ARIES Insitutional Digital Repositary (ARIES-IDR): Recent submissions

  • On the behaviour of some visible and infrared atomic hydrogen lines in facular models 
    Bondal, K. R.; Gaur, V. P.; Pande, M. C. (1986)
    The behaviour of line profiles in the wings of the Balmer, Paschen, and Brackett lines (alpha to delta) has been theoretically investigated in five facular models at disc centre. These profiles have been compared amongst ...
  • Ultraviolet and infrared excess emission in Be stars 
    Goraya, P. S. (1986)
    Spectrophotometric observations of 26 Be stars are reported and analyzed in the wavelength range λ3200 to λ8000 Å. Two observational features readily noted in these stars are: (i) a Balmer discontinuity smaller than that ...
  • The spectrum of periodic comet Encke 
    Goraya, P. S.; Sanwal, B. B.; Rautela, B. S. (1986)
    Periodic comet Encke (P/Encke) was observed spectrophotometrically during its apparition in 1984 march, before perihelion. We observed emission features due to CN and C₂ molecules, but sodium emission was absent from the ...
  • Initial mass functions of Wolf-Rayet stars 
    Singh, M. (1986)
    On the basis of evolutionary tracks on the HR diagram the lower limit of initial mass functions for Wolf-Rayet stars are estimated. The lower limit to the initial masses of the Wolf-Rayet stars seems to be 20 Mʘ and in ...
  • On association of radio emission with solar surges 
    Verma, V. K. (1986)
    About 45% non-flare surges are found to be associated with radio bursts inferred from spectral data. Associated surges are mostly accompanied by type I (24%) and type III (29%) bursts.
  • Cyanogen lines and facula models 
    Tripathi, B. M.; Sinha, K. (1986)
    Predicted equivalent widths and profiles of facular CN lines are used here as a diagnostic tool for different model atmospheres.
  • The age distribution and total lifetimes of open clusters 
    Pandey, A. K.; Mahra, H. S. (1986)
    The age distribution of galactic clusters is obtained from well-observed star clusters, and it is concluded that the observed age distribution of clusters within 1000 pc is not seriously affected by the selection effects. ...
  • Photometric study of BZ Eridani 
    Srivastava, R. K.; Uddin, W. (1986)
    The 1980-1981 U, B and V observations of the eclipsing binary BZ Eridani have been presented. A new period of BZ Eri comes out to be 0. ͩ 6641703. The colour curves of the system show appreciable variations, and are ...
  • Atmospheric precipitable water vapour over Manora Peak, Naini Tal 
    Bhatt, B. C.; Mahra, H. S. (1987)
    Precipitable water vapour is one of the variable atmospheric constituents and its short-term and seasonal variations may affect the infrared photometric observations. From the analysis of the measurements, made at Manora ...
  • On the oscillations of a composite stellar model with a weak magnetic field 
    Kar, J. (1987)
    The unrestricted second-order virial tensor formalism has been used to calculate the characteristic frequencies of linear adiabatic oscillations of a composite stellar model having an isothermal core and a polytropic envelop ...
  • Period changes in EI Cephei 
    Srivastava, R. K. (1987)
    A new period (P = 8.ͩ 439422) of the eclipsing binary system EI Cephei has been given, which is based on all available times of minima. Periods using Strohmeier's (1958) epoch have also been presented for the observations ...
  • Delta Cap: a possible RS CVn binary 
    Srivastava, R. K. (1987)
    The eclipsing binary δ Cap (B-16°5943) was known to be a single line spectroscopic binary. Slipher (1906) first detected variable radial velocity in δ Cap. Crump (1921), Luyten (1936), Stewart (1958) and Batten (1961) ...
  • Variations in P/Halley, 1986 January 
    Goraya, P. S.; Uddin, W.; Srivastava, R. K. (1987)
    UBV photometric observations are important and can provide very interesting and valuable information on the brightness and colours of comets. In this letter we present the observed standard UBV magnitudes and U-B and B-V ...
  • Photographic observations of comet Halley (1982i) 
    Joshi, S. C.; Srivastava, J. B.; Kandpal, C. D.; Padalia, T. D.; Sanwal, B. B.; Chaubey, U. S.; Singh, M. (1987)
    Positions of Comet Halley have been measured from the photographic plates taken at Cassegrain focus the 104-cm telescope of Uttar Pradesh State Observatory.
  • On the ultraviolet fluxes of Be stars 
    Joshi, S. C.; Rautela, B. S. (1987)
    The ultraviolet fluxes of a sample of Be and normal B stars taken from ultraviolet bright-star spectrophotometric catalogue and its supplement have been compared with model atmosphere fluxes. An ultraviolet temperature has ...
  • Gravitational radiation and spiralling time of close binary system 
    Padalia, T. D. (1987)
    Power-output be gravitational radiation (Pв)and spiral time (τₒ) for individual systems of sixteen eclipsing binary stars have been evaluated, and a relation between Pв and τₒ obtained.
  • Brightness distribution in the coma of Comet Halley (1982i) 
    Joshi, S. C.; Sanwal, B. B. (1987)
    Photographic photometry on a photograph of Comet Halley taken on March 15, 1986, through a Schott GG 385 filter on Kodak 103a-O plate carried out. The average magnitude per square mm of the coma at various distance from ...
  • Photometric minima of BZ Eridani 
    Srivastava, R. K.; Uddin, W. (1985)
    The observations of the eclipsing binary BZ Eridani (BD-6°841) were initiated long back in 1928, but it was discovered as an Algol type eclipsing binary system be Hoffmeister (1934). Since its discovery it has remained ...
  • Rapid variation in Hα emission of γ Cassiopeiae 
    Joshi, S. C.; Srivastava, R. K.; Srivastava, J. B. (1987)
    The well known Be star γ Cassiopeiae has been an object of intense study through over a century. Apart form the major phases namely, Be, Be shell, and normal B star with time scales of decades, the star also shows rapid ...
  • RS CVn-binary RW Com: a possible three-body system 
    Srivastava, R. K. (1987)
    A first period study of the eclipsing RS CVn-binary RW Com is presented. A new period (p=0.ͩ 2373455) based on 223 minima is given. The O-C diagrams of RW Com have been presented for the first time. Types of ten minima ...

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