Neutron star: Difference between revisions

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Recent work, however, suggests that a starquake would not release sufficient energy for a neutron star glitch; it has been suggested that glitches may instead be caused by transitions of vortices in the theoretical superfluid core of the neutron star from one metastable energy state to a lower one, thereby releasing energy that appears as an increase in the rotation rate.<ref>{{cite web |url=http://physicsworld.com/cws/article/print/1756 |date=1 January 1998 |title=Pulsars, glitches and superfluids |publisher=Physicsworld.com |first=M. Ali |last=Alpar |access-date=12 January 2009 |archive-date=6 December 2008 |archive-url=https://web.archive.org/web/20081206090618/http://physicsworld.com/cws/article/print/1756 |url-status=live }}</ref>
 
==="Anti-glitches"===
 
An "anti-glitch", a sudden small decrease in rotational speed, or spin down, of a neutron star has also been reported.<ref name="nature">{{cite journal |title=An anti-glitch in a magnetar |journal=Nature |doi=10.1038/nature12159 |year=2013 |first1=R. F. |last1=Archibald |first2=V. M. |last2=Kaspi |first3=C. Y. |last3=Ng |first4=K. N. |last4=Gourgouliatos |first5=D. |last5=Tsang |first6=P. |last6=Scholz |first7=A. P. |last7=Beardmore |first8=N. |last8=Gehrels |first9=J. A. |last9=Kennea |pages=591–593 |volume=497 |issue=7451 |hdl=10722/186148 |pmid=23719460 |arxiv=1305.6894 |bibcode=2013Natur.497..591A |s2cid=4382559 }}</ref> It occurred in the magnetar [[1E 2259+586]], that in one case produced an X-ray luminosity increase of a factor of 20, and a significant spin-down rate change. Current neutron star models do not predict this behavior. If the cause was internal, it suggests differential rotation of solid outer crust and the superfluid component of the magnetar's inner structure.<ref name="nature" />
 
==Population and distances==