arXiv subjects

Noriaki Kitazawa

Publications and source records attributed to Noriaki Kitazawa.

At least 19 recordsLinked to original sources

arXiv2026

Self-interacting dark matter and core formation in field low-surface-brightness galaxies

Dark matter may play an important role in galaxy formation through its non-trivial properties. For example, self-interacting dark matter may contribute to the formation of the widely observed core structures in galaxies. However, galaxy formation is a complex process, and such core structures can also arise from baryonic effects within the cold dark matter framework. To clarify the role of dark matter self-interactions, it is necessary to study systems that evolve without significant baryonic disturbances. Low-surface-brightness galaxies in the field, which are gravitationally isolated and have evolved with minimal external influence, are suitable candidates for this purpose. Since these galaxies typically contain only a small amount of baryonic matter, strong baryonic effects are not expected in their evolutionary history. In this study, we assume that these galaxies decoupled from proto-clusters at high redshift. Based on this assumption, we set initial conditions and estimate the time required for core formation, which we compare with the time corresponding to the redshift of proto-clusters. We examine five low-surface-brightness galaxies in the field and three observed proto-clusters at redshifts z=2.45, 7.66 and 7.88. Our analyses, based on order-of-magnitude estimates without numerical simulations, excludes a self-interaction cross section of sigma/m = 1 cm^2/g, while sigma/m = 0.1 cm^2/g is favored. This result is consistent with constraints derived from the shapes of present-day cluster cores.

astro-ph.CO↗

arXiv2024

Hubble tension may indicate time-dependent dark matter comoving energy density

The values of Hubble constant H0 by direct measurements with standard distance ladder are typically larger than those obtained from the observation of cosmic microwave background and the galaxy survey with inverse distance ladder. On the other hand, although the errors are still large, various determinations of the value of matter density parameter Omega_m are consistent with each other. Therefore, it is possible that the difference in Hubble constant is translated to the difference of physical matter energy density omega_m = Omega_m h^2, where h = H0 / (100 Km/s/Mpc). In this article it is examined the possibility of an increase of the physical dark matter energy density (comoving energy density without the effect of expansion of the universe) by a fast transition at a certain value of redshift as a possible resolution of the Hubble tension. A phenomenological fluid model of the dark sector, which is the modification of a so-called unified dark matter model, is introduced to concretely realize such a fast transition in the physical dark matter energy density.

astro-ph.CO↗

arXiv2023

Late-time data require smaller sound horizon at recombination

The Hubble constant problem is that the values of Hubble constant from the observation of cosmic microwave background assuming the LambdaCDM model disagrees with the values from direct measurements. This problem suggests some new physics beyond the LambdaCDM model. Typically there are two ways of reconciliation: one is the realization of smaller value of sound horizon at recombination, and the other is the modification of the way of expansion of the universe after recombination. In this letter we examine the latter possibility by comparing two typical phenomenological dark energy models with the distance-redshift relation provided by Pantheon catalogue of supernova observations and galaxy surveys by BOSS and eBOSS collaborations. Though these phenomenological dark energy models globally fit observations better than the LambdaCDM model, they are strongly disfavored by the distance-redshift relation as almost the same level as the LambdaCDM model defined by cosmic microwave background observations. The distance-redshift relation strongly suggests some new physics which realize smaller value of sound horizon at recombination.

astro-ph.CO↗

arXiv2023

Stringy Threshold Corrections in D-brane Systems

We investigate string amplitudes by using the partial modular transformation which we introduced in our previous works. This enables us to extract stringy threshold corrections from the full string amplitudes and interpret them in terms of the Wilsonian effective field theory in a natural way. We calculate mass shifts and wave function renormalizations for massless scalar fields on brane-antibrane systems. We find that the mass shift can be exponentially small and negative. We also propose a strategy for realizing a hierarchical mass spectrum on D-branes.

hep-th↗

arXiv2022

Inflaton as a pseudo-Nambu-Goldstone boson

In the realistic model of cosmic inflation the inflaton potential should be flat and stable under quantum corrections. It is natural to imagine that there is some symmetry behind and an idea of the inflaton as a Nambu-Goldstone boson of spontaneous breaking of some symmetry has been examined. We give a general formulation of this idea using the non-linear realization of Nambu-Goldstone boson in low-energy effective theory with some explicit symmetry breaking to generate non-trivial potential. The potential is naturally a simple function, typically the mass term of inflaton, and the scenario of "warm inflation" should necessarily be applied under the present observational constraints. We investigate the generation mechanism of necessary thermal dissipation term in inflaton field equation for "warm inflation" without large thermal corrections to inflaton potential. A simple numerical analysis is given to investigate the viability of this scenario.

