activity
20012025
most citedUnderstanding the radio emission geometry of PSR B0329+54

165 citations · 306 across the 11 of their papers we have counts for

collaborators

11 papers

astro-ph.HE2025★ 5 cited

NGC 1851A: Revealing an ongoing three-body encounter in a dense globular cluster

A. Dutta, P. C. C. Freire, T. Gautam +16

PSR J05144002A is a binary millisecond pulsar located in the globular cluster NGC 1851. The pulsar has a spin period of 4.99 ms, an orbital period of 18.8 days, and is in a very…

astro-ph.HE2023

Single pulse polarization study of pulsars B0950+08 and B1642-03: micropulse properties and mixing of orthogonal modes

Shubham Singh, Yashwant Gupta, Kishalay De

We present the results of a high-time resolution polarization study of single pulses from pulsars B0950+08 and B1642-03. Single pulses from pulsar B0950+08 sometimes show isolated…

astro-ph.HE2018★ 6 cited

Discovery of a radio nebula around PSR J0855-4644

C. Maitra, S. Roy, F. Acero +1

We report the discovery of a diffuse radio emission around PSR J0855--4644 using an upgraded GMRT (uGMRT) observation at 1.35 GHz. The radio emission is spatially coincident with t…

astro-ph.GA2010★ 8 cited

Understanding the effects of geometry and rotation on pulsar intensity profiles

R. M. C. Thomas, Y. Gupta, R. T. Gangadhara

We have developed a method to compute the possible distribution of radio emission regions in a typical pulsar magnetosphere, taking into account the viewing geometry and rotational…

astro-ph.SR2009★ 36 cited

On the aberration-retardation effects in pulsars

K. Krzeszowski, D. Mitra, Y. Gupta +3

The magnetospheric locations of pulsar radio emission region are not well known. The actual form of the so--called radius--to--frequency mapping should be reflected in the aberrati…

astro-ph2007★ 15 cited

Results from multi-frequency observations of PSR B0826-34

B. Bhattacharyya, Y. Gupta, J. Gil

We report new results obtained from multi-frequency observations of PSR B0826-34 with the Giant Metrewave Radio Telescope (GMRT). (1) We find no evidence of weak emission during th…