Publishing type：Research paper (scientific journal)  

DOI： 10.1088/1475-7516/2024/12/050

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Publishing type：Research paper (scientific journal)  

DOI： 10.1103/PhysRevD.110.063521

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Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.1016/j.physletb.2024.138854

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Publishing type：Research paper (scientific journal)  

DOI： 10.1103/PhysRevD.109.L121305

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Publishing type：Research paper (scientific journal)  

DOI： 10.1103/PhysRevD.109.103514

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Publishing type：Research paper (scientific journal)  

DOI： 10.1007/JHEP01(2024)105

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Language：English  

DOI： 10.1016/b978-0-32-395636-9.00012-8

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Publishing type：Research paper (scientific journal)  

DOI： 10.1103/PhysRevD.108.L101304

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Publishing type：Research paper (scientific journal)  

<jats:title>Abstract</jats:title>
<jats:p>We show that a hybrid inflation model with multiple waterfall fields can result in the
formation of primordial black holes (PBHs) with an astrophysical size, by using an advanced algorithm to follow the
stochastic dynamics of the waterfall fields. This is in contrast to the case with a single
waterfall field, where the wavelength of density perturbations is usually too short to form PBHs
of the astrophysical scale (or otherwise PBHs are overproduced and the model is ruled out)
unless the inflaton potential is tuned. In particular, we demonstrate that PBHs with masses of
order 10<jats:sup>20</jats:sup> g can form after hybrid inflation consistently with other cosmological
observations if the number of waterfall fields is about 5 for the case of instantaneous
reheating. Observable gravitational waves are produced from the second-order effect of large
curvature perturbations as well as from the dynamics of texture or global defects that form after
the waterfall phase transition. </jats:p>

DOI： 10.1088/1475-7516/2023/11/089

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Publishing type：Research paper (scientific journal)   Publisher：IOP Publishing  

Abstract

In canonical single-field inflation, the production of primordial black holes (PBH) requires a transient violation of the slow-roll condition. The transient ultra slow-roll inflation is an example of such scenarios, and more generally, one can consider the transient constant-roll inflation. We investigate the squeezed bispectrum in the transient constant-roll inflation and find that Maldacena's consistency relation holds for a sufficiently long-wavelength mode, whereas it is violated for modes around the peak scale for the non-attractor case. We also demonstrate how the one-loop corrections are modified compared to the case of the transient ultra slow-roll inflation, focusing on representative one-loop terms originating from a time derivative of the second slow-roll parameter in the cubic action. We find that the perturbativity requirement on those terms does not rule out the production of PBH from the transient constant-roll inflation.Therefore, it is a simple counterexample of the recently claimed no-go theorem of PBH production from single-field inflation.

DOI： 10.1088/1475-7516/2023/08/069

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Other Link： https://iopscience.iop.org/article/10.1088/1475-7516/2023/08/069/pdf

Publishing type：Research paper (scientific journal)   Publisher：American Physical Society (APS)  

DOI： 10.1103/physrevd.107.123539

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Other Link： http://harvest.aps.org/v2/journals/articles/10.1103/PhysRevD.107.123539/fulltext

