Aryabhatta Research Institute of Observational Sciences: Recent submissions

  • Period-mass ratio relations for eclipsing binaries with periods not exceeding 5 days 
    Sinvhal, S. D.; Srivastava, J. B. (1978)
    The dependence of mass ration of eclipsing binary system on period has been studied. It has been found that semi-detached systems obey the relation m₂/m₁ = 0.64 - 0.079P or m₂/m₁ = 0.29 - 0.028P depending upon whether the ...
  • Study of the Delta-Scuti star HR 1170 
    Gupta, S. K. (1977)
    The light and colour curves of the δ-Scuti star HR 1170 are presented. The absolute and bolometric magnitudes are derived and the position of the star on the colour-colour diagram is also shown. The primary and beat periods ...
  • Spectrophotometry of comet West (1975n) after the perihelion passage 
    Chaubey, U. S. (1978)
    In the wavelength range 350to 650 nm, the flux distribution of comet West (1975n) is presented for various dates following perihelion passage. The variations with heliocentric distances, in the flux of the emission features ...
  • The photoelectric elements of AS Camelopardalis 
    Padalia, T. D.; Srivastava, R. K. (1975)
    Improved geometrical elements of the system AS Cam have been obtained and the colour of the system has been discussed. The absolute dimensions have also been obtained on the basis of the spectroscopic elements given by ...
  • Photoelectric elements of the eclipsing binary XY Ceti 
    Srivastava, R. K.; Padalia, T. D. (1975)
    The absolute elements of the system XY Ceti have been obtained on the basis of the spectroscopic elements given by Popper (1971) and the photoelectric elements derived by us. The colours of the components have been obtained. ...
  • Study of the extremely young open cluster NGC 6530 
    Sagar, R.; Joshi, U. C. (1978)
    Photoelectric magnitudes and colours in the UBV system have been determined for 101 stars in the field of NGC 6530. The interstellar reddening across the cluster varies from 0.25 to 0.48 mag, with an average value of 0.35 ...
  • Effective temperatures, radii and bolometric magnitudes of Ap and Am stars 
    Babu, G. S. D.; Rautela, B. S. (1978)
    The effective temperatures, radii and bolometric magnitudes of Ap, Am and normal A stars have been estimated from their energy distribution curves between 478 nm and 680 nm. All the Am stars and one Ap star (i.e. β CrB) ...
  • Empirical P-L-C relations for Delta Scuti stars 
    Gupta, S. K. (1978)
    Separate P-L-C relations have been empirically derived by sampling the δ Scuti stars according to their pulsation modes. The results based on these relations have been compared with those estimated from the model based ...
  • Isotopic lines of SiO in sunspots 
    Pande, M. C.; Joshi, G. C. (1978)
    As the isotopic shift for the vibration rotation band is generally much larger than the isotopic shift for the corresponding electronic transitions and thus facilitating separation of isotopic lines, the vibration rotation ...
  • Photoelctric photometry of the eclipsing binary EE Aqr 
    Padalia, T. D. (1979)
    The system EE Aqr has been observed in UBV colours. A consistent set of orbital elements and a slightly improved period of 0.ᵈ5089954 have been obtained. The eclipse is partial and varability is of β Lyrae-type. The colour ...
  • On the presence of SH in the sunspot spectrum 
    Joshi, G. C.; Pande, M. C. (1979)
    The expected equivalent widths of individual rotational lines of the most intense Q₂ branch of the 0-0 band of the A²∑-X² пi, system of S³²H and S³⁴ H have been calculated in the umbral spectrum for five disk positions ...
  • On the O₂ Schumann-Runge band system in sunspots 
    Joshi, G. C.; Punetha, L. M.; Pande, M. C. (1979)
    The visibility in the umbral ultraviolet spectrum of the O₂ Schumann-Runge absorption band system has been explored. It is found that the band system may be visible in high dispersion sunspot spectrum.
  • Emissions from the head of comet Bradfield (1978c) 
    Chaubey, U. S. (1979)
    The flux distribution in the head of comet Bradfield (1978c) during the pre-perihelion period has been obtained in the wavelength range 400-640 nm. The emission fluxes at 474 nm, 516 nm, 564 nm and 589 nm are reported. By ...
  • ARIES Academic Report 2010-2011 
    Unknown author (ARIES, 2011-08)
  • Intensity oscillations across the Ca II K line 
    Punetha, L. N (1974)
    Intensities at various wavelengths in the Ca II K line over a 10 minute duration time series spectra have been examined for oscillations. Three components have been observed:1) large period, ≥ 1000 second, due to the slowly ...
  • Equivalent widths of molecular lines in eta aquilae 
    Pande, M. C.; Joshi, G. C.; Bondal, K. R. (1974)
    Using dawe's model atmospheres the equivalent widths of R1 line belonging to the 0-0 band of the electronic transition B2∑+ →X2∑+ of the CN molecule were calculated for various phases of light variation in ŋAql. the ...
  • Absolute energy distribution og two δ scuti variable 
    Joshi, S. C.; Rautela, B. S. (1973)
    The absolute energy distribution of two δ sct stars β cas (HR 21)and υ UMa (HR 3888) have been given.by matching these with model atmospheres there effective temperatures,gravities,radii and masses have been estimated.
  • Energy distribution in early K-star 
    Chaturvedi, J. P.; Sinvhal, S. D. (1974)
    The spectral distribution of energy for 21 early K-star in the wavelength reason 450 nm to 750 nm at a definition of 5 nm have been obtained. A two dimensional photometric spectral classification index- system for these ...
  • Three- colour photometry of TW CAS 
    Kandpal, C. D. (1975)
    Photoelectric elements of the system TW Cas have been determined in U,B and V filters. A refined period of 1ᵈ.428 324 77 has been given though no change in period is noticed. Spectroscopic elements given by struve have ...
  • Three- colour photometry of the eclipsing binary EI cephei 
    Padalia, T. D.; Srivastava, R. K. (1975)
    The photoelectric elements of the system EI cephei have been determined U,B,V colours. The absolute dimensions have been determined and some evolutionary aspects have been discussed.A modified period of 8ᵈ.439334 has been ...

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