Yi, S. X. 2014 长暴X射线的平台可能是磁星所导致

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作为能量注入的中心能源。

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Title:		X-Ray Afterglow Plateaus of Long Gamma-Ray Bursts: Further Evidence for Millisecond Magnetars
Authors:		Yi, S. X.; Dai, Z. G.; Wu, X. F.; Wang, F. Y.
Publication:		eprint arXiv:1401.1601
Publication Date:		01/2014
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		13 pages, 2 figures, 1 table, submitted to ApJL
Bibliographic Code:		2014arXiv1401.1601Y

Abstract

Many long-duration gamma-ray bursts (GRBs) were observed by {\it Swift}/XRT to have plateaus in their X-ray afterglow light curves. This plateau phase has been argued to be evidence for long-lasting activity of magnetar (ultra-strongly magnetized neutron stars) central engines. However, the emission efficiency of such magnetars in X-rays is still unknown. Here we collect 24 long GRB X-ray afterglows showing plateaus followed by steep decays. We extend the well-known relationship between the X-ray luminosity ${L_{\mathrm{X}}}$ and spin-down luminosity $L_{\mathrm{sd}}$ of pulsars to magnetar central engines, and find that the initial rotation period $P_{0}$ ranges from 1 ms to 10 ms and that the dipole magnetic field $B$ is centered around $10^{15}$ G. These constraints not only favor the suggestion that the central engines of some long GRBs are very likely to be rapidly rotating magnetars but also indicate that the magnetar plateau emission efficiency in X-rays is close to 100%.

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Lü, Hou-Jun 2014 磁星作为伽马暴的中心引擎

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用closure relation和磁星的预言对比，发现一致。

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Title:		A test of the millisecond magnetar central engine model of GRBs with Swift data
Authors:		Lü, Hou-Jun; Zhang, Bing
Publication:		eprint arXiv:1401.1562
Publication Date:		01/2014
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		19 pages, 35 figures, 3 Tables. comments are welcome
Bibliographic Code:		2014arXiv1401.1562L

Abstract

A rapidly spinning, strongly magnetized neutron star (magnetar) has been proposed as one possible candidate of the central engine of gamma-ray bursts (GRBs). In this paper, we systematically analyze the Swift/XRT light curves of long GRBs detected before 2013 August, and characterize them into four categories based on how likely they may harbor a magnetar central engine: "Gold", "Silver", "Aluminum" and "Non-magnetar". We also independently analyze the data of short GRBs with a putative magnetar central engine. We then perform a statistical study of various properties of the magnetar samples and the non-magnetar sample, and investigate whether the data are consistent with the hypothesis that there exist two types of central engines. By deriving the physical parameters of the putative magnetars, we find that the observations of the Gold and Silver samples are generally consistent with the predictions of the magnetar model. For a reasonable beaming factor for long GRBs, the derived magnetar surface magnetic field $B_p$ and initial spin period $P_0$ fall into the reasonable range. Magnetar winds in short GRBs, on the other hand, are consistent with being isotropic. No GRB in the magnetar sample has a beam-corrected total energy exceeding the maximum energy budget defined by the initial spin energy of the magnetar ($E_{\rm rot}\sim 2\times 10^{52}$ erg), while some non-magnetar GRBs do violate such a limit. With beaming correction, on average the non-magnetar sample (probably powered by a black hole) is more energetic and luminous than the magnetar samples. Our analysis hints that millisecond magnetars are likely operating in a good fraction, but probably not all, GRBs.

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Bernardini 2014 GRB 130427A的磁星模型

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Title:		A magnetar powering the ordinary monster GRB 130427A?
Authors:		Bernardini, M. G.; Campana, S.; Ghisellini, G.; D'Avanzo, P.; Calderone, G.; Covino, S.; Cusumano, G.; Ghirlanda, G.; La Parola, V.; Maselli, A.; Salvaterra, A. Melandri R.; Burlon, D.; D'Elia, V.; Fugazza, D.; Sbarufatti, B.; Vergani, S. D.; Tagliaferri, G.
Publication:		eprint arXiv:1401.1972
Publication Date:		01/2014
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		5 pages, 1 figure, accepted for publication in MNRAS Letters
Bibliographic Code:		2014arXiv1401.1972B