Publishing type：Research paper (scientific journal)   Publisher：IOP Publishing  

Abstract

Primordial black holes (PBHs) whose massesare in ∼ [10^-15M_⊙,10^-11M_⊙]have been extensively studied as a candidate of whole dark matter (DM).One of the probes to test such a PBH-DM scenariois scalar-induced stochastic gravitational waves (GWs) accompanied with the enhanced primordial fluctuations to form the PBH with frequencypeaked in the mHz band being targeted by the LISA mission.In order to utilize the stochastic GW for checking the PBH-DM scenario, it needs to exactly relate the PBH abundance and the amplitude of the GW spectrum.Recently in Kitajima et al. [1],the impact of the non-Gaussianity of the enhanced primordial curvature perturbations on the PBH abundance has been investigated based on the peak theory,and they found that a specific non-Gaussian feature called the exponential tail significantly increases the PBH abundance compared with the Gaussian case.In this work, we investigate the spectrum of the induced stochastic GW associated with PBH DM in the exponential-tail case.In order to take into account the non-Gaussianity properly, we employ the diagrammatic approach for the calculation of the spectrum.We find that the amplitude of the stochastic GW spectrum is slightly lower than the one for the Gaussian case, but it can still be detectable with the LISA sensitivity.We also find that the non-Gaussian contribution can appear on the high-frequency side through their complicated momentum configurations.Although this feature emerges under the LISA sensitivity, it might be possible to obtain information about the non-Gaussianity from GW observation with a deeper sensitivity such as the DECIGO mission.

DOI： 10.1088/1475-7516/2023/05/044

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Other Link： https://iopscience.iop.org/article/10.1088/1475-7516/2023/05/044/pdf

Publishing type：Research paper (scientific journal)   Publisher：IOP Publishing  

Abstract

We propose an extension of the Higgs inflation to the hybrid metric-Palatini gravity, where we introduce non-minimal couplings between Higgs and both the metric-type and the Palatini-type Ricci scalars. We study the inflationary phenomenology of our model and find that slow-roll inflation can be realized in the large-field regime, giving the observationally favored predictions. In particular, the scalar spectral index exhibits an attractor behavior to  n_s ∼ 0.964, while the tensor-to-scalar ratio can take an arbitrary value depending on the non-minimal coupling parameters, with the metric-Higgs limit r ∼ 10^-3 being the maximum. We also investigate the unitarity property of our model. As the ultraviolet (UV) cutoff as a low-energy effective field theory (EFT) of this model is significantly lower than the Planck scale due to a strong curvature of field-space, we consider a possible candidate of UV-extended theories with an additional scalar field introduced so as to flatten the field-space in five-dimension. While the field-space can be flatten completely and this approach can lead to a weakly-coupled EFT, we gain an implication that Planck-scale EFT can be only realized in the limit of metric-Higgs inflation. We also discuss generalizations of the model up to mass-dimension four.

DOI： 10.1088/1475-7516/2023/05/047

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Other Link： https://iopscience.iop.org/article/10.1088/1475-7516/2023/05/047/pdf

Publishing type：Research paper (scientific journal)   Publisher：{IOP} Publishing  

<jats:title>Abstract</jats:title>
<jats:p>We develop the stochastic formalism for U(1) gauge fields that has the Chern-Simons coupling to a rolling pseudo-scalar field during inflation.
The Langevin equations for the physical electromagnetic fields are derived and the analytic solutions are studied. Using numerical simulation we demonstrate that the electromagnetic fields averaged over the Hubble scale continuously change their direction and their amplitudes fluctuate around the analytically obtained expectation values.
Though the isotropy is spontaneously broken by picking up a particular local Hubble patch, each Hubble patch is understood independent and the isotropy is conserved globally by
averaging all the Hubble patches.</jats:p>

DOI： 10.1088/1475-7516/2022/12/026

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Publishing type：Research paper (scientific journal)  

DOI： 10.3847/1538-4357/ac93f1

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Publishing type：Research paper (scientific journal)   Publisher：{IOP} Publishing  

Abstract

The axionic inflaton with the Chern-Simons coupling may generate U(1) gauge fields and charged particles simultaneously. In order to incorporate the backreaction from the charged particles on the gauge fields, we develop a procedure to obtain an equilibrium solution for the gauge fields by treating the induced current as effective electric and magnetic conductivities. Introducing mean field approximation, and numerically solving self-consistency equations, we find that the gauge field amplitudes are drastically suppressed. Interestingly, as the production becomes more efficient, the charged particles gain a larger part of the transferred energy from the inflaton and eventually dominate it. Our formalism offers a basis to connect this class of inflationary models to a rich phenomenology such as baryogenesis and magnetogenesis.

