Charge and pH effects on inhibitor performance

Malik, Hassan

doi:10.1108/00035590110410227

Cited by 6 publications

(8 citation statements)

References 11 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…A gauge-invariant theory of linear perturbations about FRW metric was proposed by Bardeen [11] and subsequently developed by many authors (for example, see [12][13][14][15][16]). No such gaugeinvariant formalism has been developed for nonlinear cosmological perturbations 3 .…”

Section: Gauge Choices and Gauge-invariant Variablesmentioning

confidence: 99%

“…We draw a distinction here between quantities that are automatically gauge independent, i.e., those that have no gauge dependence (such as perturbations about a constant scalar field), and quantities that are in general gauge dependent (such as the curvature perturbation) but can have a gauge-invariant definition once their gauge dependence is fixed (such as the curvature perturbation on uniform-density hypersurfaces). Although this approach has been widely used, at least implicitly, to construct gauge-invariant quantities at first order [3,13], it has not been previously used at higher order. In this letter, we show that it is possible to define gauge-invariant quantities at second order corresponding to physical perturbations.…”

Section: Gauge Choices and Gauge-invariant Variablesmentioning

confidence: 99%

See 1 more Smart Citation

Evolution of second-order cosmological perturbations

Malik

Wands

2004

Class. Quantum Grav.

168

279

View full text Add to dashboard Cite

We present a method for constructing gauge-invariant cosmological perturbations which are gaugeinvariant up to second order. As an example we give the gauge-invariant definition of the second order curvature perturbation on uniform density hypersurfaces. Using only the energy conservation equation we show that this curvature perturbation is conserved at second order on large scales for adiabatic perturbations.

show abstract

Section: Gauge Choices and Gauge-invariant Variablesmentioning

confidence: 99%

Section: Gauge Choices and Gauge-invariant Variablesmentioning

confidence: 99%

Evolution of second-order cosmological perturbations

Malik

Wands

2004

Class. Quantum Grav.

168

279

View full text Add to dashboard Cite

show abstract

“…For a definition of R in terms of the metric perturbations and its relation to curvature perturbations defined on different hypersurfaces see for example [26]. On sub-horizon scales therefore…”

Section: Jcap03(2007)010mentioning

confidence: 99%

Constraints on the primordial curvature perturbation from primordial black holes

Zaballa

Green

Malik

et al. 2007

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

We calculate the constraints on the primordial curvature perturbation at the end of inflation from the present day abundance of Primordial Black Holes (PBHs), as a function of the reheat temperature TRH. We first extend recent work on the formation of PBHs on scales which remain within the horizon during inflation and calculate the resulting constraints on the curvature perturbation. We then evaluate the constraint from PBHs that form, more conventionally, from super-horizon perturbations. The constraints apply for TRH < 10 8 GeV and the inclusion of sub-horizon PBHs leads to a limit which is roughly three times tighter than the bound from super-horizon PBHs.

show abstract

“…(The vorticity vanishes for a hypersurface orthogonal vector field.) For the metric (10) we find [27,28]…”

Section: Scalar Metric Perturbationsmentioning

confidence: 99%

Cosmological matching conditions

Copeland

Wands

2007

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

We investigate the evolution of scalar metric perturbations across a sudden cosmological transition, allowing for an inhomogeneous surface stress at the transition leading to a discontinuity in the local expansion rate, such as might be expected in a big crunch/big bang event. We assume that the transition occurs when some function of local matter variables reaches a critical value, and that the surface stress is also a function of local matter variables. In particular we consider the case of a single scalar field and show that a necessary condition for the surface stress tensor to be perturbed at the transition is the presence of a non-zero intrinsic entropy perturbation of the scalar field. We present the matching conditions in terms of gauge-invariant variables assuming a sudden transition to a fluid-dominated universe with barotropic equation of state. For adiabatic perturbations the comoving curvature perturbation is continuous at the transition, while the Newtonian potential may be discontinuous if there is a discontinuity in the background Hubble expansion.

show abstract

Charge and pH effects on inhibitor performance

Cited by 6 publications

References 11 publications

Evolution of second-order cosmological perturbations

Evolution of second-order cosmological perturbations

Constraints on the primordial curvature perturbation from primordial black holes

Cosmological matching conditions

Contact Info

Product

Resources

About