scholarly journals The large-mass limit of cloudy black holes

2015 ◽  
Vol 32 (13) ◽  
pp. 134002 ◽  
Author(s):  
Shahar Hod
Keyword(s):  
Black Holes ◽  
Large Mass ◽  
Mass Limit

scholarly journals FUNCTIONAL BOSONIZATION OF NONRELATIVISTIC FERMIONS IN 2+1 DIMENSIONS

2000 ◽  
Vol 15 (29) ◽  
pp. 4655-4679 ◽  
Author(s):  
DANIEL G. BARCI ◽  
C. A. LINHARES ◽  
A. F. DE QUEIROZ ◽  
J. F. MEDEIROS NETO
Keyword(s):  
Transverse Electric ◽  
Gaussian Approximation ◽  
Large Mass ◽  
Dispersion Relations ◽  
Collective Excitations ◽  
Nonlinear Dispersion ◽  
Mass Limit ◽  
Linear Dispersion ◽  
Density Maps ◽  
Fermionic Systems

We analyze the universality of the bosonization rules in nonrelativistic fermionic systems in (2+1)d. We show that, in the case of linear fermionic dispersion relations, a general fermionic theory can be mapped into a gauge theory in such a way that the fermionic density maps into a magnetic flux and the fermionic current maps into a transverse electric field. These are universal rules in the sense that they remain valid whatever the interaction considered. We also show that these rules are universal in the case of nonlinear dispersion relations provided we consider only density–density interactions. We apply the functional bosonization formalism to a nonrelativistic and nonlocal massive Thirring-like model and evaluate the spectrum of collective excitations in several limits. In the large mass limit, we are able to exactly calculate this spectrum for arbitrary density–density and current–current interactions. We also analyze the massless case and show that it has no collective excitations for any density–density potential in the Gaussian approximation. Moreover, the presence of current interactions may induce a gapless mode with a linear dispersion relation.

scholarly journals Can the graviton have a large mass near black holes?

2018 ◽  
Vol 97 (8) ◽  
Author(s):  
Jun Zhang ◽  
Shuang-Yong Zhou
Keyword(s):  
Black Holes ◽  
Large Mass

scholarly journals A higher-multipole gravitational waveform model for an eccentric binary black holes based on the effective-one-body-numerical-relativity formalism

2021 ◽  
Author(s):  
Xiaolin Liu ◽  
Zhoujian Cao ◽  
Zong-Hong Zhu
Keyword(s):  
Black Holes ◽  
Inclination Angle ◽  
Source Localization ◽  
Numerical Relativity ◽  
Large Mass ◽  
Reference Frequency ◽  
Binary Black Holes ◽  
Higher Modes ◽  
Minimal Matching ◽  
Initial Orbit

Abstract We have previously constructed a waveform model, SEOBNRE, for spinning binary black hole moving along eccentric orbit based on effective-one-body (EOB) formalism. In the current paper, we update SEOBNRE waveform model in the following three respects. Firstly, we update the EOB dynamics from SEOBNRv1 to SEOBNRv4. Secondly we properly treat the Schott term which has been ignored in previous SEOBNRE. Thirdly, we construct a new factorized waveform including (l,|m|)=(2,2),(2,1),(3,3),(4,4) modes based on effective-one-body (EOB) formalism, which is valid for spinning binary black holes (BBH) in general equatorial orbit. Following our previous SEOBNRE waveform model, we call our new waveform model SEOBNREHM. The (l,|m|)=(2,2) mode waveform of SEOBNREHM can fit the original SEOBNRv4 waveform very well in the case of a quasi-circular orbit. We have validated SEOBNREHM waveform model through comparing the waveform against the Simulating eXtreme Spacetimes (SXS) catalog. The comparison is done for BBH with total mass in (20,200)M_sun using Advanced LIGO designed sensitivity. For the quasi-circular cases we have compared our (2,2) mode waveforms to the 281 numerical relativity (NR) simulations of BBH along quasi-circular orbits. All of the matching factors are bigger than 98\%. For the elliptical cases, 24 numerical relativity simulations of BBH along an elliptic orbit are used. For each elliptical BBH system, we compare our modeled gravitational polarizations against the NR results for different combinations of the inclination angle, the initial orbit phase and the source localization in the sky. We use the minimal matching factor respect to the inclination angle, the initial orbit phase and the source localization to quantify the performance of the higher modes waveform. We found that after introducing the higher modes, the minimum of the minimal matching factor among the 24 tested elliptical BBHs increases from 90\% to 98\%. Our SEOBNREHM waveform model can match all tested 305 SXS waveforms better than 98\% including highly spinning ($\chi=0.99$) BBH, highly eccentric ($e\approx0.6$ at reference frequency $Mf_0=0.002$) BBH and large mass ratio ($q=10$) BBH.

