13-19 May 2018
Venice, Italy
Europe/Zurich timezone
The organisers warmly thank all participants for such a lively QM2018! See you in China in 2019!

Effect of Quantum Corrections on a Realistic Nuclear Matter EoS and on Compact Star Observables

15 May 2018, 17:00
2h 40m
First floor and third floor (Palazzo del Casinò)

First floor and third floor

Palazzo del Casinò

Poster High baryon density and astrophysics Poster Session

Speaker

Gergely Gabor Barnafoldi (Wigner RCP Hungarian Academy of Sciences (HU))

Description

The accuracy of astrophysical observations regarding compact stars are
ahead of a big evolution jump thanks to instruments like NICER [1],
which will increase the accuracy of the measurements. The discovery of
gravitational waves originating from merging neutron stars in this year
(GW170817 [2]) is the first step to use gravitational waves as a probe
for extremely dense nuclear matter.

Despite these developments the masquarade problem still persists in
modeling cold superdense nuclear matter based on compact star
observables. Since many different models yield similar neutron star
parameters only high-precision measurements and theoretical reasons can
exclude models.

In this talk we present a realistic, Walecka-type model where the
bosonic fluctuations are included using the Functional Renormalization
Group (FRG) method in the Local Potential Approximation (LPA), based on
a our technique published previously [3,4]. The thermodynamical
quantities, equation of state (EoS), compressibility are calculated in
different approximations: mean field, 1st order and high order. Based
on these EoS, the properties of the corresponding neutron stars are
also calculated using the Tolman--Oppenheimer--Volkov (TOV) equations.

It is also presented, how calculating quantum corrections in different
approximations change the predicted neutron star parameters like mass,
radius and compactness. These results show, that in the light of the
new developments in astrophysical observations quantum corrections are
approaching the threshold where calculating them will be necessary for
the correct comparison between different models.

References
[1] NASA 2017, Nicer, https://www.nasa.gov/nicer
[2] Ligo/Virgo 2017, Phys. Rev. Lett., 119, 161101
[3] Barnaföldi G. G., Jakovac A., Posfay P., 2017, Phys. Rev., D95,025004
[4] Pósfay P. Barnaföldi G.G., A. Jakovác,
arXiv:1710.05410, arXiv:1610.03674

Collaboration Cost Action CA16214, PHAROS
Centralised submission by Collaboration Presenter name already specified
Content type Theory

Primary authors

Péter Pósfay (Wigner Research Centre for Physics) Antal Jakovac (Eotvos University Budapest) Gergely Gabor Barnafoldi (Wigner RCP Hungarian Academy of Sciences (HU))

Presentation Materials

Your browser is out of date!

If you are using Internet Explorer, please use Firefox, Chrome or Edge instead.

Otherwise, please update your browser to the latest version to use Indico without problems.

×