Astronomy

Nuclear pasta

Print edition : July 12, 2013

Artistic representation of a neutron star. The layer of “nuclear pasta” would be located in the innermost crust, near the core.

A STUDY led by the University of Alicante has detected what may be the first observational evidence of the existence of a new exotic phase of matter in the inner crust of neutron stars.



The latest issue of Nature Physics shows the results of a research that addressed one of the unknowns in the field of X-ray pulsars, the existence of a limit higher than 12 seconds in the rotation periods of isolated neutron stars. This limit is actually due to the existence of new exotic phases of matter.



Pulsars are neutron stars (ultracompact and strongly magnetised stars) in rotation, which emit electromagnetic radiation with amazing precision in their periodicity.



“This may be the first observational evidence of existence of the phase of nuclear ‘pasta’ inside neutron stars, which may allow that future missions of X-ray observatories can be used to define aspects of how nuclear interaction works, which is not yet entirely clear,” says José A. Pons of the University of Alicante, who led the work.



Nuclear pasta, named for its resemblance to the Italian pasta, occurs when the combination of nuclear and electromagnetic forces, at densities close to the atomic nuclei, favours the ordering of the nucleons (protons and neutrons) in non-spherical shapes, as sheets or filaments (lasagna or spaghetti). It is this nuclear ‘pasta’ that seems to limit the period of rotation of pulsars.



Daniele Viganò, a doctoral student at the University of Alicante, notes: “The pulsars are born spinning very quickly, more than 100 times per second. However, their strong magnetic fields slow them down during their life, which increases the rotation period. Meanwhile, the inner crust corrodes the star’s magnetic field and when it becomes weak, it is unable to further slow down the rotation of the star and limits it to a period of about 10-12 seconds.”



Historically, radio pulsars (those detected in radio waves) were known to have a limit spin period with no theoretical explanation. Normally, this limit is thought to be a simple observational effect: those with slower rotation are less bright in radio and cannot be observed. Space missions in the past decade have identified a growing number of isolated X-ray pulsars, and none of them has a rotation period longer than 12 seconds, but there was no theoretical explanation for this phenomenon.







R. Ramachandran

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