Vela pulsar

In section I we consider the dynamics of rotation of a two-component neutron star and obtain the relaxation solutions for spin-down rate of the star. In section II we compare our solutions for the relaxation process with the observation data from the Vela pulsar. 

Next we compare Eq. (11) with an interpolation formula for the eight glitches of the Vela pulsar [16] ... 

Note that similar curves are obtained for the eight glitches of the Vela pulsar. As we see from Fig. 1, the behavior of AQ + AQ.S. is quite different in different parts of the relaxation region. The first part is the region of exponential relaxation with constants t and r2 and is located within the shell 9.533 < r < 9.61 km. The second part is the region of the exponential relaxation with t3 and linear relaxation, located within the shell 9.36 < r 5 9.533... 

Figure 1. The dependence of AO + AQ,S on the radius of the star for the first glitch of Vela pulsar.

Alignment between spin axis and spatial velocity for Crab and Vela pulsars (see for example Lai et al. 2001)... 

Pavlov, G. et al. (2001), The X-ray spectrum of the Vela pulsar resolved with the Chandra X-ray observatory , ApJ 552, L129. 

Figure 5. The limiting (gravitational) mass Mum, according to generalized definition given in the present work, is plotted as a function of the Bag constant. Solid (dashed) lines show the results for the GM3+Bag (GMl+Bag) model. In both cases we take a = 30 MeV/fm2. The values of some measured masses of compact stars in radio pulsars and in Vela X-l and Cygnus X-2 are also reported for comparison.

Table 2. Rates for the EGRET pulsars (forth column) and observation time (fifth column) to detect them with 5a with a proton rate R = 70 Hz for

A number of persistent, bright X-ray sources have been monitored over long periods during the GRANAT and EURECA missions [1,2]. The period development have been followed for the pulsars Vela X-1 [7], GX 301-2... 

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