Volume 5, Issue 2
June 1984, pages 99-185
pp 99-110 June 1984
Radiation from the Magellanic Clouds is discussed from the point of view of near future possibilities in observational γ-ray astronomy. The γ-ray fluxes expected according to the metagalactic and galactic theories of the origin of cosmic rays are compared. It is shown that the strongest test of the metagalactic hypothesis will be provided by a determination of the ratio of γ-ray fluxes from SMC and LMC. The γ-ray luminosity of a typical young supernova remnant that can generate sufficient antiprotons is estimated. It is shown that such remnants must have a short phase during which they are very powerful γ-ray emitters.
pp 111-130 June 1984
The potential of high-resolution spatial interferometry for detailed mapping and precision astrometry in the mid-infrared region, somewhat analogous to interferometry now done in the microwave region, is discussed from an instrumental point of view. Some results from a prototype system and from tests of atmospheric properties are given. The design of a more advanced two-telescope system now under construction is outlined. This involves movable telescopes of 1.65 m aperture and of high precision, using heterodyne detection of infrared in the 10 Μm atmospheric window.
pp 131-138 June 1984
The main bands of the Schüler system of ND4 and NH4 have been observed at high resolution. On the basis of these spectra, Watson, in a separate paper, has analysed the ND4 main band showing that it represents a2F2→2 A1 transition of a tetrahedral molecule. The observed wavenumber data for both ND4 and NH4 are presented; the latter have not yet been analysed. Isotopic bands for15ND4,14ND3H,14ND2H2,14NDH3 have also been obtained and as previously pointed out confirm the assumed carrier of the spectrum. The much weaker bands accompanying the main Schüler band on the short and long wavelength sides are photographed at medium resolution. The interpretation of these bands in terms of the vibrational levels of upper and lower states is briefly discussed.
pp 139-148 June 1984
A 4-km synthesis radio telescope has recently been commissioned at Ootacamund, India for operation at 327 MHz. It consists of the Ooty Radio Telescope (530 m × 30 m) and 7 small antennas which are distributed over an area of about 4 km × 2 km. It has a coverage of about ± 40‡ in declination δ. The beam-width is about 40 arcsec × 90 arcsec at δ = 0‡ and about 40 arcsec × 50 arcsec at δ = 40‡. The sensitivity attained for a 5:1 signal-to-noise ratio is about 15 m Jy after a 10-hour integration.
The observational programmes undertaken and some of the results obtained recently are summarized. The radio halo around the edge-on spiral NGC 4631 is found to have a larger scale-height at 327 MHz than is known at higher frequencies. Mapping of interesting radio galaxies at 327 MHz is being carried out; preliminary results for 0511-305 (∼2 Mpc) and 1333-337 (∼750 kpc) are summarized. The very-steep-spectrum radio source in the Abell cluster A85 is found to be resolved; since it has no obvious optical counterpart, it is conceivable that it is a remnant of past activity of a galaxy that has drifted away in about 109 years.
pp 149-158 June 1984
During the eclipse of 1980 February 16 we photographed the solar corona at an effective wavelength of 6300 å. Using a quadruple camera we also obtained the coronal pictures in polarized light for four Polaroid orientations. We have used these observations to derive the coronal brightness and polarization and from these the electron densities in the corona out to a distance of about 2.5 R⊙ from the centre of the disc. The coronal brightness matches well with that of the corona of 1958 October 12.
pp 159-168 June 1984
Photoelectric observations of the RS CVn type non-eclipsing binary UX Arietis obtained at Nizamiah Observatory during the observing seasons of 1975–76, 1981–82 and 1982–83 are presented. The light curve of UX Ari showed a distortion wave with an amplitude inV varying from 0.02 mag during 1975–76 to 0.15 mag during 1982–83. An analysis of the available data shows that the light maximum is almost constant. It is also evident that the light-curve minimum decreases as the wave amplitude increases. The constant light at maximum,V = 6.51 ± 0.03 indicates the unspotted photospheric brightness. It is also suggested that the variation in meanV brightness is mainly due to spot activity and not due to intrinsic variation.
pp 169-180 June 1984
The effects of partial frequency redistribution on the formation of spectral lines have been studied. We considered the angle-averaged RII, RIII andRv types of redistribution with isotropic phase function, Transfer equation with plane-parallel geometry is solved in isothermal atmospheres. For an atmosphere with constant thermal sources, the frequency-dependent source function SL (Rv) lies below SL (RIII) but above SL(RIII) in the line wings.
pp 181-185 June 1984
Photoelectric radial-velocity measurements confirm and refine the preliminary orbit derived for HR 4668 by Christie on the basis of eight Lick spectrograms taken more than 50 years ago.
Volume 40 | Issue 2
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