Type I supernovae and iron nucleosynthesis in the universe

Shklovskii, I. S.

doi:10.1007/bf02714968

Cited by 85 publications

(103 citation statements)

References 12 publications

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“…13 However, state-of-the-art threedimensional numerical calculations 14 show that even the most extreme asymmetric explosions do not produce pulsar velocities greater than 200 km/s. Earlier twodimensional calculations 15 claimed a somewhat higher maximal pulsar velocity, up to 500 km/s.…”

Section: Pulsar Velocitiesmentioning

confidence: 99%

Pulsar Kicks From Neutrino Oscillations

Kusenko

2004

Int. J. Mod. Phys. D

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Neutrino oscillations in a core-collapse supernova may be responsible for the observed rapid motions of pulsars. Given the present bounds on the neutrino masses, the pulsar kicks require a sterile neutrino with mass 2-20 keV and a small mixing with the active neutrinos. The same particle can be the cosmological dark matter. Its existence can be confirmed the by the X-ray telescopes if they detect a 1-10 keV photon line from the decays of the relic sterile neutrinos. In addition, one may be able to detect gravity waves from a pulsar being accelerated by neutrinos in the event of a nearby supernova.

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Section: Pulsar Velocitiesmentioning

confidence: 99%

Pulsar Kicks From Neutrino Oscillations

Kusenko

2004

Int. J. Mod. Phys. D

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“…Acceleration of the synchrotron electrons to GeV−TeV energies occurs at the shock boundary (Reynolds & Chevalier 1981). The ambient gas is heated at the shock to X-ray emitting temperatures (Shklovskii 1968;Grader et al 1970;Chevalier 1977), and radiative cooling of the gas in slower shocks produces optical emission in Hα, [S ii] and [O iii] lines (Fesen et al 1985). Observations of the thermal X-ray and optical emission can be used to derive fundamental properties such as the age of the remnant and the local gas density.…”

Section: Introductionmentioning

confidence: 99%

IKT 16: a composite supernova remnant in the Small Magellanic Cloud

Owen

Filipović

Ballet

et al. 2011

A&A

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Aims. IKT 16 is an X-ray and radio-faint supernova remnant (SNR) in the Small Magellanic Cloud (SMC). A previous X-ray study of this SNR found a hard X-ray source near its centre. Using all available archival and proprietary XMM-Newton data, alongside new multi-frequency radio-continuum surveys and optical observations at Hα and forbidden [SII] and [OIII] lines, we aim to constrain the properties of the SNR and discover the nature of the hard source within. Methods. We combine XMM-Newton datasets to produce the highest quality X-ray image of IKT 16 to date. We use this, in combination with radio and optical images, to conduct a multi-wavelength morphological analysis of the remnant. We extract separate spectra from the SNR and the bright source near its centre, and conduct spectral fitting of both regions. Results. We find IKT 16 to have a radius of 37 ± 3 pc, with the bright source located 8 ± 2 pc from the centre. This is the largest known SNR in the SMC. The large size of the remnant suggests it is likely in the Sedov-adiabatic phase of evolution. Using a Sedov model to fit the SNR spectrum, we find an electron temperature kT of 1.03 ± 0.12 keV and an age of ≈14700 yr. The absorption found requires the remnant to be located deep within the SMC. The bright source is fit with a power law with index Γ = 1.58 ± 0.07, and is associated with diffuse radio emission extending towards the centre of the SNR. We argue that this source is likely to be the neutron star remnant of the supernova explosion, and infer its transverse kick velocity to be 580 ± 100 km s −1 . The X-ray and radio properties of this source strongly favour a pulsar wind nebula (PWN) origin.

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“…However, some of the observed pulsars have a negativė p value due to various effects such as acceleration of the pulsar along the line of sight, the differential Galactic rotation and the Shklovskii effect (Shklovskii 1970). Thus, we need to investigate the statistical feature ofṗ of many pulsars, rather than that of individual pulsars, in order to probe the existence of linearlychanging GWs.…”

Section: Detectability Of Gravitational Wavesmentioning

confidence: 99%

Gravitational waves from an SMBH binary in M 87

Yonemaru

Kumamoto

Kuroyanagi

et al. 2016

Publications of the Astronomical Society of Japan

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In this paper, we study gravitational-wave (GW) emission from a hypothetical supermassive black-hole (SMBH) binary at the center of M87. The existence of a SMBH other than that usually identified with the central AGN is a possible explanation for the observed displacement (∼ O(1) pc) between the AGN and the galactic centroid, and it is reasonable to assume considering the evolution of SMBHs through galaxy mergers. Because the period of the binary and the resulting GWs is much longer than the observational time span, we calculate the variation of the GW amplitude, rather than the amplitude itself. We investigate the dependence on the orbital elements and the second BH mass taking the observational constraints into account. The frequency of the GWs is too low to be detected with the conventional pulsar timing array and we propose a new method to detect such low-frequency GWs with the distribution function of pulsar spin-down rates. Although the GWs from a SMBH binary which explains the observed displacement is extremely hard to be detected even with the new method, GWs are still a useful way to probe the M87 center.

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Type I supernovae and iron nucleosynthesis in the universe

Cited by 85 publications

References 12 publications

Pulsar Kicks From Neutrino Oscillations

Pulsar Kicks From Neutrino Oscillations

IKT 16: a composite supernova remnant in the Small Magellanic Cloud

Gravitational waves from an SMBH binary in M 87

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