astro-ph.CO↗

arXiv2022

Reionization process dependence of the ratio of CMB polarization power spectra at low-$\ell$

We investigate how much the ratio of cosmic microwave background (CMB) polarization power spectra $C^{BB}_\ell/C^{EE}_\ell$ at low-$\ell$ ($\ell \lesssim 10$) depends on the process of reionization. Both such low-$\ell$ B-mode and E-mode polarization powers are dominantly produced by Thomson scattering of CMB photons off the free electrons which are produced in the process of reionization. Since the reionization should be finished until at least the redshift $z \simeq 6$ and the low-$\ell$ polarization powers are produced at late time, the ratio is rather insensitive by the ionization process at higher redshifts, but it is sensitive to the value of optical depth.The value of the ratio at $\ell=2$, however, is almost insensitive to the reionization process including the value of optical depth, and the value is approximately half of the value of tensor-to-scalar ratio. This fact can be utilized for future determination of tensor-to-scalar ratio in spite of the ambiguity due to cosmic variance.

astro-ph.CO↗

arXiv2021

Polarization of CMB and possible time dependence of dark energy

Dark energy has been introduced to explain the present accelerating expansion of the universe. In the LambdaCDM model, the present standard model of cosmology, dark energy is described as a cosmological constant which is time independent. The possibility of the time dependence of dark energy has been investigated to obtain deeper understanding of it by looking redshit-magnitude relation of type Ia supernova, for example. We investigate the constraints to the time dependence of dark energy with several phenomenological models by fitting their parameters to the redshit-magnitude relation of the Pantheon supernova catalog, and confirm that little time dependence can not be excluded by the goodness-of-fit criterion only. Such a non-trivial time dependence causes different expansion rate in the period of reionization, which affects the low-l polarization power spectrum of CMB. We investigate the possibility to detect the effect in future probe like LiteBIRD, for example. We find that the low-l EE polarization power spectrum is enhanced in general, but it will be difficult to be detected as far as looking the EE polarization power spectrum only because of the limitation by cosmic variance.

astro-ph.CO↗

arXiv2021

Gauge Symmetry Restoration by Higgs Condensation in Flux Compactifications on Coset Spaces

Extra-dimensional components of gauge fields in higher-dimensional gauge theories will play a role of the Higgs field and become tachyonic after Kaluza-Klein compactifications on internal spaces with (topologically nontrivial) gauge field backgrounds. Its condensation is then expected to break gauge symmetries spontaneously. But, contrary to the expectation, some models exhibit restoration of gauge symmetries. In this paper, by considering all the massive Kaluza-Klein excitations of gauge fields, we explicitly show that some of them indeed become massless at the minimum of the Higgs potential and restore (a part of) the gauge symmetries which are broken by gauge field backgrounds. We particularly consider compactifications on $S^2$ with monopole-like fluxes and also on $\mathbb{CP}^2$ with instanton and monopole-like fluxes. In some cases, the gauge symmetry is fully restored, as argued in previous literature. In other cases, there is a stable vacuum with a partial restoration of the gauge symmetry after Higgs condensation. Topological structure of the gauge field configurations prevent the gauge symmetries to be restored.

hep-th↗

arXiv2021

Polarizations of CMB and the Hubble tension

Future precision measurements of CMB polarizations can shed new light on the problem so called Hubble tension. The Hubble tension comes from the difference of the evolutions of the Hubble parameter which are determined with two different distance ladders. The standard distance ladder with the observation of Cepheid variables and type Ia supernovae gives larger values of the Hubble constant, and the inverse distance ladder with the observation of the baryon acoustic oscillations both in the CMB and in the clustering of galaxies gives smaller values of the Hubble constant. These different evolutions of the Hubble parameter indicate different evolutions of the free electron density in the process of the reionization of the universe and different magnitudes of low-l polarizations of the CMB, since these polarizations are mainly produced through the Thomson scattering of CMB photons off these free electrons. We investigate the effect on CMB E-mode and B-mode polarizations of l < 12 assuming non-trivially time-dependent equation of state of dark energy. We find that the case of the standard distance ladder gives higher power of polarizations than the prediction in the LambdaCDM model.

