Possible Evidence for Free Precession of a Strongly Magnetized Neutron Star in the Magnetar 4U<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mn>0142</mml:mn><mml:mo>+</mml:mo><mml:mn>61</mml:mn></mml:mrow></mml:math>

Makishima, Kazuo; Enoto, T.; Hiraga, Junko S.; Nakano, T.; Nakazawa, K.; Sakurai, S.; Sasano, M.; Murakami, Hiroaki

doi:10.1103/physrevlett.112.171102

Cited by 107 publications

(106 citation statements)

References 38 publications

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“…First and second Suzaku observations were performed in 2007 and 2009 and already reported focusing the spectral feature and pulse modulation, respectively Makishima et al 2014). A ∼37 ks ToO was performed in 2011 September after short burst activities on July 29, 2011 (Oates et al 2011) which states showed a slight brightening than previous observations.…”

Section: U 0142+61mentioning

confidence: 99%

“…b Preceding Suzaku studies: SGR 1806−20 (Esposito et al 2007;Nakagawa et al 2009), 1E 1841−45 (Morii et al 2010), SGR 1900+14 (Nakagawa et al 2009) 4U 0142+61 Makishima et al 2014), AX J1818.8−586 (Mereghetti et al 2012), 1E 1547.0−5408 (Enoto et al 2010b;Iwahashi et al 2013;Enoto et al 2012;Makishima et al 2015), SGR 0501+4516 (Enoto et al 2009(Enoto et al , 2010cNakagawa et al 2011) CXOU J164710.2−455216 (Naik et al 2008), SGR 1833−0832 ), Swift J1822.3−1606, and Paper I. c Objects are sorted by the dipole field B d calculated from the period P and its derivativeṖ assuming the magnetic dipole radiation. d Type of observations: PV (Performance Verification phase, i.e., first 9 month after the launch), AO (Announcement of Opportunity observations), ToO (Target of Opportunity observations), and Key (Key Project observations).…”

Section: Reduction Of Broad-band Suzaku Spectramentioning

confidence: 99%

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Magnetar Broadband X-Ray Spectra Correlated with Magnetic Fields: Suzaku Archive of SGRs and AXPs Combined with NuSTAR, Swift, and RXTE

Enoto¹,

Shibata²,

Kitaguchi³

et al. 2017

ApJS

116

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Studies were made of the 1-70 keV persistent spectra of fifteen magnetars as a complete sample observed with Suzaku from 2006 to 2013. Combined with early NuSTAR observations of four hard X-ray emitters, nine objects showed a hard power-law emission dominating at 10 keV with the 15-60 keV flux of ∼1-11 × 10 −11 ergs s −1 cm −2 . The hard X-ray luminosity L h , relative to that of a soft-thermal surface radiation L s , tends to become higher toward younger and strongly magnetized objects. Updated from the previous study, their hardness ratio, defined as ξ = L h /L s , is correlated with the measured spin-down rateṖ as ξ = 0.62 × (Ṗ /10 −11 s s −1 ) 0.72 , corresponding with positive and negative correlations of the dipole field strength B d (ξ ∝ B d) and the characteristic age τ c (ξ ∝ τ −0.68 c ), respectively. Among our sample, five transients were observed during X-ray outbursts, and the results are compared with their long-term 1-10 keV flux decays monitored with Swift/XRT and RXTE/PCA. Fading curves of three bright outbursts are approximated by an empirical formula used in the seismology, showing a ∼10-40 d plateau phase. Transients show the maximum luminosities of L s ∼1035 erg s −1 , which is comparable to those of the persistently bright ones, and fade back to 10 32 erg s −1 . Spectral properties are discussed in a framework of the magnetar hypothesis.