DOI： 10.1088/1475-7516/2022/09/023

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Other Link： https://iopscience.iop.org/article/10.1088/1475-7516/2022/09/023/pdf

Publishing type：Research paper (scientific journal)   Publisher：{IOP} Publishing  

<jats:title>Abstract</jats:title>
<jats:p>We investigate the UV-completion of the Higgs inflation in
the metric and the Palatini formalisms. It is known that the cutoff
scales for the perturbative unitarity of these inflation models
become much smaller than the Planck scale to be consistent with
observations. Expecting that the low cutoff scales originate in the
curvature of a field-space spanned by the Higgs fields, we consider
embedding the curved field-space into a higher dimensional flat
space and apply this procedure to the metric-Higgs and the
Palatini-Higgs scenarios. The new field introduced in this way
successfully flattens the field-space and UV-completes the Higgs
inflation in the metric formalism. However, in the Palatini
formalism, the new field cannot uplift the cutoff up to the Planck
scale. We also discuss the unavoidable low cutoff in the Palatini
formalism in the context of the local conformal symmetry. </jats:p>

DOI： 10.1088/1475-7516/2022/05/035

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Publishing type：Research paper (scientific journal)   Publisher：{IOP} Publishing  

<jats:title>Abstract</jats:title>
<jats:p>In this work, we have performed numerical simulations of
primordial black hole (PBH) formation in the Friedman-Lemaître-Robertson-Walker universe filled by radiation fluid, introducing the local-type non-Gaussianity to the primordial curvature fluctuation.
We have compared the numerical results from simulations with previous analytical estimations on the threshold value for PBH formation done in the previous paper [1], particularly for negative values of the non-linearity parameter <jats:italic>f</jats:italic>
<jats:sub>NL</jats:sub>.
Our numerical results show the existence of PBH formation of (the so-called) type I also in the case <jats:italic>f</jats:italic>
<jats:sub>NL</jats:sub> ≲ -0.336, which was not found in the previous analytical expectations using the critical averaged compaction function.
In particular, although the universal value for the averaged critical compaction function 𝒞̅<jats:sub>𝒸</jats:sub> = 2/5 found previously in the literature is not satisfied for all the profiles considered in this work, an alternative direct analytical estimate has been found to be roughly accurate to estimate the thresholds, which gives the value of the critical averaged density with a few % deviation from the numerical one for <jats:italic>f</jats:italic>
<jats:sub>NL</jats:sub> ≳ -1.</jats:p>

DOI： 10.1088/1475-7516/2022/05/012

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Publishing type：Research paper (scientific journal)   Publisher：{IOP} Publishing  

<jats:title>Abstract</jats:title>
<jats:p>We present a generic framework to compute the one-point
statistics of cosmological perturbations, when coarse-grained at an
arbitrary scale <jats:italic>R</jats:italic>, in the presence of quantum diffusion. Making
use of the stochastic-δ <jats:italic>N</jats:italic> formalism, we show how it can be
related to the statistics of the amount of expansion realised until
the scale <jats:italic>R</jats:italic> crosses out the Hubble radius. This leads us to
explicit formulae for the probability density function (PDF) of the
curvature perturbation, the comoving density contrast, and the
compaction function. We then apply our formalism to the calculation
of the mass distribution of primordial black holes produced in a
single-field model containing a “quantum well” (i.e. an exactly
flat region in the potential). We confirm that the PDFs feature
heavy, exponential tails, with an additional cubic suppression in
the case of the curvature perturbation. The large-mass end of the
mass distribution is shown to be mostly driven by
stochastic-contamination effects, which produce black holes more
massive than those naively expected. This work bridges the final gap
between the stochastic-inflation formalism and the calculation of
the mass distribution of astrophysical objects such as primordial
black holes, and opens up various prospects that we finally discuss.</jats:p>

DOI： 10.1088/1475-7516/2022/02/021

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Other Link： http://arxiv.org/pdf/2111.15280v2

