V. Radhakrishnan

Vela, its X-ray nebula, and the polarization of pulsar radiation

The recent identification of the perpendicular mode of radio polarization as the primary one in the Vela pulsar by Lai et al. (2001) is interpreted in terms of the maser mechanism proposed by Luo & Melrose (1995). We suggest that such a mechanism may also be operative for the parallel mode which opens up the possibility of accounting for all types of polarization observed in pulsars. We propose an alternative interpretation of the arcs in the nebular X-radiation observed by Pavlov et al. (2000) and Helfand et al. (2001) with the Chandra Observatory, and interpreted by the latter as an equatorial wind. We interpret the arcs as traces of the particle beams from the two magnetic poles at the shock front. We also propose that the alignment with the rotation axis of the jet-like feature bisecting the arcs is an effect of projection on the sky plane and that there is no physical jet along the axis of rotation.

Pulsar observations at 34.5 MHz using the Gauribidanur Telescope. I

The behaviour of pulsars at low radio-frequencies (below ≈ 50 MHz) remains poorly understood mainly due to very limited observational data on pulsars at these frequencies. We report here our measurements of pulse profiles at 34.5 MHz of 8 pulsars using the Gauribidanur Radio Telescope. None of the 8 pulsars show any significant interpulse emission at this frequency which conflicts with an earlier claim from 25 MHz observations. With the exception of one pulsar (PSR 0943 + 10) all the observed pulsars show turnovers at frequencies above 35 MHz in their spectra. We also report our attempts to study the short and long term variations in the pulsar signals at this low frequency.

Further Evidence for Collimated Particle Beams from Pulsars and Precession

We follow up on our (Radhakrishnan & Deshpande) radically different interpretation of the observed structures and morphologies in the X-ray observations of the nebulae around young pulsars (PWNe). In our general model for PWNe (Radhakrishnan & Deshpande), originally motivated by the Chandra observations of the Vela X-ray nebula, the bright arcs, the jetlike feature, and the diffuse components in such nebulae can be explained together in detail, wherein the arcs are understood as traces of the particle beams from the two magnetic poles at the shock front. We consider this as important evidence for collimated particle beams from pulsars magnetic poles. In this paper we discuss the variability in the features in the Vela X-ray nebula observed by Pavlov and coworkers and assess the relevance and implication of our model to the observations on the Crab and other remnants. Our basic picture after incorporating the signatures of free precession of the central compact object can readily account for the variability and significant asymmetries, including the bent jetlike features, in the observed morphologies. The implications of these findings are discussed.

VLA observations of 1E 1740.7-2942 - A search for radio recombination lines of positronium

We have searched for the Ps87α (ν rest =4911.105 MHz) recombination line of positronium at the position of the Einstein X-ray source 1E 1740.7-2942 which has been identified as a strong source of time-variable annihilation line radiation. No line was detected with a 3 σ upper limit or 330 μJy for a line width or 23.5 MHz, the expected width if the temperature of the annihilation region is ∼7×10 4 K. A continuum image of the field made from the same data shows, within the 90% confidence error circle of the X-ray source, a weak radio source with a core and lobe structure similar to extragalactic double radio sources

On selection effects in pulsar searches

Selection effects are a major source of error in statistical studies of pulsar data since the observed sample is a biased subset of the full galactic pulsar population. It is important to identify all selection effects and make a reasonable model before attempting to determine pulsar properties. Here we discuss a hitherto neglected selection effect which is a function of the periodP of the pulsar. We find that short-P pulsars are more difficult to detect, particularly if their dispersion measures are high. We also discuss a declination-dependent selection effect in the II Molonglo Survey (II MS), and find some evidence for the existence of both selection effects in the pulsar data from this survey. We discuss the implications of these additional selection effects for the recently proposed ‘injection’ of pulsars whereby pulsars seem to switch on only at longerP. Using the II MS data we calculate that the observability of pulsars withP between 0.0 s and 0.5 s is about 18 per cent less with the new selection effects than hitherto believed; the mean correction is 6 per cent forP between 0.5 s and 1.0 s. We conclude that injection is not qualitatively affected by these corrections.

Pulsar Observations at Decametric Wavelengths using a Swept-frequency Dedisperser

In this paper, we describe pulsar observations at decametric wavelengths using the Gauribidanur Radio Telescope made subsequent to our earlier measurements (Deshpande & Radhakrishnan 1992). To improve the time-resolution in our measurements of pulse profiles, we have used the ‘swept-frequency dedispersion’ method with some modifications to suit its application at such low radio frequencies. We also present a new scheme that simplifies the calibration of the receiver gain characteristics. We present average profiles on four pulsars from these improved measurements at 34.5 MHz.

The structure of integrated pulse profiles

We offer two possible explanations to account for the characteristics of integrated pulse profiles, in particular their degree of complexity, their variation from pulsar to pulsar, their stability, and the tendency of complex profiles to be associated with older pulsars. It is proposed that the pulse structure could be a reflection of surface irregularities at the polar caps, and it is shown how the surface relief can affect the number of positrons released into the magnetosphere which are subsequently responsible for the observed radio radiation. The electrons produced in the vacuum break-down in the gap carry enough energy to allow creating such a surface relief in ~ 10 years, and one way in which this could be achieved is discussed. Alternatively, the presence of multipole components in the magnetic fields of older pulsars could lead to significant variations in the curvature of the field lines across the gap, and hence to structure in the integrated pulse profiles. An assessment of the two hypotheses from observed pulse profiles seems to favour the polar cap relief picture.

Source-noise in radio synthesis images

Open Access. Radio interferometry: Theory, techniques, and applications; Proceedings of the 131st IAU Colloquium, Socorro, NM, Oct. 8-12, 1990.