scholarly journals Casimir energy calculation for massive scalar field on spherical surfaces: an alternative approach

2018 ◽  
Vol 96 (9) ◽  
pp. 1004-1009 ◽  
Author(s):  
M.A. Valuyan
Keyword(s):  
Scalar Field ◽  
Spherical Surface ◽  
Original System ◽  
Large Mass ◽  
Casimir Energy ◽  
Energy Calculation ◽  
Massive Scalar ◽  
Mass Limit ◽  
Massive Scalar Field ◽  
Spherical Surfaces

In this study, the Casimir energy for massive scalar field with periodic boundary condition was calculated on spherical surfaces with S1, S2, and S3 topologies. To obtain the Casimir energy on a spherical surface, the contribution of the vacuum energy of Minkowski space is usually subtracted from that of the original system. In the large mass limit for surface S2, however, some divergences would eventually remain in the obtained result. To remove these remaining divergences, a secondary renormalization program was manually performed. In the present work, a direct approach for calculation of the Casimir energy has been introduced. In this approach, two similar configurations were considered and then the vacuum energies of these configurations were subtracted from each other. This method provides more physical meaning than the other common methods. Additionally, in the large mass limit for surface S2, it provides a situation in which the second renormalization program is automatically conducted in the calculation procedure, and there was no longer a need to do so manually. Finally, by plotting the obtained values for the Casimir energy of the topologies and investigating their appropriate limits, the logic agreement between the results of our scheme and those of previous studies was discussed.

scholarly journals Primordial black holes and the origin of the matter–antimatter asymmetry

2019 ◽  
Vol 377 (2161) ◽  
pp. 20190091 ◽  
Author(s):  
Juan García-Bellido
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Dark Matter ◽  
Cold Dark Matter ◽  
Hot Spot ◽  
Large Mass ◽  
New Physics ◽  
Primordial Black Holes ◽  
Far From Equilibrium ◽  
The Universe

We review here a new scenario of hot spot electroweak baryogenesis where the local energy released in the gravitational collapse to form primordial black holes (PBHs) at the quark-hadron (QCD) epoch drives over-the-barrier sphaleron transitions in a far from equilibrium environment with just the standard model CP violation. Baryons are efficiently produced in relativistic collisions around the black holes and soon redistribute to the rest of the universe, generating the observed matter–antimatter asymmetry well before primordial nucleosynthesis. Therefore, in this scenario there is a common origin of both the dark matter to baryon ratio and the photon to baryon ratio. Moreover, the sudden drop in radiation pressure of relativistic matter at H 0 / W ± / Z 0 decoupling, the QCD transition and e + e − annihilation enhances the probability of PBH formation, inducing a multi-modal broad mass distribution with characteristic peaks at 10 −6 , 1, 30 and 10 6   M ⊙ , rapidly falling at smaller and larger masses, which may explain the LIGO–Virgo black hole mergers as well as the OGLE-GAIA microlensing events, while constituting all of the cold dark matter today. We predict the future detection of binary black hole (BBH) mergers in LIGO with masses between 1 and 5  M ⊙ , as well as above 80  M ⊙ , with very large mass ratios. Next generation gravitational wave and microlensing experiments will be able to test this scenario thoroughly. This article is part of a discussion meeting issue ‘Topological avatars of new physics’.