Publishing type：Research paper (scientific journal)   Publisher：IOP Publishing  

DOI： 10.1088/1475-7516/2021/10/053

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Other Link： https://iopscience.iop.org/article/10.1088/1475-7516/2021/10/053/pdf

Publishing type：Research paper (scientific journal)   Publisher：IOP Publishing  

Abstract

The standard model of particle physics is known to be intriguingly successful. However, their rich phenomena represented by the phase transitions (PTs) have not been completely understood yet, including the possibility of the existence of unknown dark sectors. In this paper, we investigate the measurement of the equation of state parameter w and the sound speed of the PT plasmawith the use ofthe gravitational waves (GWs) of the universe. Though the propagation of GW is insensitive to in itself, the sound speed value affects the dynamics of primordial density (or scalar curvature) perturbations, and the induced GW by their horizon reentry can then be an indirect probe both w and . We numerically reveal the concrete spectrum of the predicted induced GW with two simple examples of the scalar perturbation spectrum: the monochromatic and scale-invariant spectra. In the monochromatic case, we see that the resonant amplification and cancellation scales of the induced GW depend on the values at different times respectively. The scale-invariant case gives a more realistic spectrum and its specific shape will be compared with observations. In particular, the QCD phase transition corresponds with the frequency range of the pulsar timing array (PTA) observations. If the amplitude of primordial scalar power is in the range of 10^-4 ≲ A_ζ ≲ 10^-2, the induced GW is consistent with current observational constraints and detectable in the future observation in Square Kilometer Array. Furthermore, the recent possible detection of stochastic GWs by NANOGrav 12.5 yr analysis [1] can be explained by the induced GW if A_ζ ∼ √(7) × 10^-3.

DOI： 10.1088/1475-7516/2021/06/048

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Other Link： https://iopscience.iop.org/article/10.1088/1475-7516/2021/06/048/pdf

Publishing type：Research paper (scientific journal)   Publisher：American Physical Society (APS)  

DOI： 10.1103/physrevd.103.l101303

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Other Link： http://harvest.aps.org/v2/journals/articles/10.1103/PhysRevD.103.L101303/fulltext

Publishing type：Research paper (scientific journal)   Publisher：Oxford University Press (OUP)  

Abstract

We revisit the squeezed-limit non-Gaussianity in the single-field non-attractor inflation models from the viewpoint of the cosmological soft theorem. In the single-field attractor models, inflaton’s trajectories with different initial conditions effectively converge into a single trajectory in the phase space, and hence there is only one clock degree of freedom (DoF) in the scalar part. Its long-wavelength perturbations can be absorbed into the local coordinate renormalization and lead to the so-called consistency relation between n- and (n + 1)-point functions. On the other hand, if the inflaton dynamics deviates from the attractor behavior, its long-wavelength perturbations cannot necessarily be absorbed and the consistency relation is expected not to hold any longer. In this work, we derive a formula for the squeezed bispectrum including the explicit correction to the consistency relation, as a proof of its violation in the non-attractor cases. First one must recall that non-attractor inflation needs to be followed by attractor inflation in a realistic case. Then, even if a specific non-attractor phase is effectively governed by a single DoF of phase space (represented by the exact ultra-slow-roll limit) and followed by a single-DoF attractor phase, its transition phase necessarily involves two DoF in dynamics and hence its long-wavelength perturbations cannot be absorbed into the local coordinate renormalization. Thus, it can affect local physics, even taking account of the so-called local observer effect, as shown by the fact that the bispectrum in the squeezed limit can go beyond the consistency relation. More concretely, the observed squeezed bispectrum does not vanish in general for long-wavelength perturbations exiting the horizon during a non-attractor phase.

