4,867 research outputs found
Dynamical radion superfield in 5D action
We derive 5D N=1 superspace action including the radion superfield. The
radion is treated as a dynamical field and identified as a solution of the
equation of motion even in the presence of the radius stabilization mechanism.
Our derivation is systematic and based on the superconformal formulation of 5D
supergravity. We can read off the couplings of the dynamical radion superfield
to the matter superfields from our result. The correct radion mass can be
obtained by calculating the radion potential from our superspace action.Comment: 29 pages, no figures, LaTeX, some comments adde
Numerical Study of Velocity Statistics in Steady Counterflow Quantum Turbulence
We investigate the velocity statistics by calculating the Biot--Savart
velocity induced by vortex filaments in steady counterflow turbulence
investigated in a previous study [Phys. Rev. B {\bf 81}, 104511 (2010)]. The
probability density function (PDF) obeys a Gaussian distribution in the
low-velocity region and a power-law distribution in the high-velocity
region. This transition between the two distributions occur at the velocity
characterized by the mean inter-vortex distance. Counterflow turbulence causes
anisotropy of the vortex tangle, which leads to a difference in the PDF for the
velocities perpendicular to and parallel to the counterflow.Comment: 4 pages, 7 figure
A model for the infrared dust emission from forming galaxies
In the early epoch of galaxy evolution, dust is only supplied by supernovae
(SNe). With the aid of a new physical model of dust production by SNe developed
by Nozawa et al. (2003) (N03), we constructed a model of dust emission from
forming galaxies on the basis of the theoretical framework of Takeuchi et al.
(2003) (T03). N03 showed that the produced dust species depends strongly on the
mixing within SNe. We treated both unmixed and mixed cases and calculated the
infrared (IR) spectral energy distribution (SED) of forming galaxies for both
cases. Our model SED is less luminous than the SED of T03 model by a factor of
2-3. The difference is due to our improved treatment of UV photon absorption
cross section, as well as different grain size and species newly adopted in
this work. The SED for the unmixed case is found to have an enhanced near to
mid-IR (N-MIR) continuum radiation in its early phase of the evolution (age <
10^{7.25} yr) compared with that for the mixed case. The strong N--MIR
continuum is due to the emission from Si grains, which only exist in the
species of the unmixed dust production. We also calculated the IR extinction
curves for forming galaxies. Then we calculated the SED of a local starbursting
dwarf galaxy SBS 0335-052. Our present model SED naturally reproduced the
strong N--MIR continuum and the lack of cold FIR emission of SBS 0335-052. We
found that only the SED of unmixed case can reproduce the NIR continuum of this
galaxy. We then made a prediction for the SED of another typical star-forming
dwarf, I Zw 18. We also presented the evolution of the SED of LBGs. Finally, we
discussed the possibility of observing forming galaxies at z > 5.Comment: MNRAS, in press. 18 pages, 15 figures. Abstract abridge
Infrared Spectral Energy Distribution Model for Extremely Young Galaxies
The small grain sizes produced by Type II supernova (SN II) models in young,
metal-poor galaxies make the appearance of their infrared (IR) spectral energy
distribution (SED) quite different from that of nearby, older galaxies. To
study this effect, we have developed a model for the evolution of dust content
and the IR SED of low-metallicity, extremely young galaxies based on Hirashita
et al. (2002). We find that, even in the intense ultraviolet (UV) radiation
field of very young galaxies, small silicate grains are subject to stochastic
heating resulting in a broad temperature distribution and substantial MIR
continuum emission. Larger carbonaceous grains are in thermal equilibrium at T
\simeq 50 - 100K, and they also contribute to the MIR. We present the evolution
of SEDs and IR extinction of very young, low-metallicity galaxies. The IR
extinction curve is also shown. In the first few Myrs, the emission peaks at
\lambda \sim 30-50um at later times dust self-absorption decreases the apparent
grain temperatures, shifting the bulk of the emission into the submillimetre
band. We successfully apply the model to the IR SED of a low metallicity (1/41
Z_\odot) dwarf galaxy SBS0335-052. We find the SED, optical properties and
extinction of the star forming region to be consistent with a very young and
