Supernova explosions and historical chronology

Imshennik, V. S.

doi:10.1070/pu2000v043n05abeh000753

Cited by 4 publications

(5 citation statements)

References 15 publications

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“…A non-stationary model of a target corona created by fast electron heating was proposed in [19]. It is based on the selfsimilar solution [20] of a plane isothermal expansion of a given mass of substance. This solution is fully adequate to the phenomenon of thermal expansion of plasma heated by a fast electron stream, because the Coulomb mean free pass of the fast electrons depends only on its initial energy.…”

Section: Powerful Laser-accelerated Electron Stream Interaction With ...mentioning

confidence: 99%

Ultra-power shock wave driven by a laser-accelerated electron beam

Gus’kov¹

2015

Phys. Scr.

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This review is presented on modern research to achieve in a laboratory experiment the new level of shock-wave pressure of a few hundred or even thousands of Mbar when a substance is exposed to a stream of laser-accelerated fast electrons. The applications associated with the use of ultra-power shock waves as the ignition driver of inertial fusion targets as well as the tool in studying the equation of a state of a matter are discussed.

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Section: Powerful Laser-accelerated Electron Stream Interaction With ...mentioning

confidence: 99%

Ultra-power shock wave driven by a laser-accelerated electron beam

Gus’kov¹

2015

Phys. Scr.

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“…) is a specific heat; k B is the Boltzmann constant; m p is the proton mass; γ is the adiabat exponent; the constant a 0.5 th » represents the ratio of the thermal plasma energy to its full energy, see [18].…”

Section: Hydrodynamic Model Of Plasma Heated By Highenergetic Ion Fluxmentioning

confidence: 99%

“…A non-stationary hydrodynamic evolution model of a half-space plasma heated by a monoenergetic constant intensity fast electron flow was constructed in [16]. The analytical solution presented in [16] is a superposition of solutions for an isothermal rarefaction wave [17] and a selfsimilar solution for the isothermal expansion of a given mass of matter [18]. The mass in that case remains unchanged because it does not depend on the temperature of plasma heated by fast electrons.…”

Section: Introductionmentioning

confidence: 99%

Specifics of powerful shock initialization by energetic ion beam

Gus'kov

Solyanikova

Korneev

2019

Plasma Phys. Control. Fusion

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An analytical model for heating matter in the semi-infinite space by a high-energy ion flow is presented. The obtained solution obtained describes the temporal evolution of the thermodynamics and hydrodynamics of plasma in the heated region. It counts for the general stopping power dependence on plasma temperature. While the matter is heated, the mean free path of heating ions changes functionally with temperature. Namely, it does not depend on the plasma temperature at the beginning and increases with the temperature after it passes a thermal threshold. At this threshold, the thermal velocity of plasma electrons is equal to the velocity of the ions in the heating beam. The solution shows that the most advantageous regime for the initialization of the quasi-stationary shock wave realizes when the ion energy is equal to the thermal threshold. This regime corresponds to the maximum shock pressure and the slowest subsequent pressure decay with time. Special attention is devoted to the powerful shock wave driven by the laser-accelerated fast ion beam. For example, a Gbar shock pressure may be achieved by heating an aluminum target by a proton beam with intensity of about 5 10 W cm 15 2´and particle energy of about 4 MeV.

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“…In a few cases where NSs are related to historical SNe, the NS age is known rather accurately (e.g. Clark & Stephenson 1982;Imshennik 2000). However, other estimates are required to get a larger statistics.…”

Section: Initial Neutron Star Spin Periodsmentioning

confidence: 99%

Rapidly rotating neutron star progenitors

Постнов¹,

Куранов²,

Kolesnikov³

et al. 2016

Mon. Not. R. Astron. Soc.

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Rotating proto-neutron stars can be important sources of gravitational waves to be searched for by present-day and future interferometric detectors. It was demonstrated by Imshennik that in extreme cases the rapid rotation of a collapsing stellar core may lead to fission and formation of a binary proto-neutron star which subsequently merges due to gravitational wave emission. In the present paper, we show that such dynamically unstable collapsing stellar cores may be the product of a former merger process of two stellar cores in a common envelope. We applied population synthesis calculations to assess the expected fraction of such rapidly rotating stellar cores which may lead to fission and formation of a pair of proto-neutron stars. We have used the BSE population synthesis code supplemented with a new treatment of stellar core rotation during the evolution via effective core-envelope coupling, characterized by the coupling time, τ c . The validity of this approach is checked by direct MESA calculations of the evolution of a rotating 15 M ⊙ star. From comparison of the calculated spin distribution of young neutron stars with the observed one, reported by Popov and Turolla, we infer the value τ c ≃ 5 × 10 5 years. We show that merging of stellar cores in common envelopes can lead to collapses with dynamically unstable proto-neutron stars, with their formation rate being ∼ 0.1 − 1% of the total core collapses, depending on the common envelope efficiency.

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Supernova explosions and historical chronology

Cited by 4 publications

References 15 publications

Ultra-power shock wave driven by a laser-accelerated electron beam

Ultra-power shock wave driven by a laser-accelerated electron beam

Specifics of powerful shock initialization by energetic ion beam

Rapidly rotating neutron star progenitors

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