DOI： 10.1093/ptep/ptab063

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Publishing type：Research paper (scientific journal)   Publisher：IOP Publishing  

Abstract

Stochastic inflation is an effective theory describing the super-Hubble, coarse-grained, scalar fields driving inflation, by a set of Langevin equations. We previously highlighted the difficulty of deriving a theory of stochastic inflation that is invariant under field redefinitions, and the link with the ambiguity of discretisation schemes defining stochastic differential equations. In this paper, we solve the issue of these "inflationary stochastic anomalies" by using the Stratonovich discretisation satisfying general covariance, and identifying that the quantum nature of the fluctuating fields entails the existence of a preferred frame defining independent stochastic noises. Moreover, we derive physically equivalent Itô-Langevin equations that are manifestly covariant and well suited for numerical computations. These equations are formulated in the general context of multifield inflation with curved field space, taking into account the coupling to gravity as well as the full phase space in the Hamiltonian language, but this resolution is also relevant in simpler single-field setups. We also develop a path-integral derivation of these equations, which solves conceptual issues of the heuristic approach made at the level of the classical equations of motion, and allows in principle to compute corrections to the stochastic formalism. Using the Schwinger-Keldysh formalism, we integrate out small-scale fluctuations, derive the influence action that describes their effects on the coarse-grained fields, and show how the resulting coarse-grained effective Hamiltonian action can be interpreted to derive Langevin equations with manifestly real noises. Although the corresponding dynamics is not rigorously Markovian, we show the covariant, phase-space Fokker-Planck equation for the Probability Density Function of fields and momenta when the Markovian approximation is relevant, and we give analytical approximations for the noises' amplitudes in multifield scenarios.

DOI： 10.1088/1475-7516/2021/04/048

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Other Link： https://iopscience.iop.org/article/10.1088/1475-7516/2021/04/048/pdf

Publishing type：Research paper (scientific journal)   Publisher：Oxford University Press (OUP)  

Abstract

Non-Gaussianities of primordial perturbations in the soft limit provide important information about the light degrees of freedom during inflation. The soft modes of the curvature perturbations, unobservable for a local observer, act to rescale the spatial coordinates. We determine how the trispectrum in the collapsed limit is shifted by the rescaling due to the soft modes. We find that the form of the inequality between the $f_\mathrm{NL}$ and $\tau_\mathrm{NL}$ parameters is not affected by the rescaling, demonstrating that the role of the inequality as an indicator of the light degrees of freedom remains intact. We also comment on the local observer effect on the consistency relation for ultra-slow-roll inflation.

DOI： 10.1093/ptep/ptaa144

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Other Link： http://academic.oup.com/ptep/article-pdf/2020/11/113E01/34299933/ptaa144.pdf

Publishing type：Research paper (scientific journal)   Publisher：IOP Publishing  

Systematic understanding for classes of inflationary models is investigated from the viewpoint of the local conformal symmetry and the slightly broken global symmetry in the framework of the metric-affine geometry. In the metric-affine geometry, which is a generalisation of the Riemannian one adopted in the ordinary General Relativity, the affine connection is an independent variable of the metric rather than given e.g. by the Levi-Civita connection as its function. Thanks to this independency, the metric-affine geometry can preserve the local conformal symmetry in each term of the Lagrangian contrary to the Riemannian geometry, and then the local conformal invariance can be compatible with much more kinds of global symmetries. As simple examples, we consider the two-scalar models with the broken $\mathrm{SO}(1,1)$ or $\mathrm{O}(2)$, leading to the well-known $\alpha$-attractor or natural inflation, respectively. The inflaton can be understood as their pseudo Nambu-Goldstone boson.