astro-ph.CO↗

arXiv2020

More on Effective Potentials for Revolving D-Branes

We continue to investigate the effective potential between a pair of D$p$-branes revolving around each other by using the technique of ${\it partial\ modular\ transformation}$ developed in our previous work. We determine the shape of the potential for general $p$ for a wide range of regions interpolating smaller and larger distances than the string scale $l_s$. We also discuss the backreaction of the D-brane system to the space-time metric and the validity of our calculations.

hep-th↗

arXiv2019

Dynamics of Revolving D-Branes at Short Distances

We study the behavior of the effective potential between revolving D$p$-branes at all ranges of the distance $r$, interpolating $r \gg l_s$ and $r \ll l_s$ ($l_s$ is the string length). Since the one-loop open string amplitude cannot be calculated exactly, we instead employ an efficient method of $\it{ partial\ modular\ transformation}$. The method is to perform the modular transformation partially in the moduli parameter and rewrite the amplitude into a sum of contributions from both of the open and closed string massless modes. It is nevertheless free from the double counting and can approximate the open string amplitudes with less than $3\%$ accuracy. From the D-brane effective field theory point of view, this amounts to calculating the one-loop threshold corrections of infinitely many open string massive modes. We show that threshold corrections to the $ω^2 r^2$ term of the moduli field $r$ cancel among them, where $ω$ is the angular frequency of the revolution and sets the scale of supersymmetry breaking. This cancellation suggests a possibility to solve the hierarchy problem of the Higgs mass in high scale supersymmetry breaking models.

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arXiv2019

A Possibility of Lorentz Violation in the Higgs Sector

In string theory, a scalar field often appears as a moduli of a geometrical configuration of D-branes in higher dimensional space. In the low energy effective theory on D-branes, the distance between D-branes is translated into the energy scale of the gauge symmetry breaking. In this paper, we study a phenomenological consequence of a possibility that the Higgs field is such a moduli field and the D-brane configuration is stabilized by a stationary motion, in particular, revolution of D-branes on which we live. Then, due to the Coriolis force, Higgs mode is mixed with the angular fluctuation of branes and the Lorentz symmetry is violated in the dispersion relation of the Higgs boson. The Higgs boson mass measurements at LHC experiments give an upper bound $\sim {\cal O}(0.1)$ GeV for the angular frequency of the revolution of D-branes.

hep-ph↗

arXiv2019

On CMB B-modes and the Onset of Inflation

The temperature perturbations of the cosmic microwave background radiation (CMB) appear systematically suppressed, at large angular scales, with respect to the prediction of the LambdaCDM concordance model. This behavior might be a glimpse of the inflaton deceleration from fast-roll at the start of inflation. If this were true, the spectrum of primordial tensor perturbations should be distorted in a corresponding way, with a suppression of large angular scale B-mode polarization that might be within reach for future probes like LiteBIRD. We investigate this scenario by a semi-analytic method based on a truncation of the B-mode polarization spectrum, which in our opinion has the virtue of highlighting the underlying Physics. We present some mild evidence that, with sufficient knowledge of the reionization process, the suppression of large-scale B-modes might be within reach.

astro-ph.CO↗

arXiv2018

Extraction of $|V_{cb}|$ from two-body hadronic B decays

We propose a method of extracting the Cabibbo-Kobayashi-Maskawa matrix element $|V_{cb}|$ from two-body hadronic decay processes of $B\to DK$ with precisely determined form factors of $B$ meson semi-leptonic decays. The amplitude $\mathcal{M}(\bar{B}^0 \to D^+ K^-)$ which does not include the effect of hadronic final state interactions can be theoretically evaluated by using factorization and form factors of semi-leptonic B decays. We can obtain all the amplitudes in an isospin relation $\mathcal{A}(B^-\to D^0K^-) =\mathcal{A}(\bar{B}^0\to D^+K^{-})+\mathcal{A}(\bar{B}^0\to D^{0}\bar{K}^0)$ including the effect of hadronic final state interactions as well as $|V_{cb}|$ using the experimental data of branching fractions of these three processes with a truncation of the states which contribute to the hadronic final state interactions. The extracted value of $|V_{cb}|$ is $(37\pm 6)\times 10^{-3}$. The decay processes of $B\to DK^{*}$ and $B\to D^{*}K$ can also be used in the same way and the extracted values of $|V_{cb}|$ are $(41\pm 7)\times 10^{-3}$ and $(42\pm 9)\times 10^{-3}$, respectively. This method becomes possible by virtue of recent precise determinations of the form factors of semi-leptonic B decays. The uncertainties of $|V_{cb}|$ by this method are expected to be reduced by the results of future B-factory experiments and lattice calculations.

