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송두종,Song, Doo-Jong 한국천문학회 2007 天文學論叢 Vol.22 No.4
On the framework of stochastic gravitational wave background(SGWB) by compact binary systems, we studied the strain spectra of SGWB produced by cosmological cataclysmic variables(CV). For this we reviewed the empirical properties of CVs by using newly published CV catalogue and calculated the cosmological densities of CVs considering the galaxy luminosity function and cosmic stellar birth rate function. Assuming the secular evolution of CVs, we calculated the time scale of CV gravitational wave(GW) radiation and derived formulae for the strain spectra of SGWB by cosmological CVs.
건드림된 비앙키 I형 우주 모형과 SACHS-WOLFE 공식
송두종,SONG D. J. 한국천문학회 2001 天文學論叢 Vol.16 No.1
In the framework of the C-gauge condition for the perturbed variables and the linear approximation for the anisotropy of the spacetime, we studied the formulae for the Sachs-Wolfe effect in dust filled and perturbed Bianchi type I universe model. The results were compared with those of the flat Friedmann model.
건드림된 프리이드만 시공간 속의 각지름 거리: 중력파의 효과
송두종,SONG D. J. 한국천문학회 2004 天文學論叢 Vol.19 No.1
On the framework of a linearly perturbed Friedmann-Robertson-Walker spacetime, we derive an expression for the cosmological angular diameter distance affected by scalar and tensor perturbations. Our expression is applicable in linear order to distances in general FRW models. We study the effect of a stocastic gravitaional wave background on the two-point correlation function of the angular diameter distance fluctuations and, on the basis of this we also derive an expression for the power spectrum of the angular diameter distance fluctuations.
비앙키 I 형 시공간 속의 CMBR 흔들림: 중력파의 영향
송두종,Song, D.J. 한국천문학회 2003 天文學論叢 Vol.18 No.1
In the framework of linear perturbation theory and linear approximation of spacetime anisotropy, we investigated the formulae for the CMBR temperature anisotropy and fluctuation spectrum which have their origin in the primordial tensor perturbations of the perturbed Bianchi type I universe model. The resulting formulae were compared with those of the flat Friedmann model.