Proton Conductive Membrane Based on Polyelectrolyte Complex Preparation and Its Ionic Conductivity

Kamada, Masaya; Umeda, Minoru; Yamada, Akifumi; Uchida, Isamu

doi:10.4139/sfj.54.1028

Cited by 1 publication

(5 citation statements)

References 14 publications

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“…1) appears different from k −2 for k τ −1 , we have confirmed that this is owing to the limitation of the simulation time (see Ref. [47]). …”

supporting

confidence: 71%

“…While details are given in Ref. [47], we stress that our results are independent of the choices of the time step, simulation size, and grid size by changing their values by a factor of 50%. Initial fluctuations of the field value are seeded by the vacuum fluctuations though we have checked that our results are qualitatively insensitive to the detailed form of the initial conditions.…”

Section: Results Of Numerical Simulationsmentioning

confidence: 99%

“…If the flat direction has a non-renormalizable superpotential, the resultant GW background is generally too small to be detected [47]. Thus, we consider the case that the superpotential of the flat direction is absent due to discrete R-symmetries.…”

Section: Dynamics Of Flat Directionmentioning

confidence: 99%

“…Also in this case, GWs are emitted by the dynamics of randomly distributed Nambu-Goldstone modes of the flat direction [30][31][32][33][34]47], though cosmic strings are absent. 3 Since d 2 V (φ)/dφ 2 ∼ H 2 (t) at φ = φ , a typical width of cosmic strings is of the order of the Hubble radius.…”

Section: Caluculation Of Gwsmentioning

confidence: 99%

“…The functions f A and f B are calculated by matching solutions of the Einstein equation in the oscillation era with that in the radiation dominated era at τ = τ RH such as [47] …”

Section: T T Ijmentioning

confidence: 99%

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Gravitational waves as a probe of the SUSY scale

Kamada

Yamada

2015

Phys. Rev. D

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We investigate the sources of the Hubble-induced mass for a flat direction in supersymmetric theories and show that the sign of the Hubble-induced mass generally changes just after the end of inflation. This implies that global cosmic strings generally form after the end of inflation in most supersymmetric models, including the Minimal Supersymmetric Standard Model. The cosmic strings emit gravitational waves whose frequency corresponds to the Hubble scale, until they disappear when the Hubble parameter decreases down to the soft mass of the flat direction. As a result, the peak frequency of gravitational waves is related to the supersymmetric scale. The observation of this gravitational wave signal will give us information of supersymmetric scale and reheating temperature.Introduction. The observation of gravitational waves (GWs) will open a new window onto the early Universe and provide information on physics at correspondingly high energy scales [1]. Stochastic GW signals are generated by non-equilibrium phenomena during the post-inflationary period, such as preheating [2][3][4][5][6][7][8] [40]. The observation of these GW signals will improve our understanding on particle physics beyond the Standard Model.

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“…1) appears different from k −2 for k τ −1 , we have confirmed that this is owing to the limitation of the simulation time (see Ref. [47]). …”

supporting

confidence: 71%

Section: Results Of Numerical Simulationsmentioning

confidence: 99%

Section: Dynamics Of Flat Directionmentioning

confidence: 99%

Section: Caluculation Of Gwsmentioning

confidence: 99%

“…The functions f A and f B are calculated by matching solutions of the Einstein equation in the oscillation era with that in the radiation dominated era at τ = τ RH such as [47] …”

Section: T T Ijmentioning

confidence: 99%

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