DOI： 10.1209/0295-5075/132/39001

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Other Link： https://iopscience.iop.org/article/10.1209/0295-5075/132/39001/pdf

Publishing type：Research paper (scientific journal)  

In the context of string theory, several conjectural conditions have been proposed for low energy effective field theories not to be in swampland, the UV-incomplete class. The recent ones represented by the de Sitter and trans-Planckian censorship conjectures in particular seem to conflict with the inflation paradigm of the early universe. We first point out that scenarios where inflation is repeated several times (multi-phase inflation) can be easily compatible with these conjectures. In other words, we relax the constraint on the single inflation for the large scale perturbations to only continue at least around 10 e-folds. In this context, we then investigate if a spectator field can be a source of the almost scale-invariant primordial perturbations on the large scale. As a consequence of such an isocurvature contribution, the resultant perturbations exhibit the non-vanishing non-Gaussianity in general. Also the perturbation amplitude on smaller scales can be completely different from that on the large scale due to the multiplicity of inflationary phases. These signatures will be a smoking gun of this scenario by the future observations.

DOI： 10.1103/PhysRevD.101.103514

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Other Link： http://arxiv.org/pdf/2003.06753v2

Language：English   Publishing type：Research paper (scientific journal)  

We propose a class of single-field, slow-roll inflation models in which a
typical number of $e$-folds can be extremely large. The key point is to
introduce a very shallow local minimum near the top of the potential in a
hilltop inflation model. In particular, a typical number of $e$-folds is
enhanced if classical behavior dominates around the local minimum such that the
inflaton probability distribution is drifted to the local minimum as a whole.
After the inflaton escapes from the local minimum due to the stochastic
dynamics, the ordinary slow-roll inflation follows and it can generate the
primordial density perturbation consistent with observation. Interestingly, our
scenario inherits the advantages of the old and new inflation: the typical
$e$-folds can be extremely large as in the old inflation, and slow-roll
inflation naturally follows after the stochastic regime as in the new
inflation. In our numerical example, the typical number of $e$-folds can be as
large as $10^{10^{10 } }$, which is large enough for various light scalars such
the QCD axion to reach the Bunch-Davies distribution.

DOI： 10.1016/j.physletb.2019.135097

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Other Link： http://arxiv.org/pdf/1908.08694v2

Publishing type：Research paper (scientific journal)   Publisher：American Physical Society ({APS})  

We investigate a possibility of primordial black hole (PBH) formation with a hierarchical mass spectrum in multiple phases of inflation. As an example, we find that one can simultaneously realize a mass spectrum which has recently attracted a lot of attention: stellar-mass PBHs ($\sim\mathcal{O}(10)M_\odot$) as a possible source of binary black holes detected by LIGO/Virgo collaboration, asteroid-mass ($\sim\mathcal{O}(10^{-12})M_\odot$) as a main component of dark matter, and earth-mass ($\sim\mathcal{O}(10^{-5})M_\odot$) as a source of ultrashort-timescale events in Optical Gravitational Lensing Experiment microlensing data. The recent refined de Sitter swampland conjecture may support such a multi-phase inflationary scenario with hierarchical mass PBHs as a transition signal of each inflationary phase.

DOI： 10.1103/PhysRevD.100.023537

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Other Link： http://arxiv.org/pdf/1904.10298v2

Publishing type：Research paper (scientific journal)  

The stochastic approach aims at describing the long-wavelength part of quantum fields during inflation by a classical stochastic theory. It is usually formulated in terms of Langevin equations, giving rise to a Fokker-Planck equation for the probability distribution function of the fields, and possibly their momenta. The link between these two descriptions is ambiguous in general, as it depends on an implicit discretisation procedure, the two prominent ones being the It\^o and Stratonovich prescriptions. Here we show that the requirement of general covariance under field redefinitions is verified only in the latter case, however at the expense of introducing spurious `frame' dependences. This stochastic anomaly disappears when there is only one source of stochasticity, like in slow-roll single-field inflation, but manifests itself when taking into account the full phase space, or in the presence of multiple fields. Despite these difficulties, we use physical arguments to write down a covariant Fokker-Planck equation that describes the diffusion of light scalar fields in non-linear sigma models in the overdamped limit. We apply it to test scalar fields in de Sitter space and show that some statistical properties of a class of two-field models with derivative interactions can be reproduced by using a correspondence with a single-field model endowed with an effective potential. We also present explicit results in a simple extension of the single-field $\lambda \phi^4$ theory to a hyperbolic field space geometry. The difficulties we describe seem to be the stochastic counterparts of the notoriously difficult problem of maintaining general covariance in quantum theories, and the related choices of operator ordering and path-integral constructions. Our work thus opens new avenues of research at the crossroad between cosmology, statistical physics, and quantum field theory.

