パンパーニッチ シラチャック (パンパーニッチ シラチャック)

写真a

所属

理工学術院 先進理工学部

職名

講師(任期付)

学歴 【 表示 / 非表示

  • 2014年09月
    -
    2017年09月

    早稲田大学   大学院先進理工学研究科  

 

研究分野 【 表示 / 非表示

  • 素粒子、原子核、宇宙線、宇宙物理にする理論

研究キーワード 【 表示 / 非表示

  • Gravity

  • Cosmology

論文 【 表示 / 非表示

  • Resolving Hubble Tension with Quintom Dark Energy Model

    Sirachak Panpanich, Piyabut Burikham, Supakchai Ponglertsakul, Lunchakorn Tannukij

       2019年08月

     概要を見る

    Recent low-redshift observations give value of the present-time Hubble
    parameter $H_{0}\simeq 74~\rm{km s}^{-1}\rm{Mpc}^{-1}$, roughly 10\% higher
    than the predicted value $H_{0}=67.4~\rm{km s}^{-1}\rm{Mpc}^{-1}$ from Planck's
    observations of the Cosmic Microwave Background radiation~(CMB) and the
    $\Lambda$CDM model. Phenomenologically, we show that by adding an extra
    component X with negative density in the Friedmann equation, it can relieve the
    Hubble tension without changing the Planck's constraint on the matter and dark
    energy densities. For the extra negative density to be sufficiently small, its
    equation-of-state parameter must satisfy $1/3\leq w_{X}\leq1$. We propose a
    quintom model of two scalar fields that realizes this condition and potentially
    alleviate the Hubble tension. One scalar field acts as a quintessence while
    another "phantom" scalar conformally couples to matter in such a way that
    viable cosmological scenario can be achieved. The model depends only on two
    parameters, $\lambda_{\phi}$ and $\delta$ which represent rolling tendency of
    the self-interacting potential of the quintessence and the strength of
    conformal phantom-matter coupling respectively. The toy quintom model with
    $H_{0}=73.4~\rm{km s}^{-1}\rm{Mpc}^{-1}$~(Quintom I) gives good Supernovae-Ia
    luminosity fits, decent $r_{\rm BAO}$ fit, but slightly small acoustic
    multipole $\ell_{A}=285.54$. Full parameter scan reveals that quintom model
    provide better model than the $\Lambda$CDM model in certain region of the
    parameter space, $0.02<\delta<0.10, \Omega_{m}^{(0)}<0.31$, while significantly
    relieving Hubble tension even though not completely resolving it. A benchmark
    quintom model, Quintom II, is presented as an example.

  • Particle motions and Gravitational Lensing in de Rham-Gabadadze-Tolley Massive Gravity Theory

    Sirachak Panpanich, Supakchai Ponglertsakul, Lunchakorn Tannukij

       2019年04月

     概要を見る

    We investigate gravitational lensing and particle motions around
    non-asymptotically flat black hole spacetime in non-linear, ghost-free massive
    gravity theory, called de Rham-Gabadadze-Tolley (dRGT) massive gravity.
    Deflection angle formulae are derived in terms of perihelion parameter. The
    deflection angle can be positive, zero or even negative with various perihelion
    distance. The negative angle reveals repulsive behaviour of gravity from a
    linear term $\gamma$ in the dRGT black hole solution. We also find an
    analytically approximated formula of deflection angle in two regimes: large and
    small $\gamma$ term regimes which are shown to be consistent with direct
    numerical integration. Null and timelike geodesic motions on equatorial plane
    are explored. Particle trajectories around the dRGT black hole are plotted and
    discussed in details.

