A5013526613- Pulsars and Gravitational Waves Research
- Geophysics and Gravity Measurements
- Gamma-ray bursts and supernovae
- High-pressure geophysics and materials
- Cosmology and Gravitation Theories
- Quantum Chromodynamics and Particle Interactions
- Quantum, superfluid, helium dynamics
- High-Energy Particle Collisions Research
- Inertial Sensor and Navigation
Technical University of Munich
2021-2025
Information on the phase structure of strongly interacting matter at high baryon densities can be gained from observations neutron stars and their detailed analysis. In present work Bayesian inference methods are used to set constraints speed sound in interior stars, based recent multi-messenger data combination with limiting conditions nuclear physics low densities. Two general parametric representations introduced for $c_s$ order examine independence respect choices parametrisation Priors....
With the aim of exploring evidence for or against phase transitions in cold and dense baryonic matter, inference sound speed equation state matter neutron stars is extended view recent new observational data. The impact heavy ($2.35{M}_{\ensuremath{\bigodot}}$) black-widow pulsar PSR J0952-0607 unusually light supernova remnant HESS J1731-347 inspected. In addition, a detailed reanalysis performed low-density constraint based on chiral effective field theory perturbative QCD at...
As an update to our previously performed Bayesian inference analyses of the neutron star matter equation-of-state and related quantities, additional impact recently published NICER data PSR J0437-4751 is examined. Including mass radius distributions this pulsar in database results modest shifts from inferred median posterior values radii <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mi>R</a:mi></a:math> central densities <c:math...
Recent inference results of the sound velocity in cores neutron stars are summarized. Implications for equation state and phase structure highly compressed baryonic matter discussed. In view strong constraints imposed by heaviest known pulsars, must be very stiff order to ensure stability these extreme objects. This required stiffness limits possible appearance transitions star cores. For example, a Bayes factor analysis quantifies evidence squared velocities cs2>0.1 2.1 solar-mass...
Abstract Neutron stars provide a unique opportunity to study strongly interacting matter under extreme density conditions. The intricacies of inside neutron and their equation state are not directly visible, but determine bulk properties, such as mass radius, which affect the star's thermal X-ray emissions. However, telescope spectra these emissions also affected by stellar distance, hydrogen column, effective surface temperature, always well-constrained. Uncertainties on nuisance parameters...
Abstract The phase structure of baryonic matter is investigated with focus on the role fluctuations beyond mean-field approximation. prototype test case studied chiral nucleon-meson model, added comments quark-meson model. Applications to nuclear include liquid-gas transition. Extensions high baryon densities are performed for both and neutron matter. vacuum systematically explored. It pointed out that such tend stabilize hadronic characterized by spontaneously broken symmetry, shifting...
Neutron stars provide a unique opportunity to study strongly interacting matter under extreme density conditions. The intricacies of inside neutron and their equation state are not directly visible, but determine bulk properties, such as mass radius, which affect the star's thermal X-ray emissions. However, telescope spectra these emissions also affected by stellar distance, hydrogen column, effective surface temperature, always well-constrained. Uncertainties on nuisance parameters must be...
As an update to our previously performed Bayesian inference analyses of the neutron star matter equation-of-state and related quantities, additional impact recently published NICER data PSR J0437-4751 is examined. Including mass radius distributions this pulsar in base results modest shifts from inferred median posterior values radii $R$ central densities $n_c$ for representative $1.4\,M_\odot$ $2.1\,M_\odot$ stars: are reduced by about $0.2-0.3$ km $R_{1.4} = 12.1\pm 0.5$ $R_{2.1}...
With the aim of exploring evidence for or against phase transitions in cold and dense baryonic matter, inference sound speed equation-of-state matter neutron stars is extended view recent new observational data. The impact heavy (2.35 $M_\odot$) black widow pulsar PSR J0952-0607 unusually light supernova remnant HESS J1731-347 inspected. In addition a detailed re-analysis performed low-density constraint based on chiral effective field theory perturbative QCD at asymptotically high...
Recent inference results of the sound velocity in cores neutron stars are summarized. Implications for equation state and phase structure highly compressed baryonic matter discussed. In view strong constraints imposed by heaviest known pulsars, must be very stiff order to ensure stability these extreme objects. This required stiffness limits possible appearance transitions star cores. empirical findings, much discussed issues such as quest a transition towards restored chiral symmetry active...
Recent inference results of the sound velocity in cores neutron stars are summarized. Implications for equation state and phase structure highly compressed baryonic matter discussed. In view strong constraints imposed by heaviest known pulsars, must be very stiff order to ensure stability these extreme objects. This required stiffness limits possible appearance transitions star cores. For example, a Bayes factor analysis quantifies evidence squared velocities $c_s^2 > 0.1$ 2.1 solar-mass...
Information on the phase structure of strongly interacting matter at high baryon densities can be gained from observations neutron stars and their detailed analysis. In present work Bayesian inference methods are used to set constraints speed sound in interior stars, based recent multi-messenger data combination with limiting conditions nuclear physics low densities. Two general parametric representations introduced for $c_s$ order examine independence respect choices parametrisation Priors....