A strong  correlation in radio pulsars with implications for torque variations

doi:10.1111/j.1745-3933.2006.00192.x

If you are seeing this message, you may be experiencing temporary network problems. Please wait a few minutes and refresh the page. If the problem persists, you may wish to report it to your local Network Manager.

It is also possible that your web browser is not configured or not able to display style sheets. In this case, although the visual presentation will be degraded, the site should continue to be functional. We recommend using the latest version of Microsoft or Mozilla web browser to help minimise these problems.

Systems Maintenance, Monday, 15th February 2010

Wiley InterScience

Monthly Notices of the Royal Astronomical Society: Letters

See Also:

Monthly Notices of the Royal Astronomical Society

Volume 370 Issue 1, Pages L76 - L79

Published Online: 23 Jun 2006

A Journal of the Royal Astronomical Society

Go to Society Site

< Previous Abstract | Next Abstract >

Save Article to My Profile Download Citation Request Permissions

Abstract | References | Full Text: HTML, PDF (Size: 111K) | Related Articles | Citation Tracking

A strong

correlation in radio pulsars with implications for torque variations

J. O. Urama ^1,2★† B. Link ^3★ and J. M. Weisberg ⁴

¹ Department of Physics & Astronomy, University of Nigeria, Nsukka, Nigeria ² Hartebeesthoek Radio Astronomy Observatory (HartRAO), PO Box 443, Krugersdorp 1740, South Africa ³ Department of Physics, Montana State University, Bozeman, MT 59717, USA ⁴ Department of Physics and Astronomy, Carleton College, 1 N. College Street, Northfield, MN 55057, USA

Correspondence to ^★ E-mail: johnson@hartrao.ac.za (JOU); link@physics.montana.edu (BL) †Presently on leave at the Department of Industrial Physics, Ebonyi State University, Abakaliki, Nigeria.

KEYWORDS

stars: neutron • pulsars: general

ABSTRACT

We present an analysis of the spin-down parameters for 131 radio pulsars for which has been well determined. These pulsars have characteristic ages ranging from 10³ to 10⁸ yr and spin periods in the range 0.4–30 s; nearly equal numbers of pulsars have as have . We find a strong correlation of with , independent of the sign of . We suggest that this trend can be accounted for by small, stochastic deviations in the spin-down torque that are directly proportional (in magnitude) to the spin-down torque.