    DOI

  • Cosmological Dynamics and Double Screening of DBI Galileon Gravity

    Sirachak Panpanich, Supakchai Ponglertsakul, Kei-ichi Maeda

       2019年02月

     概要を見る

    We investigate cosmological dynamics and screening mechanism of the
    Dirac-Born-Infeld (DBI) Galileon model. The model has been divided into two
    regimes, one has positive signs in front of scalar field kinetic terms
    so-called the DBI galileon, another one has negative signs and it is dubbed as
    the DBIonic galileon. We find de Sitter solution and evolution of the Universe
    starting from radiation dominated era to late-time accelerated expansion in the
    DBI galileon model without the presence of potential term. In one of the
    attractors, the ghost and Laplacian instabilities vanishes for the whole
    evolution. We find mixing of screening mechanisms between the Vainshtein
    mechanism and the DBIonic screening mechanism in the DBIonic galileon model, in
    which a scale changing between these two mechanisms depends on a mass of a
    source.

    DOI

  • Fitting rotation curve of galaxies by de Rham-Gabadadze-Tolley massive gravity

    Sirachak Panpanich, Piyabut Burikham

       2018年06月

     概要を見る

    We investigate effects of massive graviton on the rotation curves of the
    Milky Way, spiral galaxies and Low Surface Brightness~(LSB) galaxies. Using a
    simple de Rham, Gabadadze, and Tolley (dRGT) massive gravity model, we find
    static spherically symmetric metric and a modified Tolman-Oppenheimer-Volkoff
    (TOV) equation. The dRGT nonlinear graviton interactions generate density and
    pressures which behave like a dark energy that can mimic the gravitational
    effects of a dark matter halo. We found that rotation curves of most galaxies
    can be fitted well by a single constant-gravity parameter $\gamma \sim
    m_{g}^{2}C \sim 10^{-28}~{\rm m^{-1 } }$ corresponding to the graviton mass in
    the range $m_g \sim 10^{-21}-10^{-30} {\rm eV}$ depending on the choice of the
    fiducial metric parameter $C\sim 1-10^{18}~\text{m}$. Fitting rotation curve of
    the Milky Way puts strong constraint on the Yukawa-type coupling of the massive
    graviton exchange as a result of the shell effects.

    DOI

  • Cosmological Dynamics of D-BIonic and DBI Scalar Field and Coincidence Problem of Dark Energy

    Sirachak Panpanich, Kei-ichi Maeda, Shuntaro Mizuno

       2017年03月

     概要を見る

    We study the cosmological dynamics of D-BIonic and DBI scalar field, which is
    coupled to matter fluid. For the exponential potential and the exponential
    couplings, we find a new analytic scaling solution yielding the accelerated
    expansion of the Universe. Since it is shown to be an attractor for some range
    of the coupling parameters, the density parameter of matter fluid can be the
    observed value, as in the coupled quintessence with a canonical scalar field.
    Contrary to the usual coupled quintessence, where the value of matter couple
    giving observed density parameter is too large to satisfy observational
    constraint from CMB, we show that the D-BIonic theory can give similar solution
    with much smaller value of matter coupling. As a result, together with the fact
    that the D-BIonic theory has a screening mechanism, the D-BIonic theory can
    solve the so-called coincidence problem as well as the dark energy problem.

    DOI

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特定課題研究 【 表示 / 非表示

  • Cosmological dynamics and screening mechanisms of modified gravity theories

    2020年   MAEDA Kei-ichi

     概要を見る

    We study cosmology dynamics of the cuscuta-galileon gravity. This model has only two gravitational degrees of freedom as the General Relativity, thus it is satisfied observations in the solar system scale. We use dynamical system approach to find behavior under cosmological background. We found that the cuscuta-galileon model without a potential term cannot provide the thermal history of the universe correctly. After adding a potential term we successfully find radiation dominated, matter dominated, and dark energy dominated eras. By studying stabilities of the dynamical system we found that if we start from the radiation dominated era, it will follow by matter dominated and dark energy dominated eras respectively which corresponds to the thermal history of the universe. Therefore the model can be one of the candidates for the dark energy to explain the accelerated expansion of the universe. However, the amount of dark energy in the matter dominated and the radiation dominated eras is large comparing to the cosmological constant. Thus, some observations such as the Cosmic Microwave Background, the cuscuta-galileon gravity may not satisfy. Moreover, in the perturbations level we found that there is an instability in the model which arises from negative sound speed squared.

 

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