Address for correspondence: Krasin str. 19, ap. 81, Moscow 123056, Russia.

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For other recent images of S 147 see http://www.skyfactory.org/simeis147/simeis147.htm

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...2003)

Another possible way to reduce the age of the pulsar is to assume that the pulsar's magnetic field grows exponentially with a characteristic time-scale of $\sim$ $4\tau /(n-\tilde{n} ) ~ \simeq 2$ $\times$ 10⁴ yr, where n=3, $\tilde{n} = \ddot{\nu} \nu /{\dot{\nu}} ^2$ , and $\nu, \dot{\nu}$ and $\ddot{\nu}$ are, respectively, the pulsar spin frequency and its two first time derivatives (measured by Kramer et al. 2003).

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...2002)

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...1998)

For $\phi =0{\hbox{$^\circ$ }}$ and $0{\hbox{$^\circ$ }} \leq \theta \leq 180{\hbox{$^\circ$ }}$ , the kick vector lies in the orbital plane and points to the half-sphere occupied by the old NS.

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...a

Vlemmings et al. (2004) draw an erroneous conclusion that in a wide binary disrupted after the second (asymmetric) SN explosion the old NS could be accelerated to a velocity $\sim$ w, while the second-born NS to a velocity several times exceeding w.

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... observations

See, http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3table.pl

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... Catalog

http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc/

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... PIMMS

http://heasarc.gsfc.nasa.gov/Tools/w3pimms.html

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