ar X iv : a st ro - p h / 02 06 16 6 v 1 1 1 Ju n 20 02 How fast could a proto - pulsar rotate ?

ar X iv : q ua nt - p h / 02 06 11 6 v 1 1 8 Ju n 20 02 Five Lectures On Dissipative Master Equations

ar X iv : a st ro - p h / 02 06 48 5 v 1 2 7 Ju n 20 02 Noise and the strong signal limit in radio astronomical measurement

Received ; accepted – 2 – ABSTRACT The random error of radioastronomical measurements is usually computed in the weak-signal limit, which assumes that the system temperature is sensibly the same on and off source, or with and without a spectral line. This assumption is often very poor. We give examples of common situations in which it is important to distinguish the system noise in signal-beari...

ar X iv : a st ro - p h / 06 02 25 5 v 1 1 1 Fe b 20 06 Proper Motion of the Crab Pulsar

It has been suggested that the Crab pulsar’s proper motion is well aligned with the symmetry axis of the pulsar wind nebula. We have re-visited this question, examining over 6 years of F547M WFPC2 chip 3 images to obtain a best-fit value of μ∗ = 14.9± 0.8mas/yr at PA 278 ◦ ± 3. At 26± 3 to the nebula axis, this substantially relaxes constraints on the birth kick of this pulsar. Such misalignmen...

ar X iv : h ep - p h / 02 06 27 0 v 1 2 6 Ju n 20 02 1 The charge asymmetry from Pomeron - Odderon interference in hard

ar X iv : a st ro - p h / 02 06 29 8 v 1 1 8 Ju n 20 02 KUNS - 1791 astro - ph / 0206298 Tracking K - essence

We derive a condition for converging a common evolutionary track (“tracking condition”) for k-essence (a scalar field dark energy with non-canonical kinetic terms). For the Lagrangian density V (φ)W (X) with X = φ̇/2, we find tracker solutions with wφ < wB exist if Γ ≡ V V/(V ) > 3/2. Here wφ(wB) is the equation-of-state of the scalar field (background radiation/matter). Our condition may be use...