Bounds on Neutron- Mirror Neutron Mixing from Pulsar Timings and Gravitational Wave Detections. (arXiv:1901.07077v2 [hep-ph] CROSS LISTED)

Bounds on Neutron- Mirror Neutron Mixing from Pulsar Timings and Gravitational Wave Detections. (arXiv:1901.07077v2 [hep-ph] CROSS LISTED)
<a href="http://arxiv.org/find/hep-ph/1/au:+Goldman_I/0/1/0/all/0/1">Itzhak Goldman</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Mohapatra_R/0/1/0/all/0/1">Rabindra N. Mohapatra</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Nussinov_S/0/1/0/all/0/1">Shmuel Nussinov</a>

The mass loss in putative neutron star to mixed neutron – mirror neutron star
transition implies a significant change of orbital period. The precise
constancy of the latter can restrict scenarios recently suggested where neutron
to mirror neutron mixing occurring in neutron stars, transforms them into mixed
stars helping explain the narrow mass distribution observed for pulsars in
binary systems. The observation of a very old millisecond pulsar with a mass of
2 solar masses is an additional strong constraint on the above transition.We
also note that the observed gravitational waves signals from neutron-neutron
stars merger constrain the neutron to mirror neutron transitions inside neutron
stars. These considerations exclude a large region in the $epsilon’$, $delta
m’$ plane of the neutron-mirror neutron mixing and mass

The mass loss in putative neutron star to mixed neutron – mirror neutron star
transition implies a significant change of orbital period. The precise
constancy of the latter can restrict scenarios recently suggested where neutron
to mirror neutron mixing occurring in neutron stars, transforms them into mixed
stars helping explain the narrow mass distribution observed for pulsars in
binary systems. The observation of a very old millisecond pulsar with a mass of
2 solar masses is an additional strong constraint on the above transition.We
also note that the observed gravitational waves signals from neutron-neutron
stars merger constrain the neutron to mirror neutron transitions inside neutron
stars. These considerations exclude a large region in the $epsilon’$, $delta
m’$ plane of the neutron-mirror neutron mixing and mass

http://arxiv.org/icons/sfx.gif

Comments are closed.