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| Paper: |
Statistical Properties of Magnetic Fields and Fluxes of Neutron Stars |
| Volume: |
518, Physics of Magnetic Stars |
| Page: |
108 |
| Authors: |
Kholtygin, A.; Makarenko, E. I. |
| Abstract: |
Young neutron stars (NS) of our Galaxy in the evolutionary stage before the death line
can be divided into two groups: normal pulsars and magnetars with
magnetic fields log(B)∼11–13 and log(B)∼14–15 respectively. The average magnetic fluxes (G cm2) of these
groups are overline{log(Φ)} = 23.9 for normal pulsars and overline{log(Φ)} = 26.8 for magnetars. Massive OB
stars, precursors of neutron stars, also can be divided into two groups: magnetic stars with average magnetic fields
from several hundreds gauss to tens of kilogauss and non-magnetic or weakly magnetic stars, whose magnetic fields can not yet be measured
accurately. The average magnetic flux of weakly magnetic stars can be estimated using recent measurements of the magnetic
fields of selected A and B stars: Vega, Sirius A, and others. For such stars mean magnetic flux overline{log(Φ)}= 23.8
is close to the corresponding value for normal pulsars, whereas the average magnetic flux of magnetic OB stars is similar to
that for magnetars. For this reason we assume that normal pulsars are descendants of weakly magnetic stars, and magnetars are
progenitors of magnetic OB stars. The fraction of magnetars among NSs is only 1%, in contrast to the 7% fraction of magnetic stars
among OB stars. The relatively small fraction of magnetars among neutron stars can be explained by their short lifetime. |
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