Exotic atoms at extremely high magnetic fields: the case of neutron star atmosphere

@article{Fontana2017ExoticAA,
  title={Exotic atoms at extremely high magnetic fields: the case of neutron star atmosphere},
  author={Andrea Fontana and Alessandro Colombi and Pietro Carretta and Alessandro Drago and Paolo Esposito and Paola Gianotti and Carlotta Giusti and Diego Lonardoni and Alessandro Lovato and Vincenzo Lucherini and Francesco Pederiva},
  journal={arXiv: Nuclear Theory},
  year={2017}
}
The presence of exotic states of matter in neutron stars (NSs) is currently an open issue in physics. The appearance of muons, kaons, hyperons, and other exotic particles in the inner regions of the NS, favored by energetic considerations, is considered to be an effective mechanism to soften the equation of state (EoS). In the so-called two-families scenario, the softening of the EoS allows for NSs characterized by very small radii, which become unstable and convert into a quark stars (QSs). In… 

Figures and Tables from this paper

References

SHOWING 1-10 OF 76 REFERENCES
Atomic calculation for the atmospheres of strongly-magnetized neutron stars
Complete modeling of radiative transfer in neutron star atmospheres is in progress, taking into account the anisotropy induced by magnetic fields, nonideal effects, and general relativity. As part of
Quark matter nucleation in neutron stars and astrophysical implications
Abstract.A phase of strong interacting matter with deconfined quarks is expected in the core of massive neutron stars. We investigate the quark deconfinement phase transition in cold ( $ T=0$ and hot
Hyperon puzzle: hints from quantum Monte Carlo calculations.
TLDR
It is found that the three-body hyperon-nucleon interaction plays a fundamental role in the softening of the equation of state and for the consequent reduction of the predicted maximum mass of neutron stars.
Can very compact and very massive neutron stars both exist
The existence of neutron stars with masses of ∼2M⊙ requires a stiff equation of state at high densities. On the other hand, the necessary appearance also at high densities of new degrees of freedom,
Opacities and spectra of hydrogen atmospheres of moderately magnetized neutron stars
Context. There is observational evidence that central compact objects (CCOs) in supernova remnants have moderately strong magnetic fields B ∼ 10 11 G. Meanwhile, available models of partially ionized
The scenario of two families of compact stars
Abstract.We present several arguments which favor the scenario of two coexisting families of compact stars: hadronic stars and quark stars. Besides the well-known hyperon puzzle of the physics of
A neutron star with a carbon atmosphere in the Cassiopeia A supernova remnant
TLDR
This result suggests that there is nuclear burning in the surface layers and also identifies the compact X-ray source in the centre of the Cassiopeia supernova remnant as a very young (∼330-year-old) neutron star.
A two-solar-mass neutron star measured using Shapiro delay
TLDR
Radio timing observations of the binary millisecond pulsar J1614-2230 that show a strong Shapiro delay signature are presented and the pulsar mass is calculated to be (1.97 ± 0.04)M⊙, which rules out almost all currently proposed hyperon or boson condensate equations of state.
A Massive Pulsar in a Compact Relativistic Binary
Introduction Neutron stars with masses above 1.8 solar masses (M☉), possess extreme gravitational fields, which may give rise to phenomena outside general relativity. These strong-field deviations
Isolated neutron stars: magnetic fields, distances,and spectra
Abstract We present timing measurements, astrometry, and high-resolution spectra of a number of nearby, thermally emitting, isolated neutron stars. We use these to infer magnetic field strengths and
...
...