A 24 HR GLOBAL CAMPAIGN TO ASSESS PRECISION TIMING OF THE MILLISECOND PULSAR J1713+0747

The traditional template-matching method used to calculate pulse times of arrival (ToAs) may not function effectively on these broad-band data due to a variety of effects such

In this section, the complex variation of the light curve of J1643
1224 observed at 1.28 and 1.41 GHz is modeled first with a single ionized cloud, and second with three clouds

We test three aspects of SEP using observed change rates in the orbital period and eccentricity of binary pulsar J1713 +0747: (1) the gravitational constant’s constancy as part

Name Time span Observing Galactic Period Ecliptic DM Log Observations sites coo. The table reports the source name, the covered time span, the number of observing sites that have

We report our findings as follows: in Section 2 , we discuss the perturbations to pulsar TOAs caused by asteroid belts; in Section 3 , we discuss the formation of asteroidal

Number density distribution (lower panel) of pulses with respect to their relative peak flux densities and phase of pulse peak, compared with the integrated profile (upper panel)..

Picard, Non linear filtering of one-dimensional diffusions in the case of a high signal to noise ratio, Siam J. Picard, Filtrage de diffusions vectorielles faiblement

The columns give the pulsar name, the DM, the distance based on the NE2001 electron density model D NE2001 (Cordes & Lazio 2002), the distance based on the M2 and M3 models, D