Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003head....7.2013m&link_type=abstract
American Astronomical Society, HEAD meeting #7, #20.13; Bulletin of the American Astronomical Society, Vol. 35, p.635
Astronomy and Astrophysics
Astronomy
Scientific paper
The spin-down rate ( ˙ Ω ) of an isolated magnetar, canonically described by I ˙ Ω = - KΩ n, gives the time after birth for achieving Ω as τ sd ˜ Ω /(n-1) ˙ Ω only for n > 1. When pulsar wind carries off stellar spin angular momentum, n ˜ 3 and Ω /(n-1)˙ Ω ˜ the time since birth to a currently observed spin angular frequency Ω . However, when a magnetar with magnetic dipole field Bd ˜ 1015 G moves at high velocity (v > 107 cm s-1) through the ISM, a transition to ``propeller effect'' spin-down with n <= 1 may occur in less than 106 years. Then a measured Ω / (1-n) ˙ Ω becomes the time remaining before the stellar spin is quenched. We consider RX J1856.5-3754 as such a magnetar. This is consistent with observed thermal X-ray emission (featureless and nearly blackbody for one X-ray polarization mode and almost no emission in the orthogonal mode). We propose that this magnetar's spin period has already grown to >> 104 sec and compare this conjecture to predictions from a large number of different propeller effect spin-down models.
Mori Kaya
Ruderman Malvin A.
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