Effects of friction on cosmic strings

Garriga, Jaume; Sakellariadou, Mairi

doi:10.1103/physrevd.48.2502

Cited by 72 publications

(102 citation statements)

References 17 publications

Supporting

Mentioning

101

Contrasting

Order By: Relevance

“…One is phase transition involving violent processes like bubble collision [9,10,11] or the collapse of string loops [12,13,14,15]. As we will see in the next section, however, both scenarios have difficulties.…”

Section: Introductionmentioning

confidence: 99%

“…There are several ways to realize large density fluctuations leading to the PBH formation. One is the phase transition which leads to violent processes like bubble collision [9,10,11] or the collapse of string loops [12,13,14,2 As pointed out in Ref. [29], the Bondi solution becomes invalid for the PBH of mass M BH > ∼ 10 4 M ⊙ .…”

Section: Pbh Formation and Observational Constraintsmentioning

confidence: 99%

See 1 more Smart Citation

Primordial black holes as all dark matter

Frampton

Kawasaki

Takahashi

et al. 2010

J. Cosmol. Astropart. Phys.

221

188

View full text Add to dashboard Cite

We argue that a primordial black hole is a natural and unique candidate for all dark matter. We show that, in a smooth-hybrid new double inflation model, a right amount of the primordial black holes, with a sharply-defined mass, can be produced at the end of the smooth-hybrid regime, through preheating. We first consider masses < 10 −7 M ⊙ which are allowed by all the previous constraints. We next discuss much heavier mass 10 5 M ⊙ hinted at by entropy, and galactic size evolution, arguments. Effects on the running of the scalar spectral index are computed.

show abstract

Section: Introductionmentioning

confidence: 99%

Section: Pbh Formation and Observational Constraintsmentioning

confidence: 99%

Primordial black holes as all dark matter

Frampton

Kawasaki

Takahashi

et al. 2010

J. Cosmol. Astropart. Phys.

221

188

View full text Add to dashboard Cite

show abstract

“…In this case, the probability of PBH formation at a given epoch is determined by the nature and evolution of the perturbations. (3) The collapse of cosmic string loops (Caldwell & Casper 1996;Garriga & Sakellariadou 1993;Hawking 1989;Polnarev & Zembowicz 1991;MacGibbon et al 1998). Due to frequent collisions and reconnections, cosmic strings may occasionally form loops compact enough that the loop is within its Schwarzschild radius in every dimension.…”

Section: Primordial Black Hole Productionmentioning

confidence: 99%

Growth of Structure Seeded by Primordial Black Holes

Mack

Ostriker

Ricotti

2007

ApJ

153

187

View full text Add to dashboard Cite

We discuss the possibilities for the growth of primordial black holes (PBHs) via the accretion of dark matter. In agreement with previous works, we find that accretion during the radiation-dominated era does not lead to a significant mass increase. However, during matter domination, PBHs may grow by up to 2 orders of magnitude in mass through the acquisition of large dark matter halos. We discuss the possibility of PBHs being an important component in dark matter halos of galaxies, as well as their potential to explain the ultraluminous X-ray sources (ULXs) observed in nearby galactic disks. We point out that although PBHs are ruled out as the dominant component of dark matter, there is still a great deal of parameter space that is open to their playing a role in the modern-day universe. For example, a primordial halo population of PBHs each at 10 2.5 M , making up 0.1% of the dark matter, grows to 10 4.5 M via the accumulation of dark matter halos and accounts for $10% of the dark matter mass by a redshift of z % 30. These intermediate-mass black holes may then ''light up'' when passing through molecular clouds, becoming visible as ULXs at the present day, or they may form the seeds for supermassive black holes at the centers of galaxies.

show abstract

“…We have apparently neglected to consider the loops formed along with the long strings at the time of the cosmological phase transition. These loops, as has been recently shown in [18], may be smoothed by the friction with the cosmological fluid [25]. The loops most smoothed by the friction, however, have Schwarzschild radii smaller than the string thickness; these loops will not collapse to form black holes.…”

Section: Production and Evolution Of Black Holes From The Collapmentioning

confidence: 79%

“…The work of Garriga and Vilenkin [18] considered nucleated cosmic string loops, which may collapse to form black holes. The behavior of classical fluctuations on the loops were examined, and it was shown that while transverse perturbations maintain constant amplitude as the cosmic string loop contracts, radial perturbations shrink by a factor of the perturbation mode number.…”

Section: Collapse Of Cosmic String Loopsmentioning

confidence: 99%

Constraints on cosmic strings due to black holes formed from collapsed cosmic string loops

Caldwell

Gates

1993

Phys. Rev. D

View full text Add to dashboard Cite

The cosmological features of primordial black holes formed from collapsed cosmic string loops are studied. Observational restrictions on a population of primordial black holes are used to restrict f , the fraction of cosmic string loops which collapse to form black holes, and µ, the cosmic string mass-per-unit-length. Using a realistic model of cosmic strings, we find the strongest restriction on the parameters f and µ is due to the energy density in 100M eV photons radiated by the black holes. We also find that inert black hole remnants cannot serve as the dark matter. If earlier, crude estimates of f are reliable, our results severely restrict µ, and therefore limit the viability of the cosmic string large-scale structure scenario. 0 I. IntroductionThe cosmic string scenario for the formation of large scale structure has many observable features. Primarily, cosmic strings may serve to produce perturbations to the cosmological fluid of the necessary magnitude and distribution to seed the formation of galaxies and clusters, as observed today. Cosmic strings leave an observational signature through these perturbations, as well as through the emission of gravitational radiation. Broadly, then, there are two areas of cosmic string research. These are studies of the large-scale structure produced by cosmic strings, and tests of the compatibility of cosmic strings with cosmological observations. Such tests focus, for example, on the anisotropies produced by cosmic strings in the microwave background and the noise in pulsar timing due to the cosmic string stochastic gravitational wave background. Ultimately, the test of compatibility results in a restriction on µ, the mass-per-unit-length and sole free parameter in the cosmic string model. In this report, we will examine the restrictions on black holes formed from collapsed cosmic string loops.It is well known that a sufficiently smooth, circular cosmic string loop may collapse to form a black hole [1,2,3,4,5]. During the evolution of a network of cosmic strings, some cosmic string loops may collapse to form black holes. In this case, the observational restrictions on a population of primordial black holes may be used to restrict such a cosmic string scenario.The study of primordial black holes has been vigorously carried out in, for example, [6,7,8,9,10,11,12]. We will take advantage of this work in applying constraints to a population of black holes formed from collapsed cosmic string loops. In turn, we will place restrictions on the cosmic string network. In this paper, we will find observational restrictions on the cosmic string scenario from cosmic string loops which collapse to form black holes.The organization of this paper is as follows. In section II we will summarize previous efforts to estimate the fraction f of cosmic string loops which collapse to form black holes. In section III we will present the models of cosmic strings and black hole evaporation used to calculate the energy density in black holes and black hole radiation. In section IV we wil...

show abstract

Effects of friction on cosmic strings

Cited by 72 publications

References 17 publications

Primordial black holes as all dark matter

Primordial black holes as all dark matter

Growth of Structure Seeded by Primordial Black Holes

Constraints on cosmic strings due to black holes formed from collapsed cosmic string loops

Contact Info

Product

Resources

About