this study, we performed the Fabry–Perot scanning interferometry of the system in $\rm{H}\alpha$ line and studied the velocity fields of the galaxies. We found that the rotation curve of NGC 7769 is weakly distorted. The rotation curve of NGC 7771 is strongly distorted with the tidal arms caused by direct flyby of NGC 7769 and flyby of a smaller neighbor NGC 7770. The rotation curve of NGC 7770 is significantly skewed because of the interaction with the much massive NGC 7771. The rotation curves and morphological disturbances suggest that the NGC 7769 and NGC 7771 have passed the first pericenter stage, however, probably the second encounter has not happened yet. Profiles of surface brightness of NGC 7769 have a characteristic break, and profiles of color indices have a minimum at a radius of intensive star formation induced by the interaction with NGC 7771.
Article ID 0009370 March 2016
Ragadeepika Pucha K. M. Hiremath Shashanka R. Gurumath
Sunspots are the most conspicuous aspects of the Sun. They have a lower temperature, as compared to the surrounding photosphere; hence, sunspots appear as dark regions on a brighter background. Sunspots cyclically appear and disappear with a 11-year periodicity and are associated with a strong magnetic field $(\sim 10^3$ G) structure. Sunspots consist of a dark umbra, surrounded by a lighter penumbra. Study of umbra–penumbra area ratio can be used to give a rough idea as to how the convective energy of the Sun is transported from the interior, as the sunspot’s thermal structure is related to this convective medium. An algorithm to extract sunspots from the white-light solar images obtained from the Kodaikanal Observatory is proposed. This algorithm computes the radius and center of the solar disk uniquely and removes the limb darkening from the image. It also separates the umbra and computes the position as well as the area of the sunspots. The estimated results are compared with the Debrecen photoheliographic results. It is shown that both area and position measurements are in quite good agreement.
Article ID 0009371 March 2016
Joginder Singh Dhiman Rajni Sharma
The self-gravitating instability of an infinitely extending axisymmetric cylinder of viscoelastic medium permeated with non uniform magnetic field and rotation is studied for both the strongly coupled plasma (SCP) and weakly coupled plasma (WCP). The non uniform magnetic field and rotation are considered to act along the axial direction of the cylinder. The normal mode method of perturbations is applied to obtain the dispersion relation. The condition for the onset of gravitational instability has been derived from the dispersion relation under both strongly and weakly coupling limits. It is found that the Jeans criterion for gravitational collapse gets modified due to the presence of shear and bulk viscosities for the SCP, however, the magnetic field and rotation whether uniform or non uniform has no effect on the Jeans criterion of an infinitely extending axisymmetric cylinder of a self-gravitating viscoelastic medium.
Article ID 0009373 March 2016
Hubble’s Law Implies Benford’s Law for Distances to Galaxies
Theodore P. Hill Ronald F. Fox
A recent article by Alexopoulos and Leontsinis presented empirical evidence that the first digits of the distances from the Earth to galaxies are a reasonably good fit to the probabilities predicted by Benford’s law, the well known logarithmic statistical distribution of significant digits. The purpose of the present article is to give a theoretical explanation, based on Hubble’s law and mathematical properties of Benford’s law, why galaxy distances might be expected to follow Benford’s law. The new galaxy-distance law derived here, which is robust with respect to change of scale and base, to additive and multiplicative computational or observational errors, and to variability of the Hubble constant in both time and space, predicts that conformity to Benford’s law will improve as more data on distances to galaxies becomes available. Conversely, with the logical derivation of this law presented here, the recent empirical observations may be viewed as independent evidence of the validity of Hubble’s law.
Article ID 0009375 March 2016
Einstein–Maxwell Field Equation in Isotropic Coordinates: An Application to Modeling Superdense Star
Neeraj Pant Mohammad Ahmad N. Pradhan
We present a charged analogue of Pant et al. (2010, Astrophys.Space Sci., 330, 353) solution of the general relativistic field equations in isotropic coordinates by using simple form of electric intensity $E$ that involve charge parameter $K$. Our solution is well behaved in all respects for all values of $X$ lying in the range 0 < $X \leq 0.11$, $K$ lyingin the range 4 < $K \leq 6.2$ and Schwarzschild compactness parameter $u$ lying in the range 0 < $u \leq 0.247$. Since our solution is well behaved for wide ranges of the parameters, we can model many different types of ultra-cold compact stars like quark stars and neutron stars. We have shown that corresponding to $X = 0.077$ and $K = 6.13$ for which $u = 0.2051$ and by assuming surface density $ρb = 4.6888 × 10^14 {\rm g cm}^(−3)$ the mass and radius are found to be 1.509 $M_\odot$, 10.906 km respectively which match with the observed values of mass 1.51 $M_\odot$ and radius 10.90 km of the quark star XTE J1739-217. The well behaved class of relativistic stellar models obtained in this work might have astrophysical significance in the study of more realistic internal structures of compact stars.
Article ID 0009376 March 2016
The propagation of magnetoacoustic waves in the neighbourhood of a 2D null point is investigated for both $\beta =$ 0 and $\beta$ $\neq$ 0 plasmas. Previous work has shown that the Alfvén speed, here $\nu_A \propto r$, plays a vital role in such systems and so a natural choice is to switch to polar coordinates. For $\beta =$ 0 plasma, we derive an analytical solution for the behaviour of the fast magnetoacoustic wave in terms of the Klein–Gordone equation. We also solve the system with a semi-analytical WKB approximation which shows that the $\beta =$ 0 wave focuses on the null and contracts around it but, due to exponential decay, never reaches the null in a finite time. For the $\beta$ $\neq$ 0 plasma, we solve the system numerically and find the behaviour to be similar to that of the $\beta =$ 0 system at large radii, but completely different close to the null. We show that for an initially cylindrically-symmetric fast magnetoacoustic wave perturbation, there is a decrease in wave speed along the separatrices and so the perturbation starts to take on a quasi-diamond shape; with the corners located along the separatrices. This is due to the growth in pressure gradients that reach a maximum along the separatrices, which in turn reduces the acceleration of the fast wave along the separatrices leading to a deformation of the wave morphology.
Article ID 0009378 March 2016 Editorial
Current Issue
Volume 40 | Issue 5
October 2019
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