The strongest cosmic magnets: soft gamma-ray repeaters and anomalous X-ray pulsars

Mereghetti, S.

doi:10.1007/s00159-008-0011-z

Cited by 696 publications

(797 citation statements)

References 255 publications

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“…The weaker magnetic field for SN 1998bw is required because of its brighter luminosity (Wang et al 2016b). Usually a magnetar can have dipole field in the range 10 14 − 10 15 G (Mereghetti 2008). However, it is suggested that a dipole field as strong as ∼ 10 16 G is possible in theoretical aspects (Wang et al 2016b).…”

Section: Discussionmentioning

confidence: 99%

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Wang

Liu

et al. 2017

ApJ

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Broad-lined type Ic supernovae (SNe Ic-BL) are peculiar stellar explosions that distinguish themselves from ordinary SNe. Some SNe Ic-BL are associated with long-duration ( 2 s) gamma-ray bursts (GRBs). Black holes and magnetars are two types of compact objects that are hypothesized to be central engines of GRBs. In spite of decades of investigations, no direct evidence for the formation of black holes or magnetars has been found for GRBs so far. Here we report the finding that the early peak (t 50 days) and late-time (t 300 days) slow decay displayed in the light curves of both SNe 1998bw (associated with GRB 980425) and 2002ap (not GRB-associated) can be attributed to magnetar spin-down with initial rotation period P 0 ∼ 20 ms, while the intermediate-time (50 t 300 days) exponential decline is caused by radioactive decay of 56 Ni. The connection between the early peak and late-time slow decline in the light curves is unexpected in alternative models. We thus suggest that GRB 980425 and SN 2002ap were powered by magnetars.

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Section: Discussionmentioning

confidence: 99%

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Wang

Liu

et al. 2017

ApJ

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“…It is widely accepted that soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs) correspond to magnetars [1]. The magnetars have also been proposed [2] as an acceleration site for ultra high-energy (UHE) cosmic rays (UHECRs) and a possible association between magnetar flares [3] and UHECRs has also been observed.…”

Section: Abstract: Pion Production Strong Magnetic Field Relativistmentioning

confidence: 99%

Pion Production from Proton Synchrotron Radiation in Strong Magnetic Fields

Maruyama¹,

Cheoun²,

Kajino³

et al. 2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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We study pion production by proton synchrotron radiation in the presence of a strong magnetic field. In this study we find that the decay width satisfies a robust scaling relation. This scaling implies that one can infer the decay width in more realistic magnetic fields of 10 15 G, where n i, f ∼ 10 12 − 10 13 , from the results for n i, f ∼ 10 4 − 10 5 . Then, we present the resultant pion intensity and angular distributions for realistic magnetic field strengths. KEYWORDS: Pion Production, Strong Magnetic Field, Relativistic Quantum ApproachIt is widely accepted that soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs) correspond to magnetars [1]. The magnetars have also been proposed [2] as an acceleration site for ultra high-energy (UHE) cosmic rays (UHECRs) and a possible association between magnetar flares [3] and UHECRs has also been observed. Synchrotron radiation can be produced by highenergy protons accelerated in a strong magnetic field. Particularly, the pion process is expected to exceed photon synchrotron emission in the GeV -TeV energy range [4].However, theoretical calculations were performed approximately in a semi-classical way [5][6][7] and each model gave a different result. In addition, these model could not give a momentumdistribution of a final pion.In this work we study pion production from proton synchrotron radiation in the presence of strong magnetic fields in the relativistic quantum approach. In addition, we show the energy and angular distributions of emitted pions.We assume a uniform magnetic field along the z-direction, B = (0, 0, B), and take the electromagnetic vector potential A µ to be A = (0, 0, xB, 0) at the position r ≡ (x, y, z) . The relativistic proton wave function ψ is obtained from the following Dirac equation:where M p is the proton mass, κ p is the proton anomalous magnetic moment (AMM), e is the elementary charge, and E is the single particle energy written asBy using the pseudo-vector coupling for the πN-interaction, we obtain the decay width of the proton with the above wave functions.

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“…Phenomena related with the magnetars give a lot of information about the roles of the magnetic field. Soft gamma repeaters and anomalous X-ray pulsars correspond to magnetars [3]; the magnetars emit high energy photons. Furthermore, surface temperature of the magnetars are T ≈ 0.28 − 0.72 keV, which is larger than those of normal neutron star T ≈ 0.01 − 0.15 keV with the similar age [4].…”

Section: Introductionmentioning

confidence: 99%

Cooling Process of Magnetars with \(\nu \bar{\nu }\)-Pair and Axion Emissions in Relativistic Quantum Approach

Maruyama

Kajino

Cheoun

et al. 2018

Proceedings of the Workshop on Quarks and Compact Stars 2017 (QCS2017)

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We study a cooling process of magnetars through the νν-pair emission from electron and proton, which occurs only under the strong magnetic field, in the exact quantum calculation. Our results show that the luminosity is proportional to T 0.95 − T 1.7 when the magnetic fields are B = 10 15 − 10 16 G. The powers of the temperature are much smaller than those in the direct Urca and modified Urca processes. Thus, the νν-pair emission processes by the strong magnetic field is expected to contribute very largely to the cooling process of the magnetar.

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The strongest cosmic magnets: soft gamma-ray repeaters and anomalous X-ray pulsars

Cited by 696 publications

References 255 publications

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Pion Production from Proton Synchrotron Radiation in Strong Magnetic Fields

Cooling Process of Magnetars with \(\nu \bar{\nu }\)-Pair and Axion Emissions in Relativistic Quantum Approach

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