Astron. Astrophys. 331, 535540 (1998)
3. Results and discussion
In Figs. 25 we show as a radial cut through the Galactic disk the
results for two characteristic values of the velocity distribution for
NS and BH. The scales for R and Z axes are different in
order to show clearly the structure in Z direction. Differences
between the luminosity distribution for and
demonstrate the accuracy of the statistical
computations (curves were not smoothed).

Fig. 2. The accretion luminosity distribution in the R Z plane for neutron stars for a characteristic kick velocity 200 km/s. The luminosity is in ergs per second per cubic parsec.


Fig. 3. The accretion luminosity distribution in the R Z plane for neutron stars for a characteristic kick velocity 400 km/s. The luminosity is in ergs per second per cubic parsec.


Fig. 4. The accretion luminosity distribution in the R Z plane for black holes for a characteristic kick velocity 200 km/s. The luminosity is in ergs per second per cubic parsec.


Fig. 5. The accretion luminosity distribution in the R Z plane for black holes for a characteristic kick velocity 400 km/s. The luminosity is in ergs per second per cubic parsec.

Fig. 6 shows the luminosity in the Galactic plane as a function of
radius for a characteristic kick velocity = 200
km/s. The figure is not completely symmetric. The right hand part
corresponds to the azimutal angles 0180 degrees, the left to 
180360 degrees. The differences between the left and the right parts
of the curve give an indication of the accuracy of our
computations.

Fig. 6. Slice at Z=+5 pc for NS for a characteristic kick velocity 200 km/s. . The accretion luminosity is in ergs per second per cubic parsec. The solid line is a smoothed curve.

© European Southern Observatory (ESO) 1998
Online publication: February 16, 1998
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