91 research outputs found
A Single Scalar Field Model of Dark Energy with Equation of State Crossing -1
In this paper we study the possibility of building models of dark energy with
equation of state across -1 and propose explicitly a model with a single scalar
field which gives rise to an equation of state larger than -1 in the past and
less than -1 at the present time, consistent with the current observations.Comment: 4 pages, 1 figure, the version accepted by JCAP, presentation
improved and references adde
Crossing of the Cosmological Constant Boundary - an Equation of State Description
The phenomenon of the dark energy transition between the quintessence regime
() and the phantom regime (), also known as the cosmological
constant boundary crossing, is analyzed in terms of the dark energy equation of
state. It is found that the dark energy equation of state in the dark energy
models which exhibit the transition is {\em implicitly} defined. The
generalizations of the the models explicitly constructed to exhibit the
transition are studied to gain insight into the mechanism of the transition. It
is found that the cancellation of the terms corresponding to the cosmological
constant boundary makes the transition possible.Comment: 8 pages, 2 figures, talk given at QFEXT'05, Barcelona, 5-9 September
200
UV stable, Lorentz-violating dark energy with transient phantom era
Phantom fields with negative kinetic energy are often plagued by the vacuum
quantum instability in the ultraviolet region. We present a Lorentz-violating
dark energy model free from this problem and show that the crossing of the
cosmological constant boundary w=-1 to the phantom equation of state is
realized before reaching a de Sitter attractor. Another interesting feature is
a peculiar time-dependence of the effective Newton's constant; the magnitude of
this effect is naturally small but may be close to experimental limits. We also
derive momentum scales of instabilities at which tachyons or ghosts appear in
the infrared region around the present Hubble scale and clarify the conditions
under which tachyonic instabilities do not spoil homogeneity of the
present/future Universe.Comment: 22 pages, 7 figures; Presentation modified substantially, results and
conclusions unchanged. Journal versio
Hessence: A New View of Quintom Dark Energy
Recently a lot of attention has been drawn to build dark energy model in
which the equation-of-state parameter can cross the phantom divide .
One of models to realize crossing the phantom divide is called quintom model,
in which two real scalar fields appears, one is a normal scalar field and the
other is a phantom-type scalar field. In this paper we propose a non-canonical
complex scalar field as the dark energy, which we dub ``hessence'', to
implement crossing the phantom divide, in a similar sense as the quintom dark
energy model. In the hessence model, the dark energy is described by a single
field with an internal degree of freedom rather than two independent real
scalar fields. However, the hessence is different from an ordinary complex
scalar field, we show that the hessence can avoid the difficulty of the Q-balls
formation which gives trouble to the spintessence model (An ordinary complex
scalar field acts as the dark energy). Furthermore, we find that, by choosing a
proper potential, the hessence could correspond to a Chaplygin gas at late
times.Comment: Latex2e, 12 pages, no figure; v2: discussions and references added,
14 pages, 3 eps figures; v3: published versio
Crossing the Phantom Divide: Theoretical Implications and Observational Status
If the dark energy equation of state parameter w(z) crosses the phantom
divide line w=-1 (or equivalently if the expression d(H^2(z))/dz - 3\Omega_m
H_0^2 (1+z)^2 changes sign) at recent redshifts, then there are two possible
cosmological implications: Either the dark energy consists of multiple
components with at least one non-canonical phantom component or general
relativity needs to be extended to a more general theory on cosmological
scales. The former possibility requires the existence of a phantom component
which has been shown to suffer from serious theoretical problems and
instabilities. Therefore, the later possibility is the simplest realistic
theoretical framework in which such a crossing can be realized. After providing
a pedagogical description of various dark energy observational probes, we use a
set of such probes (including the Gold SnIa sample, the first year SNLS
dataset, the 3-year WMAP CMB shift parameter, the SDSS baryon acoustic
oscillations peak (BAO), the X-ray gas mass fraction in clusters and the linear