Abstract

We present the analysis of the extraordinarily bright Gamma-Ray Burst (GRB) 130427A under the hypothesis that the GRB central engine is an accretion-powered magnetar. In this framework, initially proposed to explain GRBs with precursor activity, the prompt emission is produced by accretion of matter onto a newly-born magnetar, and the observed power is related to the accretion rate. The emission is eventually halted if the centrifugal forces are able to pause accretion. We show that the X-ray and optical afterglow is well explained as the forward shock emission with a jet break plus a contribution from the spin-down of the magnetar. Our modelling does not require any contribution from the reverse shock, that may still influence the afterglow light curve at radio and mm frequencies, or in the optical at early times. We derive the magnetic field ($B\sim 10^{16}$ G) and the spin period ($P\sim 20$ ms) of the magnetar and obtain an independent estimate of the minimum luminosity for accretion. This minimum luminosity results well below the prompt emission luminosity of GRB 130427A, providing a strong consistency check for the scenario where the entire prompt emission is the result of continuous accretion onto the magnetar. This is in agreement with the relatively long spin period of the magnetar. GRB 130427A was a well monitored GRB showing a very standard behavior and, thus, is a well-suited benchmark to show that an accretion-powered magnetar gives a unique view of the properties of long GRBs.

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Fan, Yi-Zhong 2013 GRB 130603B的超大质量磁星模型

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拟合了X和光学，除了kilonova的光学的点，其它的用磁星能量注入拟合。

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Title:		A Supramassive Magnetar Central Engine for GRB 130603B
Authors:		Fan, Yi-Zhong; Yu, Yun-Wei; Xu, Dong; Jin, Zhi-Ping; Wu, Xue-Feng; Wei, Da-Ming; Zhang, Bing
Affiliation:		AA(Key Laboratory of dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Science, Nanjing 210008, China yzfan@pmo.ac.cn), AB(Institute of Astrophysics, Central China Normal University, Wuhan 430079, China zhang@physics.unlv.edu), AC(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark), AD(Key Laboratory of dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Science, Nanjing 210008, China), AE(Chinese Center for Antarctic Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China), AF(Key Laboratory of dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Science, Nanjing 210008, China), AG(Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154, USA)
Publication:		The Astrophysical Journal Letters, Volume 779, Issue 2, article id. L25, 4 pp. (2013). (ApJL Homepage)
Publication Date:		12/2013
Origin:		IOP
Astronomy Keywords:		gamma rays: general, radiation mechanisms: non-thermal
DOI:		10.1088/2041-8205/779/2/L25
Bibliographic Code:		2013ApJ...779L..25F

Abstract

We show that the peculiar early optical emission and, in particular, the X-ray afterglow emission of the short-duration burst GRB 130603B can be explained by continuous energy injection into the blastwave from a supramassive magnetar central engine. The observed energetics and temporal/spectral properties of the late infrared bump (i.e., the "kilonova") are also found to be consistent with emission from the ejecta launched during a neutron star (NS)-NS merger and powered by a magnetar central engine. The isotropic-equivalent kinetic energies of both the gamma-ray burst (GRB) blastwave and the kilonova are approximately E_k ~ 10⁵¹ erg, consistent with being powered by a near-isotropic magnetar wind. However, this relatively small value requires that most of the initial rotational energy of the magnetar (~a few × 10⁵² erg) is carried away by gravitational wave radiation. Our results suggest that (1) the progenitor of GRB 130603B was a NS-NS binary system, the merger product of which would have been a supramassive NS that lasted for about ~1000 s (2) the equation of state of the nuclear matter should be stiff enough to allow the survival of a long-lived supramassive NS; thus this suggested that the detection of the bright electromagnetic counterparts of gravitational wave triggers without short GRB associations is promising in the upcoming Advanced LIGO/VIRGO era.