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Section: U 0142+61mentioning

confidence: 99%

Section: Reduction Of Broad-band Suzaku Spectramentioning

confidence: 99%

Magnetar Broadband X-Ray Spectra Correlated with Magnetic Fields: Suzaku Archive of SGRs and AXPs Combined with NuSTAR, Swift, and RXTE

Enoto¹,

Shibata²,

Kitaguchi³

et al. 2017

ApJS

116

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“…Recently, a precessing motion driven by deformation as Equation (21) was inferred for a galactic magnetar from the X-ray timing observation (Makishima et al 2014(Makishima et al , 2015 …”

Section: Appendix a Spin-downmentioning

confidence: 99%

Multi-Messenger Tests for Fast-Spinning Newborn Pulsars Embedded in Stripped-Envelope Supernovae

Kashiyama

Murase

Bartos

et al. 2016

ApJ

103

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Fast-spinning strongly magnetized newborn neutron stars (NSs), including nascent magnetars, are popularly implemented as the engine of luminous stellar explosions. Here, we consider the scenario that they power various stripped-envelope (SE) supernovae (SNe), not only superluminous SNe Ic but also broad-line (BL) SNe Ibc and possibly some ordinary SNe Ibc. This scenario is also motivated by the hypothesis that Galactic magnetars largely originate from fast-spinning NSs as remnants of SE SNe. By consistently modeling the energy injection from magnetized wind and Ni  . Then, we study how multi-messenger emission can be used to discriminate such pulsar-driven SN models from other competitive scenarios. First, high-energy X-ray and gamma-ray emission from embryonic pulsar wind nebulae can probe the underlying newborn pulsar. Follow-up observations of SE SNe using NuSTAR 50 100 days -after the explosion are strongly encouraged for nearby objects. We also discuss possible effects of gravitational waves (GWs) on the spin-down of proto-NSs. If millisecond proto-NSs with B a few 10 G dip 13<´emit GWs through, e.g., non-axisymmetric rotation deformed by the inner toroidal fields of B 10 G t 16  , the GW signal can be detectable from ordinary SNe Ibc in the Virgo cluster by Advanced LIGO, Advanced Virgo, and KAGRA.

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“…[1,2,3,4,5]. One expects to find even stronger magnetic fields inside these stars as already calculated in [6]. According to virial theorem arguments, which give an upper estimate for the magnetic inside neutron stars, they can possess central magnetic fields as large as 10 18−20 G, see e.g.…”

Section: Introductionmentioning

confidence: 84%

Effects of strong magnetic fields on hybrid stars

Franzon¹,

Dexheimer²,

Schramm³

2016

Proceedings of the Modern Physics of Compact Stars 2015 — PoS(MPCS2015)

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In this work we study the effects of strong magnetic fields on hybrid stars by using a full general-relativity approach, solving the coupled Maxwell-Einstein equation in a selfconsistent way. The magnetic field is assumed to be axi-symmetric and poloidal. We take into consideration the anisotropy of the energy-momentum tensor due to the magnetic field, magnetic field effects on equation of state, the interaction between matter and the magnetic field (magnetization), and the anomalous magnetic moment of the hadrons. The equation of state used is an extended hadronic and quark SU(3) non-linear realization of the sigma model that describes magnetized hybrid stars containing nucleons, hyperons and quarks. According to our results, the effects of the magnetization and the magnetic field on the EoS do not play an important role on global properties of these stars. On the other hand, the magnetic field causes the central density in these objects to be reduced, inducing major changes in the populated degrees of freedom and, potentially, converting a hybrid star into a hadronic star.

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Possible Evidence for Free Precession of a Strongly Magnetized Neutron Star in the Magnetar 4U0142+61

Cited by 107 publications

References 38 publications

Magnetar Broadband X-Ray Spectra Correlated with Magnetic Fields: Suzaku Archive of SGRs and AXPs Combined with NuSTAR, Swift, and RXTE

Magnetar Broadband X-Ray Spectra Correlated with Magnetic Fields: Suzaku Archive of SGRs and AXPs Combined with NuSTAR, Swift, and RXTE

Multi-Messenger Tests for Fast-Spinning Newborn Pulsars Embedded in Stripped-Envelope Supernovae

Effects of strong magnetic fields on hybrid stars

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