hep-ph↗

arXiv2018

Brane SUSY Breaking and the Gravitino Mass

Supergravity models with spontaneously broken supersymmetry have been widely investigated over the years, together with some notable non-linear limits. Although in these models the gravitino becomes naturally massive absorbing the degrees of freedom of a Nambu-Goldstone fermion, there are cases in which the naive counting of degrees of freedom does not apply, in particular because of the absence of explicit gravitino mass terms in unitary gauge. The corresponding models require non-trivial de Sitter-like backgrounds, and it becomes of interest to clarify the fate of their Nambu-Goldstone modes. We elaborate on the fact that these non-trivial backgrounds can accommodate, consistently, gravitino fields carrying a number of degrees of freedom that is intermediate between those of massless and massive fields in a flat spacetime. For instance, in a simple supergravity model of this type with de Sitter background, the overall degrees of freedom of gravitino are as many as for a massive spin-3/2 field in flat spacetime, while the gravitino remains massless in the sense that it undergoes null-cone propagation in the stereographic picture. On the other hand, in the ten-dimensional USp(32) Type I Sugimoto model with "brane SUSY breaking", which requires a more complicated background, the degrees of freedom of gravitino are half as many of those of a massive one, and yet it somehow behaves again as a massless one.

hep-th↗

arXiv2018

An approach to the instanton effect in B system

We discuss the constraint on the size of QCD instanton effects in low-energy effective theory. Among various instanton effects in meson mass spectrum and dynamics, we concentrate on the instanton-induced masses of light quarks. The famous instanton-induced six-quark interaction, so-called 't Hooft vertex, could give non-perturbative quantum corrections to light quark masses. Many works have already been achieved to constrain the mass corrections in light meson system, or the system of pi, K, eta and eta', and now we know for a fact that the instanton-induced mass of up-quark is too small to realize the solution of the strong CP problem by vanishing current mass of up-quark. In this work we give a constraint on the instanton-induced mass correction to light quarks from the mass spectrum of heavy mesons, B+, B0, Bs and their anti-particles. To accomplish this, the complete second order chiral symmetry breaking terms are identified in heavy meson effective theory. We find that the strength of the constraint from heavy meson masses is at the same level of that from light mesons, and it would be made even stronger by more precise data from future B factories and lattice calculations.

hep-ph↗

arXiv2017

Electromagnetic Radiation in a Semi-Compact Space

In this note, we investigate the electromagnetic radiation emitted from a revolving point charge in a compact space. If the point charge is circulating with an angular frequency $ω_0$ on the $(x,y)$-plane at $z=0$ with boundary conditions, $x \sim x+2 πR$ and $y \sim y+2πR$, it emits radiation into the $z$-direction of $z$ in $ [-\infty, +\infty]$. We find that the radiation shows discontinuities as a function of $ω_0 R$ at which a new propagating mode with a different Fourier component appears. For a small radius limit $ω_0 R \ll 1$, all the Fourier modes except the zero mode on $(x,y)$-plane are killed, but an effect of squeezing the electric field totally enhances the radiation. In the large volume limit $ω_0 R \rightarrow \infty$, the energy flux of the radiation reduces to the expected Larmor formula.

hep-th↗

arXiv2017

On D-brane dynamics and moduli stabilization

We discuss the effect of the dynamics of D-branes on moduli stabilization in type IIB string theory compactifications, with reference to a concrete toy model of T6/Z3 orientifold compactification with fractional D3-branes and anti-D3-branes at orbifold fixed points. The resulting attractive forces between anti-D3-branes and D3-branes, together with the repulsive forces between anti-D3-branes and O3-planes, can affect the stability of the compact space. There are no complex structure moduli in T6/Z3 orientifold, which should thus capture some generic features of more general settings where all complex structure moduli are stabilized by three-form fluxes. The simultaneous presence of branes and anti-branes brings along the breaking of supersymmetry. Non-BPS combinations of this type are typical of "brane supersymmetry breaking", and are a necessary ingredient in the KKLT scenario for stabilizing the remaining Kahler moduli. The conclusion of our analysis is that, while mutual D-brane interactions sometimes help Kahler moduli stabilization, this is not always the case.

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