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A Natural Explanation for Magnetars
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In this article, the authors explore the possibility that a magnetar may owe its strong magnetic field to a magnetized core which, as indicated by certain equations of state, may form due to phase transitions at high density mediated by strong interaction within a suffi ciently massive neutron star.Abstract:
Neutron stars possess some of the strongest magnetic fields k nown in the universe. The surface magnetic fields of radio pulsars are estimated to be in the range 10 8 to 10 13 Gauss, with 10 12 Gauss being the typical value. Magnetars, a class of neutron stars with even stronger magnetic fields, ∼ 10 15 Gauss, are believed to be “magnetically powered” stars, deriving most of their radiative luminosity at the cost of their magnetic fields. The origin of the strong magnetic fields of neutron stars, in p articular those of magnetars, has essentially been an open question for decades. In this paper we explore the possibility that a magnetar may owe its strong field to a magnetized core which, as indicated by certain equations of state, may form due to phase transitions at high density mediated by strong interaction within a suffi ciently massive neutron star. We argue that the field derived from such a core could explain several inferred evolutionary behaviors of magnetars.read more
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Journal ArticleDOI
Magnetar-like emission from the young pulsar in Kes 75.
Fotis P. Gavriil,Fotis P. Gavriil,M. E. Gonzalez,Eric V. Gotthelf,Victoria M. Kaspi,Margaret A. Livingstone,P. M. Woods +6 more
TL;DR: In this article, the authors reported the detection of magnetar-like x-ray bursts from the young pulsar PSR J1846-0258, at the center of the supernova remnant Kes 75.
Journal ArticleDOI
Axial anomaly and magnetism of nuclear and quark matter
Dam Thanh Son,M. A. Stephanov +1 more
Abstract: We consider the response of the QCD ground state at finite baryon density to a strong magnetic field $B$. We point out the dominant role played by the coupling of neutral Goldstone bosons, such as ${\ensuremath{\pi}}^{0}$, to the magnetic field via the axial triangle anomaly. We show that, in vacuum, above a value of $B\ensuremath{\sim}{m}_{\ensuremath{\pi}}^{2}/e$, a metastable object appears---the ${\ensuremath{\pi}}^{0}$ domain wall. Because of the axial anomaly, the wall carries a baryon number surface density proportional to $B$. As a result, for $B\ensuremath{\gtrsim}{10}^{19}\text{ }\text{ }\mathrm{G}$ a stack of parallel ${\ensuremath{\pi}}^{0}$ domain walls is energetically more favorable than nuclear matter at the same density. Similarly, at higher densities, somewhat weaker magnetic fields of order $B\ensuremath{\gtrsim}{10}^{17}--{10}^{18}\text{ }\text{ }\mathrm{G}$ transform the color-superconducting ground state of QCD into new phases containing stacks of axial isoscalar ($\ensuremath{\eta}$ or ${\ensuremath{\eta}}^{\ensuremath{'}}$) domain walls. We also show that a quark-matter state known as ``Goldstone current state,'' in which a gradient of a Goldstone field is spontaneously generated, is ferromagnetic due to the axial anomaly. We estimate the size of the fields created by such a state in a typical neutron star to be of order ${10}^{14}--{10}^{15}\text{ }\text{ }\mathrm{G}$.
Journal ArticleDOI
Post-outburst observations of the magnetically active pulsar J1846-0258. a new braking index, increased timing noise, and radiative recovery
Margaret A. Livingstone,Cherry Ng,Victoria M. Kaspi,Fotis P. Gavriil,Fotis P. Gavriil,Eric V. Gotthelf +5 more
TL;DR: In this article, the Rossi X-ray Timing Explorer was used to measure the braking index of the pulsar J1846-0258, which was found to be 2.16+/-0.13, a decrease of 18+/-5%.
Journal ArticleDOI
A dedicated Chandra ACIS observation of the central compact object in the Cassiopeia A supernova remnant
George G. Pavlov,G. J. M. Luna +1 more
TL;DR: In this article, Chandra X-ray observations of the central compact object (CCO) in the supernova remnant Cassiopeia A were used to search for pulsations with periods longer than 0.68 s.
Journal ArticleDOI
Supernova remnants with magnetars: Clues to magnetar formation
TL;DR: In this paper, the authors discuss the lack of observational evidence that magnetars are formed as rapidly rotating neutron stars, and point out the possible connection between the jets in Cas A and its X-ray point source.
References
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