Neutron star mergers and γ-ray bursts

1991 ◽  
Author(s):  
Tsvi Piran ◽  
Ramesh Narayan ◽  
Amotz Shemi
Keyword(s):  
Neutron Star ◽  
Γ Ray

Recurrence times of γ-ray bursts from neutron star/comet encounters

Nature ◽  
1990 ◽  
Vol 344 (6264) ◽  
pp. 313-315 ◽  
Author(s):  
I. G. Mitrofanov ◽  
R. Z. Sagdeev
Keyword(s):  
Neutron Star ◽  
Recurrence Times ◽  
Γ Ray

scholarly journals Gamma-Ray Bursts and Binary Neutron Star Mergers

1996 ◽  
Vol 165 ◽  
pp. 489-502
Author(s):  
Tsvi Piran
Keyword(s):  
Neutron Star ◽  
Gravitational Radiation ◽  
Gamma Ray ◽  
Indirect Evidence ◽  
Gamma Ray Bursts ◽  
Binary Neutron Star ◽  
Merger Event ◽  
Γ Rays ◽  
Γ Ray ◽  
The One

Neutron star binaries, such as the one observed in the famous binary pulsar PSR 1913+16, end their life in a catastrophic merger event (denoted here NS2M). The merger releases ∼5 1053 ergs, mostly as neutrinos and gravitational radiation. A small fraction of this energy suffices to power γ-ray bursts (GRBs) at cosmological distances. Cosmological GRBs must pass, however, an optically thick fireball phase and the observed γ rays emerge only at the end of this phase. Hence, it is difficult to determine the nature of the source from present observations (the agreement between the rates of GRBs and NS2Ms providing only indirect evidence for this model). In the future a coinciding detection of a GRB and a gravitational-radiation signal could confirm this model.

scholarly journals Prospects of joint detections of neutron star mergers and short GRBs with Gaussian structured jets

2020 ◽  
Vol 493 (2) ◽  
pp. 1633-1639
Author(s):  
M Saleem
Keyword(s):  
Neutron Star ◽  
Joint Detection ◽  
Detection Rates ◽  
Binary Neutron Star ◽  
The Core ◽  
Relativistic Jet ◽  
Inclination Angles ◽  
Γ Ray ◽  
Short Grbs ◽  
Lower Inclination

ABSTRACT GW170817 was the first ever joint detection of gravitational waves (GW) from a binary neutron star (BNS) merger with the detections of short γ-ray burst (SGRB) counterparts. Analysis of the multiband afterglow observations of over more than a year revealed that the outflow from the merger end product was consistent with structured relativistic jet models with the core of the jet narrowly collimated to half-opening angles ∼5○. In this work, assuming that all the BNS mergers produce Gaussian structured jets with properties as inferred for GW170817, we explore the prospects of joint detections of BNS mergers and prompt γ-ray emission, expected during the current and upcoming upgrades of LIGO–Virgo–KAGRA detectors. We discuss three specific observational aspects: 1) the distribution of detected binary inclination angles, 2) the distance reach, and 3) the detection rates. Unlike GW-only detections, the joint detections are greatly restricted at large inclination angles, due to the structure of the jets. We find that at lower inclination angles (say below 20○), the distance reach as well as the detection rates of the joint detections are limited by GW detectability while at larger inclinations (say above 20○), they are limited by the γ-ray detectability.

VACUUM DISCHARGE AS A POSSIBLE SOURCE OF GAMMA-RAY BURSTS

2000 ◽  
Vol 09 (02) ◽  
pp. 185-192
Author(s):  
G. MAO ◽  
S. CHIBA ◽  
W. GREINER ◽  
K. OYAMATSU
Keyword(s):  
Neutron Star ◽  
Gamma Ray ◽  
Ambient Medium ◽  
Critical Density ◽  
Compact Object ◽  
Dense Matter ◽  
Initial Energy ◽  
Strong Interactions ◽  
Γ Ray ◽  
The Impact

We propose that spontaneous particle–anti-particle pair creations from the discharged vacuum caused by the strong interactions in dense matter are major sources of γ-ray bursts. Two neutron star collisions or black-hole-neutron star mergers at cosmological distance could produce a compact object with its density exceeding the critical density for pair creations. The emitted anti-particles annihilate with corresponding particles at the ambient medium. This releases a large amount of energy. We discuss the spontaneous [Formula: see text] pair creations within two neutron star collision and estimate the exploded energy from [Formula: see text] annihilation processes. The total energy could be around 1051–1053 erg depending on the impact parameter of colliding neutron stars. This value fits well into the range of the initial energy of the most energetic γ-ray bursts.

scholarly journals Middle aged γ-ray pulsar J1957+5033 in X-rays: pulsations, thermal emission and nebula