growth rate of perturbations at z=0.15 as obtained from the 2dF galaxy redshift
survey) to investigate the priors required for cosmological observations to
favor crossing of the phantom divide. We find that a low \Omega_m prior
(0.2<\Omega_m <0.25) leads, for most observational probes (except of the SNLS
data), to an increased probability (mild trend) for phantom divide crossing. An
interesting degeneracy of the ISW effect in the CMB perturbation spectrum is
also pointed out.Comment: Accepted in JCAP (to appear). Comments added, typos corrected. 19
pages (revtex), 8 figures. The numerical analysis files (Mathematica +
Fortran) with instructions are available at
http://leandros.physics.uoi.gr/pdl-cross/pdl-cross.htm . The ppt file of a
relevant talk may be downloaded from
http://leandros.physics.uoi.gr/pdl-cross/pdl2006.pp
Observational Constraints on Undulant Cosmologies
In an undulant universe, cosmic expansion is characterized by alternating
periods of acceleration and deceleration. We examine cosmologies in which the
dark-energy equation of state varies periodically with the number of e-foldings
of the scale factor of the universe, and use observations to constrain the
frequency of oscillation. We find a tension between a forceful response to the
cosmic coincidence problem and the standard treatment of structure formation.Comment: 19 pages, 12 figures in 19 files, uses iopart.cls, iopart10.clo;
added reference
Reconstructing large running-index inflaton potentials
Recent fits of cosmological parameters by the first year Wilkinson Microwave
Anisotropy Probe (WMAP) measurement seem to favor a primordial scalar spectrum
with a large varying index from blue to red. We use the inflationary flow
equations to reconstruct large running-index inflaton potentials and comment on
current status on the inflationary flow. We find previous negligence of higher
order slow rolling contributions when using the flow equations would lead to
unprecise results.Comment: Final version to appear in Class. Quant. Grav. References adde
Cosmology with Interaction between Phantom Dark Energy and Dark Matter and the Coincidence Problem
We study a cosmological model in which phantom dark energy is coupled to dark
matter by phenomenologically introducing a coupled term to the equations of
motion of dark energy and dark matter. This term is parameterized by a
dimensionless coupling function , Hubble parameter and the energy
density of dark matter, and it describes an energy flow between the dark energy
and dark matter. We discuss two cases: one is the case where the
equation-of-state of the dark energy is a constant; the other is
that the dimensionless coupling function is a constant. We investigate
the effect of the interaction on the evolution of the universe, the total
lifetime of the universe, and the ratio of the period when the universe is in
the coincidence state to its total lifetime. It turns out that the interaction
will produce significant deviation from the case without the interaction.Comment: Latex, 17 pages including 14 figures, minor change
Cosmological Evolution of Interacting Phantom Energy with Dark Matter
We investigate the cosmological evolution of an interacting phantom energy
model in which the phantom field has interaction with the dark matter. We
discuss the existence and stability of scaling solutions for two types of
specific interactions. One is motivated by the conformal transformation in
string theory and the other is motivated by analogy with dissipation. In the
former case, there exist no scaling solutions. In the latter case, there exist
stable scaling solutions, which may give a phenomenological solution of the
coincidence problem. Furthermore, the universe either accelerates forever or
ends with a singularity, which is determined by not only the model parameters
but also the initial velocity of the phantom field.Comment: 7 pages, 11 figures, RevTe
SO(1,1) dark energy model and the universe transition
We suggest a scalar model of dark energy with the SO(1,1) symmetry. The model
may be reformulated in terms of a real scalar field and the scale factor
so that the Lagrangian may be decomposed as that of the real quintessence
model plus the negative coupling energy term of to . The existence of
the coupling term leads to a wider range of and overcomes the
problem of negative kinetic energy in the phantom universe model. We propose a
power-law expansion model of univese with time-dependent power, which can
describe the phantom universe and the universe transition from ordinary
acceleration to super acceleration.Comment: 12 pages. submitted to CQ
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