2025ApJ...980..214R

In this paper, we show the estimation of the emission altitude of pulsars PSRs B0329+54, B0450-18, B2045-16, J1909+0007, and J0337+1715 for both core and conal components at multiple radio bands by implementing a relativistic phase-shift method, which is constrained based on the plethora of standard radio emission geometry. Using the information of pulse longitudes for each component, coupled with a dipolar field geometry, we obtain a rough estimation of the height and transverse location of the emitting cones for these pulsars, i.e., footpoint location of the pulse edge, normalized with the last open magnetic field line constant. We also analyzed the profile of a well-known millisecond pulsar J0337+1715 at 1250 MHz, which has an asymmetric core-cone structure for both the main pulse and interpulse. This is the first time such a case has been analyzed to probe emission height by implementing the relativistic phase-shift method. We discuss the implications of our findings in the context of the pulsar's emission geometry to reach a consensus on the existing emission mechanism of pulsars.