2020 ◽  
Author(s):  
D A Zyuzin ◽  
A V Karpova ◽  
Y A Shibanov ◽  
A Y Potekhin ◽  
V F Suleimanov
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Power Law ◽  
Thermal Emission ◽  
Single Pulse ◽  
X Rays ◽  
Middle Aged ◽  
X Ray ◽  
Photon Index ◽  
Γ Ray

Abstract We analyze new XMM-Newton and archival Chandra observations of the middle-aged γ-ray radio-quiet pulsar J1957+5033. We detect, for the first time, X-ray pulsations with the pulsar spin period of the point-like source coinciding by position with the pulsar. This confirms the pulsar nature of the source. In the 0.15–0.5 keV band, there is a single pulse per period and the pulsed fraction is ≈18 ± 6 per cent. In this band, the pulsar spectrum is dominated by a thermal emission component that likely comes from the entire surface of the neutron star, while at higher energies (≳ 0.7 keV) it is described by a power law with the photon index Γ ≈ 1.6. We construct new hydrogen atmosphere models for neutron stars with dipole magnetic fields and non-uniform surface temperature distributions with relatively low effective temperatures. We use them in the spectral analysis and derive the pulsar average effective temperature of ≈(2 − 3) × 105 K. This makes J1957+5033 the coldest among all known thermally emitting neutron stars with ages below 1 Myr. Using the interstellar extinction–distance relation, we constrain the distance to the pulsar in the range of 0.1–1 kpc. We compare the obtained X-ray thermal luminosity with those for other neutron stars and various neutron star cooling models and set some constraints on latter. We observe a faint trail-like feature, elongated ∼8 arcmin from J1957+5033. Its spectrum can be described by a power law with a photon index Γ = 1.9 ± 0.5 suggesting that it is likely a pulsar wind nebula powered by J1957+5033.

scholarly journals Neutron Star Interior Composition Explorer X-Ray Timing of the Radio and γ-Ray Quiet Pulsars PSR J1412+7922 and PSR J1849-0001

2019 ◽  
Vol 877 (2) ◽  
pp. 69 ◽  
Author(s):  
Slavko Bogdanov ◽  
Wynn C. G. Ho ◽  
Teruaki Enoto ◽  
Sebastien Guillot ◽  
Alice K. Harding ◽  
...  
Keyword(s):  
Neutron Star ◽  
X Ray ◽  
Γ Ray

scholarly journals Shall we Observe a Radio Binary Pulsar in SN 1987A?

1992 ◽  
Vol 128 ◽  
pp. 222-224
Author(s):  
Qiao G. J.
Keyword(s):  
Neutron Star ◽  
Surface Temperature ◽  
High Surface ◽  
Star Model ◽  
Single Star ◽  
X Ray ◽  
Binary Pulsar ◽  
Collapse Model ◽  
High Surface Temperature ◽  
Γ Ray

AbstractAn induced-collapse model [hereafter IC model; He et al. (1990)] can overcome the problems of the single star model of SN1987A. According to the IC model, there is a possibility that the SN1987A remnant will be a binary system with two neutron stars, one of them (SK-69 202) will have a strong magnetic field and a high surface temperature which favors detection as an X-ray or γ-ray pulsar. If the surface temperature of the neutron star cools down to T = 107 K, a radio binary pulsar is expected. There is also the possibility that an X-ray or γ-ray pulsar will be observed first, and only later will a radio pulsar will be detected.A newly formed neutron star is thought to have a short (millisecond) period. In this case, the core emission beam is then very large (Qiao 1992) and is thus very likely to swing in the direction of the Earth.

The γ-ray bursts as a result of the proper activity of the neutron star

1981 ◽  
Vol 1 (13) ◽  
pp. 153-159 ◽  
Author(s):  
G.S. Bisnovatyi-Kogan ◽  
V.M. Chechetkin
Keyword(s):  
Neutron Star ◽  
Γ Ray

scholarly journals What will eROSITA reveal among X-ray faint isolated neutron stars?

2017 ◽  
Vol 13 (S337) ◽  
pp. 112-115
Author(s):  
Adriana M. Pires
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Radio Pulsar ◽  
X Rays ◽  
Evolutionary Models ◽  
X Ray ◽  
Sky Survey ◽  
Γ Ray ◽  
Unique Potential

AbstractSince the discovery of the first radio pulsar fifty years ago, the population of neutron stars in our Galaxy has grown to over 2,600. A handful of these sources, exclusively seen in X-rays, show properties that are not observed in normal pulsars. Despite their scarcity, they are key to understanding aspects of the neutron star phenomenology and evolution. The forthcoming all-sky survey of eROSITA will unveil the X-ray faint end of the neutron star population at unprecedented sensitivity; therefore, it has the unique potential to constrain evolutionary models and advance our understanding of the sources that are especially silent in the radio and γ-ray regimes. In this contribution I discuss the expected role of eROSITA, and the challenges it will face, at probing the galactic neutron star population.

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