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Show that it is possible to derive constraints in the presence of cosmic strings during the quark–hadron transition.
The new constraints are remarkably close to those derived from the normalization of the cosmic string model to the cosmic microwave background anisotropies. Introduction cosmic strings (cs) are linear topological defects that are believed to originate during phase.
Dec 2, 2019 a small fraction, $f$, of cosmic string loops can collapse to form primordial black holes (pbhs).
The constraints we obtained are the most stringent to date for some regions of the cosmic string parameter space. This new result places limits on physical models of cosmic strings and could be used to generate more accurate simulations of a string network.
Corrections to the ionization fraction of neutral hydrogen induced by cosmic strings lead to new constraints on the string tension around gμ∼10−16–10−20 for values of the primordial.
Constraints on cosmic strings due to black holes formed from collapsed cosmic string loops phys rev d part fields 1993 sep 15;48(6):2581-2586.
We reexamine the constraints on the cosmic string tension from cosmic microwave background (cmb) and matter power spectra, and also from limits on a stochastic background of gravitational waves provided by pulsar timing. We discuss the different approaches to modeling string evolution and radiation. In particular, we show that the unconnected segment model can describe cmb spectra expected.
Feb 5, 2012 cosmic strings consist of trapped regions of false vacuum in u(1) constraint systems appear whenever a theory has gauge symmetry, on the left hand side we observe a difference due to the consequence of the eμν term.
Note that we have assumed all cosmic strings to be superconducting and the currents through the string loops following the exponential distribution. We put forward a model in which the number density for scss can be defined in terms of the number density for cosmic strings and the distribution of strings’ currents.
This process may lead to the creation of cosmic strings these are one-dimensional topological defects, the energy of which is concentrated along a line. Cosmic strings are analogous to the cracks which can appear in ice as the water freezes.
Constraints on the tension and the abundance of cosmic strings depend crucially on the rate at which they decay into particles and gravitational radiation. We study the decay of cosmic string loops in the abelian-higgs model by performing field theory simulations of loop formation and evolution.
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 mu, the cosmic string mass-per-unit length. Using a realistic model of cosmic strings, we find the strongest restriction.
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 that the energy density.
Constraints on cosmic strings -philosophy • there is significant uncertainty: due to lack of detailed understanding of string networks - observers/experimentalists are conservative - they don’t like theories that moving targets • cmb: sensitive mainly to string density - talk by adam moss - factor of 2-3 discrepancy.
Constraints on the cosmic string scenario from the large-scale distribution of 'large-scale structures and streaming velocities due to open cosmic strings',.
Due to zel'dovich' and vilenkin: is based on the assumption that, in a radiation dominated universe constraint on the cosmic string theory of galaxy formation.
Title: constraints on cosmic strings due to black holes formed from collapsed cosmic string loops.
A network of cosmic strings would lead to gravitational waves which may be detected by pulsar timing or future interferometers.
Some string theory models propose that strings could have grown to colossal proportions during the initial rapid expansion of the cosmos. Differences in the tension of these kinds of cosmic strings and in how string loops break away would create a unique gravitational-wave signature distinguishing them from other kinds.
Of the cosmic microwave background anisotropy with remarkable precision. The same data put tight limits on other sources of anisotropy. Cosmic strings are a particularly interesting alternate source to constrain. Strings are topological defects, remnants of in ationary-era physics that persist after the big bang.
This paper is aimed at setting observational limits to the number of cosmic strings (nambu–goto, abelian-higgs, semilocal) and other topological defects (textures). Radio maps of cmb anisotropy, provided by the space mission planck for various frequencies, were filtered and then processed by the method of convolution with modified haar functions (mhf) to search for cosmic string candidates.
Constraints on cosmic strings due to black holes formed from collapsed cosmic string loops by r r caldwell and e gates.
A cosmic string is a very long (possibly as long as the diameter of the visible universe), very thin cosmic strings also lead to more exotic phenomena. Observational limits from galaxy distribution have found no signature of their.
Cosmic strings are topological defects which can be formed in gut-scale phase transitions in the early universe. They are also predicted to form in the context of string theory.
This process may lead to the creation of cosmic strings: these are one- dimensional.
Apr 4, 2014 cosmic strings can give rise to a large variety of interesting astrophysical phenomena.
Jan 14, 2013 in fact, current limits on cosmic strings already [8] pro- vide a constraint secondly, cos- mic strings lead to perturbations which are highly non-.
In string theory, the role of cosmic strings can be played by the fundamental strings (or f-strings) themselves that define the theory perturbatively, by d-strings which are related to the f-strings by weak-strong or so called s-duality, or higher-dimensional d-, ns- or m-branes that are partially wrapped on compact cycles associated to extra spacetime.
The details of the spectrum of gravitational radiation due to cosmic strings has been previously considered elsewhere8. Here we bene t from recent work9, which suggests that the e ect of the radiative back-reaction on a string loop is to damp out the higher oscillation modes.
Cosmic strings are topological defects which can be formed in grand unified theory scale phase transitions in the early universe.
May 20, 2019 constraints on the tension and the abundance of cosmic strings depend crucially on the rate at which they decay into particles and gravitational.
The observational restrictions on the cosmic string scenario for the formation of large scale structure are evaluated. These restrictions are due to the spectrum of gravitational radiation emitted by oscillating string loops, anisotropies in the cosmic microwave background caused by the strings, and evaporating black holes formed from collapsed cosmic string loops.
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