ar X iv : a st ro - p h / 03 05 53 6 v 1 2 8 M ay 2 00 3 Masses and orbital inclinations of planets in the PSR B 1257 + 12 system

ar X iv : a st ro - p h / 03 10 75 0 v 1 2 7 O ct 2 00 3 Long term stability and dynamical environment of the PSR 1257 + 12 planetary system

We study the long-term dynamics of the PSR 1257+12 planetary system. Using the recently determined accurate initial condition by Konacki & Wolszczan (2003) who derived the orbital inclinations and the absolute masses of the planets, we investigate the system stability by long-term, 1 Gyr direct integrations. No secular changes of the semi-major axes, eccentricities and inclinations appear durin...

ar X iv : a st ro - p h / 03 05 01 3 v 1 1 M ay 2 00 3 The issue of aliasing in PSR B 0943 + 10 II Signal processing arguments

Deshpande & Rankin (1999, 2001) claim that the frequency of the very narrow feature, in the spectrum of radio flux variations of PSR B0943+10, is an alias of its actual value. They also claim to have detected an amplitude modulation on the above phase modulation. This paper argues that both these claims are unjustified.

ar X iv : a st ro - p h / 96 05 14 1 v 1 2 3 M ay 1 99 6 Orbital Parameters of the PSR B 1620 − 26 Triple System

Previous timing data for PSR B1620−26 were consistent with a second companion mass m 2 anywhere in the range ∼ 10 −3 − 1 M ⊙ , i.e., from a Jupiter-type planet to a star. We present the latest timing parameters for the system, including a significant change in the projected semi-major axis of the inner binary, a marginal detection of the fourth time derivative of the pulse frequency, and the pu...

ar X iv : a st ro - p h / 04 05 34 4 v 1 1 8 M ay 2 00 4 Mid - and Far - Infrared ISO Limits on Dust Disks around Millisecond Pulsars

We report 60 and 90 µm observations of 7 millisecond pulsars with ISO. The pulsar PSR B1257+12 is orbited by three planets, and other millisecond pulsars may be orbited by dust disks that represent planets that failed to form or their residue. We do not detect any infrared emission from the 7 pulsars in our sample, and typical upper limits are 100 mJy. Using a simple model, we constrain the typ...

ar X iv : a st ro - p h / 06 05 06 7 v 1 2 M ay 2 00 6 Sensitivity and pointing accuracy of the NEMO km 3 telescope