Scintillation measurements of the millisecond pulsar PSR J0030+0451 and pulsar space velocities

Free access article

Issue		A&A Volume 368, Number 3, March IV 2001


Page(s)		1055 - 1062
Section		Formation, structure and evolution of stars
DOI		http://dx.doi.org/10.1051/0004-6361:20010074

A&A 368, 1055-1062 (2001)
DOI: 10.1051/0004-6361:20010074

Scintillation measurements of the millisecond pulsar PSR J0030+0451 and pulsar space velocities

L. Nicastro¹, F. Nigro², N. D'Amico², V. Lumiella³ and S. Johnston⁴

¹ Istituto di Fisica Cosmica con Applicazioni all'Informatica, CNR, Via U. La Malfa 153, 90146 Palermo, Italy
² Osservatorio Astronomico di Bologna, Via Ranzani 1, 40127 Bologna, Italy
³ Dipartimento di Astronomia, Università degli Studi di Bologna, Via Ranzani 1, 40127 Bologna, Italy
⁴ Research Centre for Theoretical Astrophysics, University of Sydney, NSW 2006, Australia

(Received 6 December 2000 / Accepted 12 January 2001 )

Abstract
Scintillation observations of the nearby single millisecond pulsar (MSP) PSR J0030+0451 were carried out with the Parkes 64 m radiotelescope at three different epochs in 1999. From analysis of the dynamic spectrum we obtained the amplitude of the electron density power spectrum $\log \overline{C_{\rm N}^2} \simeq -3.33$ and a scintillation velocity $V_{\rm iss} \la 15$ km s^-1. This result shows that the Shklovskii effect on the spin-down rate $\dot P$ is negligible. We also performed a correlation analysis between pulsar proper motions ( $V_{\rm pm}$ ) and scintillation velocities ( $V_{\rm iss}$ ) using updated measurements for a sample of 77 objects, 17 of which are MSPs. The full sample shows a correlation coefficient $r_{\rm s} \simeq 80\%$ at an extremely high significance level, while for the MSP sub-sample (excluding 2 outliers) we obtain $r_{\rm s} \simeq 90\%$ .

Key words: stars: kinematics -- pulsars: individual: PSR J0030+0451 -- ISM: general -- ISM: kinematics and dynamics -- ISM: structure -- radio continuum: stars

Offprint request: L. Nicastro, nicastro@ifcai.pa.cnr.it

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