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      Volume 39, Issue 5

      October 2018

    • A comparative study of geomagnetic storms for solar cycles 23 and 24


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      The aim of this paper is to investigate the association of the geomagnetic storms with themagnitude of interplanetary magnetic field IMF ($B$), solar wind speed ($V$), product of IMF and wind speed ($V\cdot B$), Ap index and solar wind plasma density ($n_{\rm p}$) for solar cycles 23 and 24. A Chree analysis by the superposed epoch method has been done for the study. The results of the present analysis showed that $V\cdot B$ is more geoeffective when compared to V or B alone. Further the high and equal anti-correlation coefficient is found between Dst and Ap index ($−$0.7) for both the solar cycles. We have also discussed the relationship between solar wind plasma density (np) and Dst and found that both these parameters are weakly correlated with each other. Wehave found that the occurrence of geomagnetic storms happens on the same day when IMF, $V$, Ap and $V\cdot B$ reach their maximum value while 1 day time lag is noticed in case of solar wind plasma density with few exceptions. The study of geomagnetic storms with various solar-interplanetary parameters is useful for the study of space weather phenomenon.

    • Dynamical model of binary asteroid systems using binary octahedrons


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      We used binary octahedrons to investigate the dynamical behaviors of binary asteroid systems. The mutual potential of the binary polyhedron method is derived from the fourth order to the sixth order. The irregular shapes, relative orbits, attitude angles, as well as the angular velocities of the binary asteroid system are included in the model. We investigated the relative trajectory of the secondary relative to the primary, the total angular momentum and total energy of the system, the three-axis attitude angular velocity of the binary system,as well as the angular momentum of the two components. The relative errors of the total angular momentum and the total energy indicate that the calculation has a high precision. It is found that the influence of the orbital and attitude motion of the primary from the gravitational force of the secondary is obvious. This study is useful in understanding the complicated dynamical behaviors of the binary asteroid systems discovered in our Solar system.

    • Short timescale UV variability study in NGC 4151 using IUE data


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      IUE has made very successful long term and intense short time-scale monitoring spectroscopic study of NGC 4151, a Seyfert 1 galaxy for over nearly 18 years from its launch in 1978 to 1996. The long-term observations have been useful in understanding the complex relation between UV continuum and emission line variability Seyfert galaxies. In this paper, we present the results of our studies on the short-timescale intense monitoring campaign of NGC 4151 undertaken during December 1–15, 1993. A most intense monitoring observation of NGC 4151 was carried out by IUE in 1993, when the source was at its historical high flux state with a shortest interval of 70 min between two successive observations.We present our results on emission line and continuum variability amplitudes characterized by $F_{\rm var}$ method.We found highest variability of nearly 8.3% at 1325 Å continuum with a smallest amplitude of 4% at 2725 Å. The relative variability amplitudes ($R_{\rm max}$) have been found to be 1.372, 1.319, 1.302 and 1.182 at 1325, 1475, 1655 and 2725 Å continuum respectively. The continuum and emission line variability characteristics obtained in the present analysis are in very good agreement with the results obtained by Edelson et al. (1996) and Crenshaw et al. (1996) from the analysis of the same observational spectral data. The large amplitude rapid variability characteristics obtained in our study have been attributed to the continuum reprocessing of X-rays absorbed by the material in the accretion disk as proposed by Shakura and Sunyaev (1973). The continuum and emission light curves have shown four distinct high amplitude events of flux maxima during the intense monitoring campaign of 15 days, providing a good limit on the amplitude of UV variability and the BLR size in low luminosity Seyfert galaxies and are useful for constraining the continuum emission models. The decreasing $F_{\rm var}$ amplitude of UV continuum with respect to increasing wavelength obtained in the present study and consistent with similar observations by Edelson et al. (1996) and Crenshaw et al. (1996) is a significant result of the intense monitoring observations.

