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• W3204189870 abstract "We simulate motions of 2 10 5 pulsars in our Galaxy with Monte- Carlo method and try to understand the evolution of pulsar height distribution. Within about 8 Myr, pulsar height distribution can be tted by a Gaussian function with a scale height linearly increasing with time. An extra exponential function is necessary to be added to the Gaussian function to t the height distribution afterwards. The Gaussian scale height increases linearly until about 40 Myr. After about 200 Myr, the height distribution is stabilized. Based on the simulation results, we obtain the initial 1D velocity dispersion of 80 km s 1 for millisecond pulsars. Pulsar motions have been involved in population synthesis (e.g. Bhattacharya et al. 1992), but not explicitly claried. Some authors tried to deduce scale height evolution theoretically, but they had to assume a simple Galactic potential (e.g. Arnaud & Rothenug 1981) or a simplied height evolution (Narayan & Ostriker 1990). In this contribution, we explore the height evolution with Monte-Carlo simulation. The initial height distribution of pulsars is assumed to be a Gaussian with a scale height of 60 pc as that of the progenitors i.e. OB stars (Ma z-Ap ell aniz 2001). The radius distribution is assumed to follow a Gamma function (Paczy nski 1990). The nal results are insensitive to the form of initial height or radius distribution. Initial velocity is the vectorial sum of Galactic rotation velocity and kick velocity from asymmetric supernovae explosions. We assumed the kick velocities follow a Maxwellian distribution, with trial 1D velocity dispersion k =100, 200, 300 and 400 km s 1 , respectively. After comparing all the potentials available, we used the one given by Paczy nski (1990) which could reproduce the Galactic rotation curve and the local volume density near the Sun better than others. Provided these initial conditions described above, we solved the Newtonian kinetic equations using 4th order Runge-Kutta method with an adaptive step size (Press et al. 1992), then tracked all the pulsars from 0 Myr to 500 Myr. The scale heights are shown in Figure 1. Within about 8 Myr, the distribution can be tted very well by a Gaussian function with a scale height hg increasing linearly with time as hg h0 + kt. As time goes, a peak appears near the Galactic plane more and more prominently, so the distribution has to be tted by a Gaussian function plus an exponential function with a scale height he. The scale height hg keeps linear increase until about 40 Myr. After about 200 Myr, both hg and he gets stabilized. Now we try to understand the distribution of available pulsars using the simulation results. Because the height distribution is stabilized after about 200 Myr, the birth rate, if does not vary much with time, has no eects on the nal distribution. We can compare height distribution of our simulated pulsars with that of observed MSPs directly. The K-S test was employed to check the consistency of the distribution of known MSPs and the distribution from simulation with initial 1D velocity dispersion from 30 km s 1 to 180 km s 1 . Finally, we" @default.
• W3204189870 created "2021-10-11" @default.
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• W3204189870 date "2003-02-01" @default.
• W3204189870 modified "2023-09-23" @default.
• W3204189870 title "Pulsar Motions in our Galaxy" @default.
• W3204189870 hasPublicationYear "2003" @default.
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