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Bucciantini 2011 部分有延展辐射的短暴可能是磁星

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考虑这种磁星起源的喷流及其准直。

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Title:		Short GRBs with Extended Emission from Magnetar Birth: Jet Formation and Collimation
Authors:		Bucciantini, N.; Metzger, B. D.; Thompson, T. A.; Quataert, E.
Publication:		eprint arXiv:1106.4668
Publication Date:		06/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		10 pages, 5 figures, submitted to MNRAS
Bibliographic Code:		2011arXiv1106.4668B

Abstract

Approximately 1/4-1/2 of short duration Gamma-Ray Bursts are followed by variable X-ray emission lasting ~ 100 s with a fluence comparable or exceeding that of the initial burst itself. The long duration and significant energy of this `extended emission'(EE) poses a major challenge to the standard binary neutron star merger model. metzger08 recently proposed that the EE is powered by the spin-down of a strongly magnetized neutron star. However, the effects of surrounding material on the magnetar outflow have not yet been considered. Here we present time-dependent axisymmetric relativistic magnetohydrodynamic simulations of the interaction of the relativistic proto-magnetar wind with a surrounding 10^-1 10^-3 M_\odot envelope, which represents material ejected during the merger; the supernova following AIC; or via outflows from the accretion disk. The collision between the relativistic magnetar wind and the expanding ejecta produces a magnetized nebula inside the ejecta. A strong toroidal magnetic field builds up in the nebula, which drives a bipolar jet out through the ejecta, similar to the magnetar model developed in the case of long duration GRBs. We quantify the `break-out' time and opening angle of the jet theta_j as a function of the wind energy flux dot{E} and ejecta mass M_ej. We show that dot{E} and theta_j are inversely correlated, such that the beaming-corrected (isotropic) luminosity of the jet is primarily a function of M_ej. Both variability arguments, and the lower limit on the power of magnetar outflows capable of producing bright emission, suggest that the true opening angle of the magnetar jet must be relatively large. The model thus predicts a class of events for which the EE is observable with no associated short GRB. These may appear as long-duration GRBs or X-Ray Flashes, which may be detected by future all-sky X-ray survey missions.

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Scholz 2011 磁星1E 1547-5408在2009年的爆发

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Title:		The 2009 outburst of magnetar 1E 1547-5408: Persistent radiative and burst properties
Authors:		Scholz, Paul; Kaspi, Victoria M.
Publication:		eprint arXiv:1106.5445
Publication Date:		06/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		10 pages, 9 figures. Accepted for publication in ApJ
Bibliographic Code:		2011arXiv1106.5445S

Abstract

The magnetar 1E~1547$-$5408 recently exhibited two periods of outburst, beginning on 2008 October 3 and 2009 January 22. Here we present an analysis of the persistent radiative evolution and a statistical study of the burst properties during the 2009 outburst using the {\em Swift} X-ray Telescope (XRT). We find that the 1--10 keV flux increased by a factor of $\sim500$ and hardened significantly, peaking $\sim6$ hours after the onset of the outburst. The pulsed fraction decreased to zero at the peak of the outburst, exhibiting an anti-correlation with phase-averaged flux. Properties of the several hundred X-ray bursts during the 2009 outburst were determined and compared to tho from other magnetar outburst events. We find that the peaks of the bursts occur randomly in phase but that the folded counts that compose the bursts exhibit a pulse which is misaligned with the persistent pulse phase. We also report a correlation between burst hardness and flux. We compare the hardness-flux evolution of the persistent emission of both outbursts to those from other magnetars and find that although there does exist an overall trend, the degree of hardening for a given increase in flux is not uniform from source to source. These results are discussed in the context of previous results and within the magnetar model.

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Metzger 2010 伽马暴的原磁星模型

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Title:		The Proto-Magnetar Model for Gamma-Ray Bursts
Authors:		Metzger, B. D.; Giannios, D.; Thompson, T. A.; Bucciantini, N.; Quataert, E.
Publication:		eprint arXiv:1012.0001
Publication Date:		11/2010
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		21 pages (plus 2 appendices), 21 figures, 1 table, submitted to MNRAS
Bibliographic Code:		2010arXiv1012.0001M

