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Gravitation Between Spherically Symmetric Masses

Gravitation Between Spherically Symmetric Masses

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Nuclear Stability

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Protons and neutrons, collectively called nucleons, are packed together tightly in a nucleus. With a radius of about 10−15 meters, a nucleus is quite small compared to the radius of the entire atom, which is about 10−10 meters. Nuclei are extremely dense compared to bulk matter, averaging 1.8 × 1014 grams per cubic centimeter. If the earth’s density were equal to the average nuclear density, the earth’s radius would be only about 200 meters.
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Updated: Jul 18, 2026

Setting Limits on Supersymmetry Using Simplified Models

Setting Limits on Supersymmetry Using Simplified Models

Published on: November 15, 2013

Binary neutron stars: Equilibrium models beyond spatial conformal flatness.

Kōji Uryū¹, François Limousin, John L Friedman

¹Department of Physics, University of Wisconsin-Milwaukee, PO Box 413, Milwaukee, Wisconsin 53201, USA.

Physical Review Letters

|December 13, 2006

Summary

Numerical simulations of binary neutron stars reveal new insights into their final orbits. These findings improve gravitational wave template generation and cutoff frequency estimates.

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Setting Limits on Supersymmetry Using Simplified Models

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Area of Science:

Astrophysics
Numerical Relativity
Gravitational Wave Astronomy

Background:

Binary neutron stars are crucial for understanding extreme gravity and astrophysical phenomena.
Accurate modeling of inspiral phases is essential for gravitational wave detection and analysis.

Purpose of the Study:

To compute equilibria of binary neutron stars in close circular orbits using a waveless formulation.
To develop and validate numerical codes for simulating inspiraling binary neutron stars.
To investigate deviations in binding energy compared to previous theoretical approximations.

Main Methods:

Solving the Einstein-relativistic-Euler system on an initial hypersurface.
Employing a waveless formulation for numerical relativity simulations.
Developing and utilizing two independent numerical codes for cross-validation.

Main Results:

Successfully computed solution sequences for inspiraling binary neutron stars during their final orbits.
Observed deviations in binding energy near the final orbit compared to post-Newtonian and conformally flat calculations.
Generated new equilibrium solutions for binary neutron star systems.

Conclusions:

The new numerical solutions provide accurate initial data for binary neutron star merger simulations.
These solutions can be used to generate improved gravitational wave templates.
The findings enhance estimates of the gravitational wave cutoff frequency from the last inspiral orbit.