• Volume 10, Issue 4

      December 1989,   pages  347-443

    • Stability of resonant planetary orbits in binary stars

      M. Michalodimitrakis F. Grigorelis

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      This paper contains a numerical study of the stability of resonant orbits in a planetary system consisting of two planets, moving under the gravitational attraction of a binary star. Its results are expected to provide us with useful information about real planetary systems and, at the same time, about periodic motions in the general four-body problem (G4) because the above system is a special case of G4 where two bodies have much larger masses than the masses of the other two (planets). The numerical results show that the main mechanism which generates instability is the destruction of the Jacobi integrals of the massless planets when their masses become nonzero and that resonances in the motion of planets do not imply, in general, instability. Considerable intervals of stable resonant orbits have been found. The above quantitative results are in agreement with the existing qualitative predictions

    • Periodic orbits in three-dimensional planetary systems

      S. Ichtiaroglou K. Katopodis Michalodimitrakis

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      Three-dimensional planetary systems are studied, using the model of the restricted three-body problem for Μ =.001. Families of three-dimensional periodic orbits of relatively low multiplicity are numerically computed at the resonances 3/1, 5/3, 3/5 and 1/3 and their stability is determined. The three-dimensional orbits are found by continuation to the third dimension of the vertical critical orbits of the corresponding planar problem

    • Analysis of Ca+ K plage area for short period variation

      Jagdev Singh S. K. Jain

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      We have analysed the observations of Solar Ca+K daily plage area for the period 1951-1977 to find evidence for the existence of short period (around 12–13 days) variation in the data. We divided the data in three groups—two corresponding to 10–20‡N and 10–20‡S latitude belts, and one corresponding to the total plage area—and used the power spectrum and autocorrelation techniques for the analysis. Both the techniques clearly show the 27-day periodicity due to solar rotation modulation in all the sets. A 12–13 day periodicity is seen in only 3, out of a total of 57 data sets when autocorrelation technique is used. A generally weak peak around 12–13 days is, however, seen in the power spectrum of all the data sets. The relative power in the 12–13 day peak is found to be significantly higher in those three data sets where the autocorrelation also shows this periodicity. On these two epochs the sunspot area distribution showed the existence of two distinct active longitudes separated by about 140–170 degrees. This seems to be the cause for the existence of a periodicity around 12–13 days in the autocorrelation and enhancement in the relative power of the 12–13 days peak in the power spectrum of these two epochs

    • Gaussian states in de Sitter spacetime and the evolution of semiclassical density perturbations. - 1. Homogeneous mode

      T. R. Seshadri T. Padmanabhan

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      The evolution of Gaussian quantum states in the de Sitter phase of the early universe is investigated. The potential is approximated by that of an inverted oscillator. We study the origin and magnitude of the density perturbations with special emphasis on the nature of the semiclassical limits

    • Gaussian states in de Sitter spacetime and the evolution of semiclassical density perturbations. 2. Inhomogeneous modes

      T. R. Seshadri T. Padmanabhan

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      In the computation of density perturbation in inflation it is conventional to assume the inflation field to be in the vacuum state. There are, however, some advantages in relaxing this assumption. In an earlier paper we have estimated the density perturbations in a Gaussian coherent state using a toy-model. Here we extend this work by doing an exact analysis of this problem. The advantages of this method is discussed and the results are compared with earlier results

    • Nature and distribution of dark matter: 2. binaries, groups and clusters

      M. M. Vasanthi T. Padmanabhan

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      We study the mass-radius relationship for aggregates of galaxies, viz. binaries, small groups and clusters. The data are subjected to a simple best-fit analysis similar to the one carried out earlier for individual field galaxies. The analysis shows that: (i) The data on binary galaxies are consistent with the assumption that binaries are just two galaxies, each with an individual isothermal (M ∫R) dark matter halo, moving under the mutual gravitational attraction, (ii) The data on the groups of galaxies are too scattered to obey a single power-law relation of the formM = kRn with any degree of reliability, (iii) The data on groups and clusters fit better with a law of the formM = AR3 +BR. This form suggests the existence of two components in dark matter—one which is clustered around the galaxies (M ∫R) and another which is distributed smoothly (M ∫R3). The smooth distributions becomes significant only at scales ≥ 1 Mpc and hence does not affect binaries significantly. We briefly discuss the theoretical implications of this analysis

    • Composite spectra - Paper 3: π aquilae

      R. & R. Griffin

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      π Aquilae is a visual double star whose angular separation of 1 ”.4 is so small that the system has been regarded as a composite-spectrum binary. However, by taking advantage of the excellence of the site and optics of the Mount Wilson 100-inch telescope, we have been able to obtain spectra of each component separately; the spectral types are about G8 III and A2V

    • Spectroscopic binaries near the North Galactic Pole paper 17: HD 111425

      R. F. Griffin

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      Photoelectric radial-velocity measurements show that HD 111425 is a double-lined spectroscopic binary, whose components probably have types of about F8 V and G6 V and are in a 51-day orbit of moderate eccentricity

  • 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.

    • Editorial Note on Continuous Article Publication

      Posted on July 25, 2019

      Click here for Editorial Note on CAP Mode

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