A New Constraint on the Nuclear Equation of State from Statistical Distributions of Compact Remnants of Supernovae

Meskhi, Mikhail M.; E., Wolfe, Noah; Dai, Zhenyu; Fröhlich, C.; Miller, Jonah; Wong, Raymond K. W.; Vilalta, Ricardo

doi:10.3847/2041-8213/ac7054

Cited by 7 publications

(2 citation statements)

References 46 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Our models densely cover a range of neutron star masses at and above the theoretical minimum of ∼1.4 M e but well below the largest observed neutron star mass. The mass distribution of NSs from our models is also consistent with that of isolated neutron stars observed to date (Meskhi et al 2022). We note that the large (∼15 km) radii of our neutron stars with the TM1 and the NL3 EOS are largely inconsistent with constraints on neutron star radii from GW observations of a binary neutron star merger (Abbott et al 2018) and those from X-ray observations of pulsars with NICER (Raaijmakers et al 2021), as well as with the combined constraints derived by Legred et al (2021).…”

Section: Numerical Setup and Modelssupporting

confidence: 69%

Gravitational Wave Eigenfrequencies from Neutrino-driven Core-collapse Supernovae

Wolfe,

Fröhlich,

Miller

et al. 2023

ApJ

View full text Add to dashboard Cite

Core-collapse supernovae (CCSNe) are predicted to produce gravitational waves (GWs) that may be detectable by Advanced LIGO/Virgo. These GW signals carry information from the heart of these cataclysmic events, where matter reaches nuclear densities. Recent studies have shown that it may be possible to infer the properties of the proto-neutron star (PNS) via GWs generated by hydrodynamic perturbations of the PNS. However, we lack a comprehensive understanding of how these relationships may change with the properties of CCSNe. In this work, we build a self-consistent suite of over 1000 exploding CCSNe from a grid of progenitor masses and metallicities combined with six different nuclear equations of state (EOS). Performing a linear perturbation analysis on each model, we compute the resonant GW frequencies of the PNS, and we motivate a time-agnostic method for identifying characteristic frequencies of the dominant GW emission. From this, we identify two characteristic frequencies, of the early- and late-time signal, that measure the surface gravity of the cold remnant neutron star, and simultaneously constrain the hot nuclear EOS. However, we find that the details of the CCSN model, such as the treatment of gravity or the neutrino transport, and whether it explodes, noticeably change the magnitude and evolution of the PNS eigenfrequencies.

show abstract

Section: Numerical Setup and Modelssupporting

confidence: 69%

Gravitational Wave Eigenfrequencies from Neutrino-driven Core-collapse Supernovae

Wolfe,

Fröhlich,

Miller

et al. 2023

ApJ

View full text Add to dashboard Cite

show abstract

“…Given a gravitational wave signal from the coalescence of compact objects, the identification of a sub-solar mass black hole could be complicated by "mimickers" such as sub-solar mass neutron stars or boson stars [60]. While such objects themselves would be astrophysically exotic [61][62][63] and potentially sourced from dark matter [64], it is not yet clear how well current methods of gravitational-wave data analysis will distinguish between sub-solar mass black holes and these alternatives. For example, when analyzing a low-significance sub-solar mass trigger, ref.…”

Section: Jcap11(2023)039mentioning

confidence: 99%

Too small to fail: characterizing sub-solar mass black hole mergers with gravitational waves

Wolfe,

Vitale,

Talbot

2023

J. Cosmol. Astropart. Phys.

Self Cite

View full text Add to dashboard Cite

The detection of a sub-solar mass black hole could yield dramatic new insights into the nature of dark matter and early-Universe physics, as such objects lack a traditional astrophysical formation mechanism. Gravitational waves allow for the direct measurement of compact object masses during binary mergers, and we expect the gravitational-wave signal from a low-mass coalescence to remain within the LIGO frequency band for thousands of seconds. However, it is unclear whether one can confidently measure the properties of a sub-solar mass compact object and distinguish between a sub-solar mass black hole or other exotic objects. To this end, we perform Bayesian parameter estimation on simulated gravitational-wave signals from sub-solar mass black hole mergers to explore the measurability of their source properties. We find that the LIGO/Virgo detectors during the O4 observing run would be able to confidently identify sub-solar component masses at the threshold of detectability; these events would also be well-localized on the sky and may reveal some information on their binary spin geometry. Further, next-generation detectors such as Cosmic Explorer and the Einstein Telescope will allow for precision measurement of the properties of sub-solar mass mergers and tighter constraints on their compact-object nature.

show abstract

Equations-of-state deduced form different types of black holes

2023

View full text Add to dashboard Cite

Black holes are seen as thermodynamical systems. They can be characterized by thermodynamic intensive quantities such as temperature, pressure, and extensive quantities such as entropy and energy density. In this paper, we focus on the thermodynamical properties of (a) Schwarzschild, (b) Reissner–Nordström, (c) Kerr, and (d) Kerr–Newman black holes. These allow to estimate the corresponding equations-of-state (EoS) and the squared speed of sound for each of them. The latter helps to calculate the ratio of the bulk viscosity to the shear viscosity for each of the black holes. We conclude that the resulting EoS enhances when moving from Schwarzschild to Reissner–Nordström to Kerr, and to Kerr–Newman black holes.

show abstract

A New Constraint on the Nuclear Equation of State from Statistical Distributions of Compact Remnants of Supernovae

Cited by 7 publications

References 46 publications

Gravitational Wave Eigenfrequencies from Neutrino-driven Core-collapse Supernovae

Gravitational Wave Eigenfrequencies from Neutrino-driven Core-collapse Supernovae

Too small to fail: characterizing sub-solar mass black hole mergers with gravitational waves

Equations-of-state deduced form different types of black holes

Contact Info

Product

Resources

About