Abstract

Long duration Gamma-Ray Bursts (GRBs) originate from the core collapse of massive stars, but the identity of the central engine remains elusive. Previous work has shown that rapidly spinning, strongly magnetized proto-neutron stars (`millisecond proto-magnetars') produce outflows with energies, timescales, and magnetizations sigma_0 (maximum Lorentz factor) that are consistent with those required to produce long GRBs. Here we extend this work in order to construct a self-consistent model that directly connects the properties of the central engine to the observed prompt emission. Just after the launch of the supernova shock, a wind heated by neutrinos is driven from the proto-magnetar. The outflow is collimated into a bipolar jet by its interaction with the star. As the magnetar cools, the wind becomes ultra-relativistic and Poynting-flux dominated (sigma_0 >> 1) on a timescale comparable to that required for the jet to clear a cavity through the star. Although the site and mechanism of the prompt emission are debated, we calculate the emission predicted by two models: magnetic dissipation and internal shocks. Our results favor the magnetic dissipation model because it (1) predicts a relatively constant `Band' spectral peak energy E_peak with time during the GRB and (2) reproduces the observed Amati/Yonetoku correlations between E_peak and the GRB energy/luminosity. The jet baryon loading decreases abruptly when the neutron star becomes transparent to neutrinos at t ~ 10-100 seconds. Jets with ultra-high magnetization cannot effectively accelerate and dissipate their energy, suggesting this transition ends the prompt emission and may explain the steep decay phase that follows. We assess several phenomena potentially related to magnetar birth, including low luminosity GRBs, thermal-rich GRBs/X-ray Flashes, very luminous supernovae, and short duration GRBs with extended emission.

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Abadie 2010 用LIGO和Virgo找6个磁星的引力波

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没有看到。

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Title:		Search for Gravitational Wave Bursts from Six Magnetars
Authors:		LIGO Scientific Collaboration; Virgo Collaboration
Publication:		eprint arXiv:1011.4079
Publication Date:		11/2010
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Comment:		9 pages, 3 figures
Bibliographic Code:		2010arXiv1011.4079L

Abstract

Soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are thought to be magnetars: neutron stars powered by extreme magnetic fields. These rare objects are characterized by repeated and sometimes spectacular gamma-ray bursts. The burst mechanism might involve crustal fractures and excitation of non-radial modes which would emit gravitational waves (GWs). We present the results of a search for GW bursts from six galactic magnetars that is sensitive to neutron star f-modes, thought to be the most efficient GW emitting oscillatory modes in compact stars. One of them, SGR 0501+4516, is likely ~1 kpc from Earth, an order of magnitude closer than magnetars targeted in previous GW searches. A second, AXP 1E 1547.0-5408, gave a burst with an estimated isotropic energy >10^{44} erg which is comparable to the giant flares. We find no evidence of GWs associated with a sample of 1279 electromagnetic triggers from six magnetars occurring between November 2006 and June 2009, in GW data from the LIGO, Virgo, and GEO600 detectors. Our lowest model-dependent GW emission energy upper limits for band- and time-limited white noise bursts in the detector sensitive band, and for f-mode ringdowns (at 1090 Hz), are 3.0x10^{44} d_1^2 erg and 1.4x10^{47} d_1^2 erg respectively, where d_1 = d_{0501} / 1 kpc and d_{0501} is the distance to SGR 0501+4516. These limits on GW emission from f-modes are an order of magnitude lower than any previous, and approach the range of electromagnetic energies seen in SGR giant flares for the first time.

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Yu 2009 X射线余辉的平降阶段可能来自奇异星而不是磁星

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Title:		The Newly Born Magnetars Powering Gamma-Ray Burst Internal-Plateau Emission: Are There Strange Stars?
Authors:		Yu, Yun-Wei; Cao, Xiao-Feng; Zheng, Xiao-Ping
Affiliation:		AA(Institute of Astrophysics, Huazhong Normal University, Wuhan 430079, China yuyw@phy.ccnu.edu.cn), AB(Institute of Astrophysics, Huazhong Normal University, Wuhan 430079, China), AC(Institute of Astrophysics, Huazhong Normal University, Wuhan 430079, China)
Publication:		The Astrophysical Journal Letters, Volume 706, Issue 2, pp. L221-L225 (2009). (ApJL Homepage)
Publication Date:		12/2009
Origin:		IOP
ApJ Keywords:		gamma rays: bursts, stars: neutron
DOI:		10.1088/0004-637X/706/2/L221
Bibliographic Code:		2009ApJ...706L.221Y