    • Transition between general relativity and quantum gravity using quark and strange quark matter with some kinematical test

      V. R. CHIRDE S. H. SHEKH

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      Contemporary piece of writing devotes to the investigation of plane symmetric cosmological model with quark and strange quark matter in the deformations of the Einstein’s theory of General Relativity (GR). At small or large scales (ultraviolet or infrared gravity), deformations of the Einstein’s theory could provide a better handling of cosmic acceleration without magnetism (along with singularities). In particular, a proper deformation of GR in the ultraviolet regime could play the role of describing the transition between GR and quantum gravity. As a matter of fact, although with a different purpose in mind, it was Einstein himself who proposed in the 30’s the reformulation of GRby taking the field of orthonormal frames or tetrads as the dynamical variable instead of the metric tensor (Einstein, Phys. Math. Kl 217, 401, 1928). As per the observation, pressure and energy density of the model approaches the bag constant in negative and positive ways at $t\to \infty$, i.e. $p \to −B_c$ and $\rho \to B_c$, the negative pressure due to the Dark Energy (DE) in the context of accelerated expansion of the universe. So the strange quark matter gives an idea of existence of dark energy in the universe and supports the observations of the SNe-I (Riess et al., Astron. J. 116,1009, 1998; Perlmutter et al. Astrophys. J. 517, 565, 1999). Also these results agree with the study of Aktas and Aygun (Chinese J. Phys. 55, 71, 2017) and Sahoo et al. (New. Astron. 60, 80, 2018).

    • Circular restricted three-body problem when both the primaries are heterogeneous spheroid of three layers and infinitesimal body varies its mass


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      The circular restricted three-body problem, where two primaries are taken as heterogeneous oblate spheroid with three layers of different densities and infinitesimal body varies its mass according to the Jeans law, has been studied. The system of equations of motion have been evaluated by using the Jeans law and hence the Jacobi integral has been determined. With the help of system of equations of motion, we have plotted the equilibrium points in different planes (in-plane and out-of planes), zero velocity curves, regions of possible motion, surfaces (zero-velocity surfaces with projections and Poincaré surfaces of section) and the basins of convergence with the variation of mass parameter. Finally, we have examined the stability of the equilibrium points with the help of Meshcherskii space–time inverse transformation of the above said model and revealed that all the equilibrium points are unstable.

    • Stellar parameters of the two binary systems: HIP 14075 and HIP 14230


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      We present the stellar parameters of the individual components of the two old close binary systems HIP14075 and HIP14230 using synthetic photometric analysis. These parameters are accurately calculated based on the best match between the synthetic photometric results within three different photometric systems with the observed photometry of the entire system. From the synthetic photometry,we derive the masses and radii of HIP14075 as ${\mathcal M}^A = 0.99\pm 0.19{\mathcal M}^{\odot}$, $R_A = 0.877\pm 0.08R_{\odot}$ for the primary and ${\mathcal M}^B = 0.96\pm 0.15{\mathcal M}_{\odot}$,$R_B = 0.821\pm 0.07R_{\odot}$ for the secondary, and of HIP14230 as ${\mathcal M}^A = 1.18\pm 0.22{\mathcal M}_{\odot}$, $R_A = 1.234\pm 0.05R_{\odot}$ for the primary and ${\mathcal M}^B = 0.84 \pm 0.12{\mathcal M}_{\odot}$, $R^B = 0.820\pm 0.05R_{\odot}$ for the secondary. Both systems depend on Gaia parallaxes. Based on the positions of the components of the two systems on a theoretical Hertzsprung–Russell diagram, we find that the age of HIP 14075 is $11.5\pm 2.0$ Gyr and of HIP 14230 is $3.5\pm 1.5$ Gyr.Our analysis reveals that both systems are old close binary systems ($\approx$>4 Gyr). Finally, the positions of the components of both the systems on the stellar evolutionary tracks and isochrones are discussed.

    • Behaviour of physical parameters in extended gravity with hyperbolic function


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      In this paper, we have constructed the cosmological model of the universe in $f (R, T)$ theory of gravity in a Bianchi type VI$_h$ universe for the functional $f (R, T)$ in the form $f (R, T) = \mu R + \mu T$, where $R$ and $T$ are respectively Ricci scalar and trace of energy momentum tensor and $\mu$ is a constant. We have made use of the hyperbolic scale factor to find the physical parameters and metric potentials defined in the space-time. The physical parameters are constrained from different representative values to build up a realistic cosmological model aligned with the observational behaviour. The state finder diagnostic pair is found to be in the acceptable range. The energy conditions of the model are also studied.

