The masses of two binary neutron star systems. Thorsett,S.E.,Arzoumanian,Z.,McKinnon,M.M.,Taylor,J.H. The Astrophysical Journal . 1993Thorsett, S.E., Arzoumanian, Z., McKinnon, M.M., and Taylor, J.H., "The Masses of Two Binary Neutron Star Systems", Astrophys. J. Lett.,...
The numerical modeling of binary neutron star mergers has become a subject of much interest in recent years. While a full and accurate model of this phenomenon would require the evolution of the equations of relativistic hydrodynamics along with the Einstein field equations, a qualitative study of ...
Misaligned protoplanetary disks in a young binary star system Many extrasolar planets follow orbits that differ from the nearly coplanar and circular orbits found in our Solar System; their orbits may be eccentric or ... ELN Jensen,R Akeson - 《Nature》 被引量: 18发表: 2014年 Trojan resonant...
Doubleneutron star(DNS) systems in tight orbits are fantastic laboratories to test Einstein’s general theory of relativity. The first such DNS system, commonly known as Hulse-Taylor binarypulsar, provided the first indirect evidence of the existence ofgravitational wavesand the impetus to buildLIGO....
these binary neutron stars orbit each other they create ripples in space-time called gravitational waves. Just like material falling to the surface of a neutron star grants it angular momentum, asgravitational wavesripple away from binary neutron stars they carry angular momentum out of the system....
It is thought that the second mechanism for making supernovae (again surprising to have two different sources of such exotic events) is the evolution of white dwarfs' binary systems. Binary star systems are common, and most old stars become white dwarfs, so such systems are not uncommon. If...
inference, we combine the grid with a framework combining Gaussian process regression and singular value decomposition66to compute generic light curves for these parameters. To connect the ejecta parameters, which determine the exact properties of the light curve, with the binary neutron-star system ...
the behavior of the binding energy and total angular momentum along a quasi-equilibrium sequence, the endpoint of sequences, and the orbital angular velocity as a function of time, changing the mass ratio, the total mass of the binary system, and the equation of state of a neutron star. It...
For this, we will place the observer on the\(\theta =0\)axis of the coordinate system, at a large distance from the star, at\(r=r_O\rightarrow \infty \), such that the line of sight connecting the center of the star with the observer corresponds to the impact parameter\(b=0\)...
have created an envelope of gas large enough to affect the binary system. It is not clear why the two stars would not have drawn much closer together or even merged during this phase. Later, when the larger star exploded, it is not clear why the two objects did not go their separate ...