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Astron. Astrophys. 331, 535-540 (1998)

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3. Results and discussion

In Figs. 2-5 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 [FORMULA] and [FORMULA] demonstrate the accuracy of the statistical computations (curves were not smoothed).


[FIGURE] 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. [FORMULA]

[FIGURE] 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. [FORMULA]

[FIGURE] 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. [FORMULA]

[FIGURE] 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. [FORMULA]

Fig. 6 shows the luminosity in the Galactic plane as a function of radius for a characteristic kick velocity [FORMULA] = 200 km/s. The figure is not completely symmetric. The right hand part corresponds to the azimutal angles 0-180 degrees, the left to - 180-360 degrees. The differences between the left and the right parts of the curve give an indication of the accuracy of our computations.


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

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© European Southern Observatory (ESO) 1998

Online publication: February 16, 1998
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