scholarly journals Soft gravitational radiation from multi-body collisions

2021 ◽  
Vol 2021 (11) ◽  
Author(s):  
Andrea Addazi ◽  
Kaiqiang Alan Zeng
Keyword(s):  
Energy Flux ◽  
Gravitational Radiation ◽  
Radiation Flux ◽  
Radiation Energy ◽  
Simple Expression ◽  
Quantum Spin ◽  
Particle Collisions ◽  
The Masses ◽  
Multi Body ◽  
Universal Expression

Abstract We derive a universal expression for the gravitational radiation energy spectrum dEGW/dω at sub-leading order emitted from a generic gravitational hard scattering of multi-particles or multi-bodies. Our result includes all $$ \mathcal{O} $$ O (ω) corrections to the gravitational radiation flux from a generic 2 → N collision, in both the cases of massless and massive particles/bodies. We also show the dependence of the radiation energy flux by the quantum spin in case of particle collisions. Then, we consider the specific case of a gravitational elastic scattering of two massive bodies, i.e. m + M → m + M with m, M the masses of the two bodies respectively. We demonstrate that in this case all $$ \mathcal{O} $$ O (ω) contributions to the energy flux exactly cancel each others. Nevertheless, we also show that, for a 2 → 2 inelastic scattering, the inclusion of sub-leading soft gravitons leads to a not zero radiation flux, having a simple expression in certain asymptotic regimes. Our results can be applied to the case of Black Hole collisions with possible testable implications in gravitational waves physics.

OBSERVATION OF THE COLLINEAR MULTI-BODY DECAYS IN THE REACTION 238U+4He (40 MEV)

2008 ◽  
Vol 17 (10) ◽  
pp. 2226-2230 ◽  
Author(s):  
◽  
YU. PYATKOV
Keyword(s):  
Inelastic Scattering ◽  
Flight Path ◽  
Scission Point ◽  
Magic Clusters ◽  
A Chain ◽  
The Masses ◽  
Multi Body

Two different modes of the multibody collinear decay from the reaction 238 U +4 He (40 MeV ) are discussed. Basing on the masses of three detected fragments one can come to conclusion that the decaying system in each mode looks like a chain consisting of two or three magic clusters respectively. Some of the clusters involved undergo "second" clusterisation in the scission point leading to formation of dinuclear molecules. These latter can disintegrate via inelastic scattering on the materials on the flight path.

Magnetic traversable wormhole as accelerator of charged particles

2020 ◽  
Vol 35 (02n03) ◽  
pp. 2040026
Author(s):  
A. A. Kirillov ◽  
E. P. Savelova
Keyword(s):  
Synchrotron Radiation ◽  
Kinetic Energy ◽  
Magnetic Fields ◽  
Stationary State ◽  
Energy Flux ◽  
Charged Particles ◽  
Radiation Energy ◽  
Traversable Wormhole ◽  
Radiation Energy Flux

We show that the scattering of radiation on a traversable wormhole forms a vortex in the radiation energy flux. Then, if the wormhole possesses also a magnetic fields, the vortex accelerates charged particles along the magnetic lines and such a system works as an accelerator. If the vortex is small, the system reaches the stationary state, when the income of the kinetic energy reradiates completely in the form of the synchrotron radiation. Such a mechanism allows us to relate a part of observed sources of the synchrotron radiation to magnetic wormholes.

scholarly journals Physical Interpretation of Dwarf Nova Primary Effective Temperatures

2004 ◽  
Vol 194 ◽  
pp. 192-193
Author(s):  
Dean M. Townsley ◽  
Lars Bildsten
Keyword(s):  
Gravitational Radiation ◽  
Accretion Rate ◽  
Thermal State ◽  
Cataclysmic Variables ◽  
Theoretical Work ◽  
Dwarf Novae ◽  
Radiation Losses ◽  
Accretion Rates ◽  
The Masses ◽  
The Impact

AbstractWe have undertaken a theoretical study of the impact of the accumulating envelopes on the thermal state of the underlying white dwarf (WD). This has allowed us to find the equilibrium WD core temperatures, the classical nova ignition masses and the thermal luminosities for WDs accreting at rates of 10–11 – 10–8M⊙ yr–1. These accretion rates are most, appropriate to WDs in cataclysmic variables (CVs) of (Porb ≲ 7 hr), many of which accrete sporadically as Dwarf Novae. Over twenty Dwarf Novae have been observed in quiescence, when the accretion rate is low and the WD photosphere is detected and Teff measured. Comparing our theoretical work to these observations allows us to constrain the WD mass and the time averaged accretion rate, ⟨Ṁ⟩. If ⟨Ṁ⟩ is that given by gravitational radiation losses alone, then the WD masses are > 0.8 M⊙. An alternative conclusion is that the masses are closer to 0.6M⊙ and ⟨Ṁ⟩ is 3-4 times larger than that expected from gravitational radiation losses.