DOI： 10.1088/1361-6382/ab097f

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Other Link： http://arxiv.org/pdf/1806.10126v2

Publisher：Elsevier {BV}  

DOI： 10.1016/j.physletb.2017.12.014

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DOI： 10.1088/1475-7516/2017/02/021

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DOI： 10.1103/PhysRevD.95.123510

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DOI： 10.1103/PhysRevD.96.043504

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DOI： 10.1103/PhysRevD.96.123527

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DOI： 10.1088/1475-7516/2016/08/041

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DOI： 10.1103/PhysRevD.94.043527

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Publishing type：Research paper (scientific journal)  

We propose a novel scenario to produce abundant primordial black holes (PBHs) in new inflation which is a second phase of a double inflation in the supergravity frame work. In our model, some preinflation phase before the new inflation is assumed and it would be responsible for the primordial curvature perturbations on the cosmic microwave background scale, while the new inflation produces only the small scale perturbations. Our new inflation model has linear, quadratic, and cubic terms in its potential and PBH production corresponds with its flat inflection point. The linear term can be interpreted to come from a supersymmetry-breaking sector, and with this assumption, the vanishing cosmological constant condition after inflation and the flatness condition for the inflection point can be consistently satisfied.

DOI： 10.1103/PhysRevD.94.083523

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DOI： 10.1088/1475-7516/2015/03/013

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DOI： 10.1103/PhysRevD.91.123534

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DOI： 10.1088/1475-7516/2015/05/054

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DOI： 10.1088/1475-7516/2014/10/030

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DOI： 10.1088/1475-7516/2013/12/036

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Venue：Beijing Normal University  

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Venue：The University of Tokyo  

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Venue：CERN  

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Venue：Institute of Cosmology and Gravitation  

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Venue：Nagoya University  

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Venue：Waseda University  

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Venue：Laboratoire de Physique de l’Ecole Normale Supérieure  

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Venue：Ludwig Maximilian University of Munich  

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Venue：Institute for Basic Science  

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Venue：Center for Theoretical Physics  

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Venue：立教大学  

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Venue：Nagoya University  

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Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Public lecture, seminar, tutorial, course, or other speech  

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Language：English   Presentation type：Poster presentation  

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Language：English   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：Nagoya University  

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Presentation type：Oral presentation (general)  

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Presentation type：Poster presentation  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：東京大学  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：University of Padova  

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Presentation type：Oral presentation (general)  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：KEK  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：Institute for Basic Science  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Poster presentation  

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Presentation type：Oral presentation (general)  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：Institut de Recherche en Astrophysique et Planétologie  

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Presentation type：Oral presentation (general)  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：Tohoku University  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：立教大学  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：Nagoya University  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：Kobe University  

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Presentation type：Oral presentation (general)  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：RESCEU  

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Presentation type：Oral presentation (general)  

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Presentation type：Poster presentation  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：Institut Astrophysique de Paris  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：Waseda University  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：Institute of Cosmology and Gravitation  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：The University of Tokyo  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：Kyoto University  

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Presentation type：Oral presentation (general)  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：RESCEU  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：KEK  

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Presentation type：Oral presentation (general)  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：Institut Astrophysique de Paris  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：University of Padova  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：AstroParticule et Cosmologie  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：名古屋大学  

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Presentation type：Oral presentation (general)  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：IPMU  

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Presentation type：Oral presentation (general)  

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Presentation type：Poster presentation  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

Venue：University of Helsinki  

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Presentation type：Oral presentation (general)  

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Presentation type：Oral presentation (general)  

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