Research Papers: Recent submissions

  • Some infrared photometric characteristics of Be stars 
    Goraya, P. S. (1985)
    A photometric study of a large sample of Be stars is reported. Infrared homogeneous observational data in the JHKL system are used to derive some photometric characteristics of Be stars, as a class. New infrared observations ...
  • Spectrophotometric study of Be stars 
    Goraya, P. S. (1985)
    A large sample of Be stars has been studied spectrophotometrically in the visible region. The continuum energy distribution data for 23 Be stars included in the list of Harmanec et al. (1983) are presented and discussed ...
  • UBV photometry of DX Aquarii 
    Srivastava, R. K.; Sinha, B. K. (1985)
    U, B, V photometry of the Eclipsing binary system DX Aqr has been presented for the first time. The period of the system comes out to be nearly half the period given by Strohmeier (1966) and a value of 0ͩ.472502 has been ...
  • Time delay between H-alpha and soft x-ray emissions during solar flares 
    Verma, V. K.; Pande, M. C. (1985)
    A statistical analysis of time delay between H-alpha and soft x-ray (SXR) emissions at onset and peak respectively during solar flares is presented. We find that at the onset of flares SXR emission starts simultaneously ...
  • Probable additional swan band lines in the solar spectrum 
    Sinha, K.; Mehrotra, M. (1985)
    Several unidentified spectral features in the solar spectrum are listed by Moore et al. (1996). They are traceable in the atlas by Delbouille et al. (1973). We attempt to identify some of these features in the region ...
  • On the dependence of solar flare occurrence on sunspot polarity 
    Verma, V. K.; Shelke, R. N. (1985)
    The possibility of predicting flare occurence on the sun has been examined. It is noticed that the p-polarity dominant spot groups. This high productivity of p-polarity dominant spot groups has been interpreted in terms ...
  • Continuum energy distribution of Be stars 
    Singh, M. (1985)
    The continuum energy distributions of four Be stars - namely, HR 7708, HR 7807, HR 7927, and HR 8171 alongwith two normal B stars HR 7426 and HR 7613 are presented in the wavelength region λλ3200-7800 Å. By a comparison ...
  • Time delay between Hα and hard X-ray emissions during implusive solar flares 
    Verma, V. K.; Pande, M. C. (1985)
    This investigation shows that statistically there are significant time delay between Hα and hard X-ray (HXR) emissions during solar flares; most impulsive flares produce HXR emissions up to ~1 min before and up to 2 min ...
  • Flare like activity of AR Lacertae in 1982 
    Srivastava, R. K. (1985)
    Investigations of the eclipsing binary system AR Lacertae have been reported earlier by author (cf. Srivastava, 1981; 1983s; 1983b; 1984; Goraya and Srivastava, 1984). AR Lac is a well known radio flaring sources. Some ...
  • On the solar surge association with microwave and hard X-ray emission bursts 
    Verma, V. K. (1985)
    It is found that 20% solar surges are associated with microwave bursts (2800-15000 MHz) and also that solar surges are not associated with hard X-ray bursts (17-40 KeV).
  • Some observations of DX Aquarii 
    Srivastava, R. K. (1985)
    U, B, V photoelectric observations of the eclipsing binary system DX Aqr, secured in 1981, have been presented. Present results, when compared with earlier ones (cf. Srivastava and Sinha, 1985), suggest that the features ...
  • Hα line emission and infrared excess in Be Stars 
    Goraya, P. S.; Rautela, B. S. (1985)
    The Hα observations of a selected sample of bright Be stars are presented. The available infrared observations at K band (2.2 µm) of these stars have been used to find the infrared excess emission. The analysis of the ...
  • Continuum energy distribution and photometric behaviour of Π Aqr 
    Goraya, P. S. (1985)
    New observations of Π Aqr in the optical and infrared (IR) region are presented. The effective temperature of Π Aqr is derived by comparing observed and computed fluxes in the optical region. No near-ultraviolet excess was ...
  • Near-infrared/optical identification of five low-luminosity X-ray pulsators 
    Kaur, R.; Wijnands, R.; Paul, B.; Patruno, A.; Degenaar, N. (2010)
    We present the identification of the most likely near-infrared (NIR)/optical counterparts of five low-luminosity X-ray pulsators (AX J1700.1−4157, AX J1740.1−2847, AX J1749.2−2725, AXJ1820.5−1434 andAXJ1832.3−0840) which ...
  • X-ray emission characteristics of two Wolf–Rayet binaries: V444 Cyg and CD Cru 
    Bhatt, H.; Pandey, J. C.; Kumar, B.; Singh, K. P.; Sagar, R. (2010)
    Using data from observations made with XMM–Newton, we present an X-ray analysis of two Wolf–Rayet (WR) binaries: V444 Cyg and CD Cru. The X-ray light curves show the phase-locked variability in both binaries, where the ...
  • Photoelectric elements and revised spectral types of XX Cas 
    Srivastava, R. K. (1987)
    In this communication, photoelectric elements of the eclipsing binary system XX Cas in U, B and V filters and revised colour indices have been presented. In the absence of good photoelectric observations and complete set ...
  • On the primary minimum of eclipsing binary AY Cam 
    Srivastava, J. B.; Kandpal, C. D. (1987)
    The eclipsing binary AY Cam (= BV 363 = BD + 77° 0328) was discovered by Strohmeier and Knigge (1961). They assigned it a period of 1ͩ. 367485. The photographic light curve is of Algol type with no indication of secondary ...
  • Intrinsic light variations in the eclipsing binary RW Ceti 
    Padalia, T. D. (1987)
    Intrinsic light variations in B and V filters have been found on the three observed light curves of RW Ceti.
  • CU Eridani - a suspected variable 
    Srivastava, J. B.; Srivastava, R. K. (1987)
    Photometric observations of CU Eridani, recently classified as non-variable, indicate it to be a variable star.
  • Possible ring system of neptune 
    Pandey, A. K.; Mahra, H. S. (1987)
    A re-analysis of the observations of occultation of MKE 31 by Neptune on September 12, 1983(Pandey et al., 1984) shows that the possible ring system of Neptune extends from 64400 km to 64190 km in Neptune's plane.

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