Gravitational radiation field of an isolated system at null infinity

1990 ◽  
Vol 431 (1882) ◽  
pp. 337-344 ◽  
Keyword(s):  
Radiation Field ◽  
Gravitational Radiation ◽  
High Frequency ◽  
Radiation Flux ◽  
Flat Space ◽  
Background Field ◽  
Null Infinity ◽  
Present Treatment ◽  
New Formula ◽  
Space Result

The quadrupole and octupole contributions to the gravitational radiation flux at null infinity from an initially stationary isolated system are computed in terms of the asymptotic moments defined there. The present treatment incorporates the influence of the background field of the source while still neglecting the nonlinear self-interaction of the radiation. Compared with the flat space result, the new formula predicts a suppression of the contribution from the high-frequency modes for which the frequency ω satisfies GM 0 ω / c 3 ≫ 1, M 0 being the initial mass of the system.

Sequential and Near-Simultaneous Multi-Body Collisions

2004 ◽  
Author(s):  
D. Dane Quinn ◽  
Kalyan Bairavarasu
Keyword(s):  
Initial Conditions ◽  
Coefficient Of Restitution ◽  
Initial Configuration ◽  
Collision Model ◽  
Sufficient Distance ◽  
Initial Spacing ◽  
Compliance Model ◽  
The Masses ◽  
Multi Body ◽  
Impact Duration

This work considers a three mass collision model with finite-time, compliant contacts. If the masses are initially separated by a sufficient distance, the collision sequence is sequential, that is, comprised of a sequence of pairwise impacts. The final velocities of each mass are then independent of the specific initial spacing. In contrast, if the initial spacing between the masses is sufficiently small there exists an interval during which the three masses interact simultaneously. In this instance the final velocity state also depends on the initial configuration of the system. Given an assumed impact duration and coefficient of restitution for a pairwise collision, a two-dimensional map is derived to describe those initial conditions that lead to pairwise sequences. Finally, for a specific nonlinear compliance model the variation in the final velocities is characterized in terms of the initial configuration and velocity state of the system.

Radiation energy flux of Dirac field of static spherically symmetric black holes

2010 ◽  
Vol 19 (9) ◽  
pp. 090402
Author(s):  
Meng Qing-Miao ◽  
Jiang Ji-Jian ◽  
Li Zhong-Rang ◽  
Wang Shuai
Keyword(s):  
Black Holes ◽  
Energy Flux ◽  
Radiation Energy ◽  
Dirac Field ◽  
Spherically Symmetric ◽  
Radiation Energy Flux

THE INFLUENCE OF THE INERTIAL DRAGGING EFFECT ON GRAVITATIONAL RADIATION EMITTED FROM A PARTICLE MOVING IN EQUATORIAL GEODESIC CIRCULAR ORBIT ABOUT A KERR’S BLACK HOLE

1993 ◽  
Vol 02 (02) ◽  
pp. 149-161
Author(s):  
BIPING GONG
Keyword(s):  
Black Hole ◽  
Continuous Function ◽  
Gravitational Radiation ◽  
Circular Orbit ◽  
Turning Point ◽  
Radiation Energy ◽  
Angular Frequency ◽  
Related Function ◽  
Classical Turning Point ◽  
Main Factors

Using Chranowski and Misner’s equations,1 gravitational radiation emitted from a particle moving in an equatorial geodesic circular orbit about a Kerr’s black hole is calculated. Outside the classical turning point, the radiation energy can be represented as a continuous function of orbital radius of the particle, and thus a corresponding curve is obtained. Using Wilkins’ approach,2 two inertial dragging related functions are obtained by restricting the orbit of the particle to the equatorial plane of a Kerr’s black hole. By comparing the curve of the gravitational radiation and the curves of the simulating functions (consisting of the angular frequency and the drag related function), we come to the conclusion that inertial dragging effect on a particle is one of the main factors that influences the gravitational radiation.

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