scholarly journals HAWKING RADIATION: A PARTICLE PHYSICS PERSPECTIVE

1993 ◽  
Vol 08 (18) ◽  
pp. 1661-1670 ◽  
Author(s):  
MATT VISSER
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Decay Rate ◽  
Hawking Radiation ◽  
Particle Physics ◽  
Naked Singularity ◽  
Black Body ◽  
Large Mass ◽  
High Energy ◽  
Radiation Process

It has recently become fashionable to regard black holes as elementary particles. By taking this suggestion reasonably seriously it is possible to cobble together an elementary particle physics based on estimate for the decay rate (black hole) i → (black hole) f+ (massless quantum) . This estimate of the spontaneous emission rate contains two free parameters which may be fixed by demanding that the high energy end of the spectrum of emitted quanta match a black body spectrum at the Hawking temperature. The calculation, though technically trivial, has important conceptual implications: (1) The existence of Hawking radiation from black holes seems ultimately dependent only on the fact that massless quanta (and all other forms of matter) couple to gravity. (2) The essentially thermal nature of the Hawking spectrum seems to depend only on the fact that the number of internal states of a large mass black hole is enormous. (3) Remarkably, the resulting formula for the decay rate gives meaningful answers even when extrapolated to low mass black holes. The analysis seems to support the scenario of complete evaporation as the end point of the Hawking radiation process (no naked singularity, no stable massive remnant).

scholarly journals The Hierarchy Principle and the Large Mass Limit of the Linear Sigma Model

2007 ◽  
Vol 46 (10) ◽  
pp. 2560-2590 ◽  
Author(s):  
D. Bettinelli ◽  
R. Ferrari ◽  
A. Quadri
Keyword(s):  
Sigma Model ◽  
Large Mass ◽  
Linear Sigma Model ◽  
Mass Limit

scholarly journals Chern-Simons theory as the large-mass limit of topologically massive Yang-Mills theory

1992 ◽  
Vol 381 (1-2) ◽  
pp. 222-280 ◽  
Author(s):  
G. Giavarini ◽  
C.P. Martin ◽  
F. Ruiz Ruiz
Keyword(s):  
Large Mass ◽  
Simons Theory ◽  
Mass Limit ◽  
Yang Mills ◽  
Chern Simons ◽  
Chern Simons Theory

scholarly journals Maximum baryon masses for static neutron stars in f(R) gravity

2021 ◽  
Author(s):  
A. V. Astashenok ◽  
Salvatore Capozziello ◽  
Sergei D. Odintsov ◽  
Vasilis K. Oikonomou
Keyword(s):  
Black Holes ◽  
Neutron Star ◽  
Neutron Stars ◽  
Equations Of State ◽  
Gravitational Mass ◽  
Mass Limit ◽  
Mass Gap ◽  
Baryon Mass ◽  
Baryonic Mass ◽  
Lower Limits

Abstract We investigate the upper mass limit predictions of the baryonic mass for static neutron stars in the context of f(R) gravity. We use the most popular f(R) gravity model, namely the R2gravity, and calculate the maximum baryon mass of static neutron stars adopting several realistic equations of state and one ideal equation of state, namely that of causal limit. Our motivation is based on the fact that neutron stars with baryon masses larger than the maximum mass for static neutron star configurations inevitably collapse to black holes. Thus with our analysis, we want further to enlighten the predictions for the maximum baryon masses of static neutron stars in R2gravity, which, in turn, further strengthens our understanding of the mysterious mass-gap region. As we show, the baryon masses of most of the equations of states studied in this paper, lie in the lower limits of the mass-gap region M ∼ 2.5 − 5M⊙, but intriguingly enough, the highest value of the maximum baryon masses we found is of the order of M ∼ 3M⊙. This upper mass limit also appears as a maximum static neutron star gravitational mass limit in other contexts. Combining the two results which refer to baryon and gravitational masses, we point out that the gravitational mass of static neutron stars cannot be larger than three solar masses, while based on maximum baryon masses results of the present work, we can conspicuously state that it is highly likely the lower mass limits of astrophysical black holes in the range of M ∼ 2.5 − 3M⊙. This, in turn, implies that maximum neutron star masses in the context of R2gravity are likely to be in the lower limits of the range of M ∼ 2.4 − 3M⊙.

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