The evolution of the \vec{z} distribution of normal neutron stars in the Galaxy

Details The evolution of the \vec{z} distribution of normal neutron stars in the Galaxy The evolution of the \vec{z} distribution of normal neutron stars in the Galaxy

Aug 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010an....331..817w&link_type=abstract

Astronomische Nachrichten, Vol.331, Issue 8, p.817

Statistics

Galaxies: Kinematics And Dynamics, Galaxy: Disk, Pulsars: General, Stars: Evolution, Stars: Neutron, Stars: Statistics

Scientific paper

Under the two initial 1-D one parameter velocity distribution forms (one is normal, the other is exponential), the z direction scale height evolution of normal neutron stars in the Galaxy is studied by numerical simulation. We do statistics for the cases at different time segments, also do statistics for the cumulative cases made of each time segment. The results show in the cumulative cases the evolution curves of the scale heights are smoother than in the each time segment, i.e., the cumulation improve the signal-to-noise ratio. Certainly the evolution cases are different at different Galactic disk locations, which also have very large difference from the average cases in the whole disk. In the initial stages of z evolution of normal neutron stars, after the beginning transient states, the cumulative scale heights increase linearly with time, and the cumulative scale height increasing rates have linear relationship with the initial velocity distribution parameters, which have larger fluctuation in the vicinity of the Sun than in the whole disk. We utilize the linear relationship of the cumulative scale height increasing rates vs. the initial velocity distribution parameters in the vicinity of the Sun to make comparison with the observation near the Sun. The results show if there is no magnetic decay, then the deserved initial velocity parameters are obvious lower than the present well known results from some authors; whereas if introducing magnetic decay, for the 1-D normal case we can make consistence among concerning results using magnetic decay time values which are supported by some authors, while for the 1-D exponential case the results show the lackness of young pulsar samples in the larger z in the vicinity of the Sun.

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