compact starburst. We also predict the SED of another extremely low-metallicity
galaxy, I Zw 18, for future observational tests. Some prospects for future
observations are discussed.Comment: MNRAS in press, pages, 6 figures, using mn2e.cls. Abstract abridge
Open String on Symmetric Product
We develop some basic properties of the open string on the symmetric product
which is supposed to describe the open string field theory in discrete
lightcone quantization (DLCQ). After preparing the consistency conditions of
the twisted boundary conditions for Annulus/M\"obius/Klein Bottle amplitudes in
generic non-abelian orbifold, we classify the most general solutions of the
constraints when the discrete group is . We calculate the corresponding
orbifold amplitudes from two viewpoints -- from the boundary state formalism
and from the trace over the open string Hilbert space. It is shown that the
topology of the world sheet for the short string and that of the long string in
general do not coincide. For example the annulus sector for the short string
contains all the sectors (torus, annulus, Klein bottle, M\"obius strip) of the
long strings. The boundary/cross-cap states of the short strings are classified
into three categories in terms of the long string, the ordinary boundary and
the cross-cap states, and the ``joint'' state which describes the connection of
two short strings. We show that the sum of the all possible boundary conditions
is equal to the exponential of the sum of the irreducible amplitude -- one body
amplitude of long open (closed) strings. This is typical structure of DLCQ
partition function. We examined that the tadpole cancellation condition in our
language and derived the well-known gauge group .Comment: 56 pages, 11 figures, Late
Winding Number in String Field Theory
Motivated by the similarity between cubic string field theory (CSFT) and the
Chern-Simons theory in three dimensions, we study the possibility of
interpreting N=(\pi^2/3)\int(U Q_B U^{-1})^3 as a kind of winding number in
CSFT taking quantized values. In particular, we focus on the expression of N as
the integration of a BRST-exact quantity, N=\int Q_B A, which vanishes
identically in naive treatments. For realizing non-trivial N, we need a
regularization for divergences from the zero eigenvalue of the operator K in
the KBc algebra. This regularization must at same time violate the
BRST-exactness of the integrand of N. By adopting the regularization of
shifting K by a positive infinitesimal, we obtain the desired value
N[(U_tv)^{\pm 1}]=\mp 1 for U_tv corresponding to the tachyon vacuum. However,
we find that N[(U_tv)^{\pm 2}] differs from \mp 2, the value expected from the
additive law of N. This result may be understood from the fact that \Psi=U Q_B
U^{-1} with U=(U_tv)^{\pm 2} does not satisfy the CSFT EOM in the strong sense
and hence is not truly a pure-gauge in our regularization.Comment: 20 pages, no figures; v2: references added, minor change
Exploring Galaxy Evolution from Infrared Number Counts and Cosmic Infrared Background
Recently reported infrared (IR) galaxy number counts and cosmic infrared
background (CIRB) all suggest that galaxies have experienced a strong evolution
sometime in their lifetime. We statistically estimate the galaxy evolution
history from these data. We find that an order of magnitude increase of the
far-infrared (FIR) luminosity at redshift z = 0.5 - 1.0 is necessary to
reproduce the very high CIRB intensity at 140 um reported by Hauser et al.
(1998). z \sim 0.75 and decreases to, even at most, a factor of 10 toward z
\sim 5, though many variants are allowed within these constraints. This
evolution history also satisfies the constraints from the galaxy number counts
obtained by IRAS, ISO and, roughly, SCUBA. The rapid evolution of the comoving
IR luminosity density required from the CIRB well reproduces the very steep
slope of galaxy number counts obtained by ISO. We also estimate the cosmic star
formation history (SFH) from the obtained FIR luminosity density, considering
the effect of the metal enrichment in galaxies. The derived SFH increases
steeply with redshift in 0
0.75. This is consistent with the SFH estimated from the reported ultraviolet
luminosity density. In addition, we present the performance of the Japanese
ASTRO-F FIR galaxy survey. We show the expected number counts in the survey. We
also evaluate how large a sky area is necessary to derive a secure information
of galaxy evolution up to z \sim 1 from the survey, and find that at least 50 -
300 deg^2 is required.Comment: 18 pages LaTeX, PASJ in press. Abstract abridge
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