Abstract

The internal-plateau X-ray emission of gamma-ray bursts (GRBs) indicates that a newly born magnetar could be the central object of some GRBs. The observed luminosity and duration of the plateaus suggest that, for such a magnetar, a rapid spin with a sub- or millisecond period is sometimes able to last thousands of seconds. In this case, the conventional neutron star (NS) model for the magnetar may be challenged, since the rapid spin of nascent NSs would be remarkably decelerated within hundreds of seconds due to r-mode instability. In contrast, the r-modes can be effectively suppressed in nascent strange stars (SSs). In other words, to a certain extent, only SSs can keep nearly constant extremely rapid spin for a long period of time during the early ages of the stars. We thus propose that the sample of the GRB rapidly spinning magnetars can be used to test the SS hypothesis based on the distinct spin limits of NSs and SSs.

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Zhang 2009 磁星的超吸积

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Title:		Hyperaccreting Disks around Magnetars for Gamma-ray Bursts: Effects of Strong Magnetic Fields
Authors:		Zhang, Dong; Dai, Z. G.
Affiliation:		AA(Department of Astronomy, Ohio State University, 140 W. 18th Avenue, Columbus, OH 43210, USA ; Department of Astronomy, Nanjing University, Nanjing 210093, China; dzhang@astronomy.ohio-state.edu ), AB(Department of Astronomy, Nanjing University, Nanjing 210093, China dzg@nju.edu.cn)
Publication:		The Astrophysical Journal, Volume 718, Issue 2, pp. 841-866 (2010). (ApJ Homepage)
Publication Date:		08/2010
Origin:		IOP
ApJ Keywords:		accretion, accretion disks, gamma-ray burst: general, magnetic fields, neutrinos, stars: neutron
DOI:		10.1088/0004-637X/718/2/841
Bibliographic Code:		2010ApJ...718..841Z

Abstract

Hyperaccreting neutron stars or magnetar disks cooled via neutrino emission can be candidates of gamma-ray burst (GRB) central engines. The strong field >=10¹⁵-10¹⁶ G of a magnetar can play a significant role in affecting the disk properties and even lead to the funnel accretion process. In this paper, we investigate the effects of strong fields on the disks around magnetars, and discuss implications of such accreting magnetar systems for GRBs and GRB-like events. We discuss quantum effects of the strong fields on the disk thermodynamics and microphysics due to modifications of the electron distribution and energy in the strong field environment, and use the magnetohydrodynamical conservation equations to describe the behavior of the disk flow coupled with a large-scale field, which is generated by the star-disk interaction. If the disk field is open, the disk properties mainly depend on the ratio between |B _phi/B_z | and Ω/Ω _K with B _phi and B_z being the azimuthal and vertical components of the disk field, and Ω and Ω _K being the accretion flow angular velocity and Keplerian velocity, respectively. On the other hand, the disk properties also depend on the magnetar spin period if the disk field is closed. In general, stronger fields give higher disk densities, pressures, temperatures, and neutrino luminosity. Moreover, strong fields will change the electron fraction and degeneracy state significantly. A magnetized disk is always viscously stable outside the Alfvén radius, but will be thermally unstable near the Alfvén radius where the magnetic field plays a more important role in transferring the angular momentum and heating the disk than the viscous stress. The funnel accretion process will be important only for an extremely strong field, which creates a magnetosphere inside the Alfvén radius and truncates the plane disk. Because of higher temperature and more concentrated neutrino emission of a ring-like belt region on the magnetar surface covered by funnel accretion, the neutrino annihilation rate from the accreting magnetar can be much higher than that from an accreting neutron star without fields. Furthermore, the neutrino annihilation mechanism, which releases the gravitational energy of the surrounding disk, and the magnetically driven pulsar wind, which extracts the stellar rotational energy from the magnetar surface, can work together to generate and feed an ultrarelativistic jet along the stellar magnetic poles.

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