    • Installation of solar chromospheric telescope at the Indian Astronomical Observatory, Merak


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      We report the observations of the solar chromosphere from a newly commissioned solar telescope at the incursion site near Pangong Tso lake in Merak (Leh/Ladakh). This new Hα telescope at the Merak site is identical to the Kodaikanal H$_{\alpha}$ telescope. The telescope was installed in the month of August 2017 at the Merak site. The telescope consists of a 20-cm doublet lens with additional re-imaging optics. A Lyot filter with 0.5 Å passband isolates the Balmer line of the hydrogen spectra to make the observations of the solarchromosphere. The observations made in Hα wavelength delineates the magnetic field directions at the sunspot and the quiet regions. A CCD detector records the images of the chromosphere with a pixel resolution of 0.27$''$and covers 9.2$'$ field-of-view. This telescope has a good guiding system that keeps the FoV in the intended position. We report the development of control software for tuning the filter unit, control detector system, observations and calibration of the data to make it useful for the scientific community. Some preliminary results obtained from the Merak H$_{\alpha}$ telescope are also presented. This high altitude facility is a timely addition to regularly obtain H$_{\alpha}$ images around the globe.

    • Template-based classification of SDSS-GALEX point sources


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      We have classified a sample of 37,492 objects from SDSS into QSOs, galaxies and stars using photometric data over five wave bands ($u, g, r , i$ and $z$) and UV GALEX data over two wave bands (near-UV and far-UV) based on a template fitting method. The advantage of this method of classification is that it does not require any spectroscopic data and hence the objects for which spectroscopic data is not available can also be studied using this technique. In this study, we have found that our method is consistent by spectroscopic methods given that their UV information is available. Our study shows that the UV colours are especially important for separating quasars and stars, as well as spiral and starburst galaxies. Thus it is evident that the UVbands play a crucial role in the classification and characterization of astronomical objects that emit over a wide range of wavelengths, but especially for those that are bright at UV. We have achieved the efficiency of 89% for the QSOs, 63% for the galaxies and 84% for the stars. This classification is also found to be in agreement with the emission line diagnostic diagrams.

    • Cosmological implications of exponential harmonic field with collisional matter


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      We have studied the evolution of cosmological parameters by considering exponential harmonic field with collisional matter. A comparison has been made with the behavior of these parameters in the presence of ordinary matter and the model $\Lambda CDM$. We have also compared the evolution of these parameters with the ones obtained in the modified gravity $f (R)$ and $f (R, T)$ theory case. The results are in line with those of the modified gravity so that the harmonic exponential field can be used to explain why the Universe has gone from the deceleration phase to the acceleration phase.

    • Halo orbit of regularized circular restricted three-body problem with radiation pressure and oblateness


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      In this paper, computation of the halo orbit for the KS-regularized photogravitational circular restricted three-body problem is carried out. This work extends the idea of Srivastava et al. (Astrophys. Space Sci. 362: 49, 2017) which only concentrated on the (i) regularization of the 3D-governing equations of motion, and (ii) validation of the modeling for small out-of-plane amplitude ($A_z = 110000$ km) assuming the third order analytical approximation as an initial guess with and without differential correction. This motivated us to compute the halo orbits for the large out-of-plane amplitudes and to study their stability analysis for the regularized motion. The stability indices are described as a function of out-of-plane amplitude, mass reduction factor and oblateness coefficient. Three different Sun–planet systems: the Sun–Earth, Sun–Mars and the Sun–Jupiter are chosen in this study. Stable halo orbits do not exist around the $L_1$ point, however, around the $L_2$ point stable halo orbits are found for the considered systems.

  • Journal of Astrophysics and Astronomy | News

    • Continuous Article Publication

      Posted on January 27, 2016

      Since January 2016, the Journal of Astrophysics and Astronomy has moved to Continuous Article Publishing (CAP) mode. This means that each accepted article is being published immediately online with DOI and article citation ID with starting page number 1. Articles are also visible in Web of Science immediately. All these have helped shorten the publication time and have improved the visibility of the articles.

© 2017 Indian Academy of Sciences, Bengaluru.