Discovery of an Ultrafast X-Ray Pulsar in the Supernova Remnant N157B

Marshall, F. E.; Gotthelf, E. V.; Zhang, W.; Middleditch, J.; Wang, Q. Daniel

doi:10.1086/311381

Cited by 202 publications

(207 citation statements)

References 8 publications

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“…The periods for our models range between 0.08 and 0.13 ms. These are extremely short periods, not only much shorter than the observed periods of young pulsars, which are between 20 and 100 ms (Muslimov & Page 1996;Marshall et al 1998;Kaspi et al 1994), but even shorter than the critical velocity of NS, which is between 0.44 and 0.65 ms 7 Some additional braking mechanism is therefore needed to reconcile our predictions with observations (see below).…”

Section: Comparisons With Observationsmentioning

confidence: 60%

Grids of stellar models with rotation

Georgy

Ekström

Meynet

et al. 2012

A&A

305

364

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Context. In recent years, many very interesting observations have appeared concerning the positions of Wolf-Rayet (WR) stars in the Hertzsprung-Russell diagram (HRD), the number ratios of WR stars, the nature of Type Ibc supernova (SN) progenitors, long and soft gamma ray bursts (LGRB), and the frequency of these various types of explosive events. These observations represent key constraints on massive star evolution. Aims. We study, in the framework of the single-star evolutionary scenario, how rotation modifies the evolution of a given initial mass star towards the WR phase and how it impacts the rates of Type Ibc SNe. We also discuss the initial conditions required to obtain collapsars and LGRB. Methods. We used a recent grid of stellar models computed with and without rotation to make predictions concerning the WR populations and the frequency of different types of core-collapse SNe. Current rotating models were checked to provide good fits to the following features: solar luminosity and radius at the solar age, main-sequence width, red-giant and red-supergiant (RSG) positions in the HRD, surface abundances, and rotational velocities. Results. Rotating stellar models predict that about half of the observed WR stars and at least half of the Type Ibc SNe may be produced through the single-star evolution channel. Rotation increases the duration of the WNL and WNC phases, while reducing those of the WNE and WC phases, as was already shown in previous works. Rotation increases the frequency of Type Ic SNe. The upper mass limit for Type II-P SNe is ∼19.0 M for the non rotating models and ∼16.8 M for the rotating ones. Both values agree with observations. Moreover, present rotating models provide a very good fit to the progenitor of SN 2008ax. We discuss future directions of research for further improving the agreement between the models and the observations. We conclude that the mass-loss rates in the WNL and RSG phases are probably underestimated at present. We show that up to an initial mass of 40 M , a surface magnetic field inferior to about 200 G may be sufficient to produce some braking. Much lower values are needed at the red supergiant stage. We suggest that the presence/absence of any magnetic braking effect may play a key role in questions regarding rotation rates of young pulsars and the evolution leading to LGRBs.

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Section: Comparisons With Observationsmentioning

confidence: 60%

Grids of stellar models with rotation

Georgy

Ekström

Meynet

et al. 2012

A&A

305

364

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“…The central angular momentum is about an order of magnitude less than what would exist had angular momentum been conserved in the core all the way from a (rigidly rotating) mainsequence model with typical observed rotation speed (about 200 km s~1). However, the calculated presupernova angular momentum in the stellar core is still about 2 orders of magnitude greater than observed even in fast pulsars like the 16 ms pulsar in SNR N157B (Marshall et al 1998). Perhaps pulsars are slowed during or after the supernova explosion (Lindblom, Owen, & Morsink 1998 ;Owen et al 1999).…”

Section: Fig 1èangular Momentum ( J) Distribution In a 20mentioning

confidence: 93%

Collapsars: Gamma‐Ray Bursts and Explosions in “Failed Supernovae”

MacFadyen

Woosley

1999

ApJ

2,173

2,195

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Using a two-dimensional hydrodynamics code (PROMETHEUS), we explore the continued evolution of rotating helium stars, in which iron-core collapse does not produce a successful out-M a Z 10 M _ , going shock but instead forms a black hole of 2È3The model explored in greatest detail is the 14 M _ . helium core of a 35 main-sequence star. The outcome is sensitive to the angular momentum. M _ M _ For cm2 material falls into the black hole almost uninhibited. No outÑows are j 16 4 j/(1016 s~1) [ 3, expected. For the infalling matter is halted by centrifugal force outside 1000 km where neutrino j 16 Z 20, losses are negligible. The equatorial accretion rate is very low, and explosive oxygen burning may power a weak equatorial explosion. For however, a reasonable value for such stars, a compact 3 [ j 16 [ 20, disk forms at a radius at which the gravitational binding energy can be efficiently radiated as neutrinos or converted to beamed outÑow by magnetohydrodynamical (MHD) processes. These are the best candidates for producing gamma-ray bursts (GRBs). Here we study the formation of such a disk, the associated Ñow patterns, and the accretion rate for disk viscosity parameter a B 0.001 and 0.1. Infall along the rotational axis is initially uninhibited, and an evacuated channel opens during the Ðrst few seconds. Meanwhile the black hole is spun up by the accretion (to a B 0.9), and energy is dissipated in the disk by MHD processes and radiated by neutrinos. For the a \ 0.1 model, appreciable energetic outÑows develop between polar angles of 30¡ and 45¡. These outÑows, powered by viscous dissipation in the disk, have an energy of up to a few times 1051 ergs and a mass D1and are rich in 56Ni. They constitute M _ a supernova-like explosion by themselves. Meanwhile accretion through the disk is maintained for approximately 10È20 s but is time variable (^30%) because of hydrodynamical instabilities at the outer edge in a region where nuclei are experiencing photodisintegration. Because the efficiency of neutrino energy deposition is sensitive to the accretion rate, this instability leads to highly variable energy deposition in the polar regions. Some of this variability, which has signiÐcant power at 50 ms and overtones, may persist in the time structure of the burst. During the time followed, the average accretion rate for the standard a \ 0.1 and model is 0.07 s~1. The total energy deposited along the rotational j 16 \ 10 M _ axes by neutrino annihilation is (1È14) ] 1051 ergs, depending upon the evolution of the Kerr parameter and uncertain neutrino efficiencies. Simulated deposition of energy in the polar regions, at a constant rate of 5 ] 1050 ergs s~1 per pole, results in strong relativistic outÑow jets beamed to about 1% of the sky. These jets may be additionally modulated by instabilities in the sides of the "" nozzle ÏÏ through which they Ñow. The jets blow aside the accreting material, remain highly focused, and are capable of penetrating the star in D10 s. After the jet breaks through the surface of the sta...

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“…The measured period derivativeṖ ≈ 5 × 10 −14 s s −1 (Marshall et al 1998;Cusumano et al 1998) implies a spin down age of ∼ 5 000 yrs and a rotational energy loss ofĖ ≈ 4.8 × 10 38 ergs s −1 , the highest among RPPs. As common of young pulsars, PSR J0537−6910 exhibts large glitches (Middleditch et al 2006) and features a compact pulsar-wind nebula (Townsley et al 2006).…”

Section: 1mentioning

confidence: 93%

Studies of neutron stars at optical/IR wavelengths

Mignani¹,

Bagnulo²,

Luca³

et al. 2007

Isolated Neutron Stars: From the Surface to the Interior

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In the last years, optical studies of Isolated Neutron Stars (INSs) have expanded from the more classical rotation-powered ones to other categories, like the Anomalous X-ray Pulsars (AXPs) and the Soft Gammaray Repeaters (SGRs), which make up the class of the magnetars, the radio-quiet INSs with X-ray thermal emission and, more recently, the enigmatic Compact Central Objects (CCOs) in supernova remnants. Apart from 10 rotation-powered pulsars, so far optical/IR counterparts have been found for 5 magnetars and for 4 INSs. In this work we present some of the latest observational results obtained from optical/IR observations of different types of INSs.

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Discovery of an Ultrafast X-Ray Pulsar in the Supernova Remnant N157B

Cited by 202 publications

References 8 publications

Grids of stellar models with rotation

Grids of stellar models with rotation

Collapsars: Gamma‐Ray Bursts and Explosions in “Failed Supernovae”

Studies of neutron stars at optical/IR wavelengths

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