• 한국컴퓨터산업학회논문지
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• 제5권4호
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• pp.491-502
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• 2004

본 논문은 화자 독립의 단독어 인식에 관한 연구로써, FSVQ(first section vector quantization), 퍼지 이론 및 이중 스펙트럼 특징을 이용한 HMM(hidden Markov model) 모델을 제안한다. 제안된 연구 방법에서, 이중 특징 파라메타로써 LPC ？스트럼과 LPC 스트럼의 회귀 계수를 사용한다. 학습 데이터는 몇 개의 구간으로 나누어지며, 첫 번째 구간의 코드북(codebook)을 만든 후, 첫 번째 구간의 코드북으로 부터, 퍼지 개념을 도입하여 확률 값이 큰 순서에 의해 다중 관측열을 구한다. 그 다음, 첫 번째 구간의 관측열을 학습시키고, 같은 방법으로 확률 값을 얻은 단어가 인식되어 진다. 제안된 방법에 의한 인식 실험을 수행하는 것 이외에도 비교를 위하여 다른 방법의 인식 실험을 같은 조건하에서 같은 데이터로 수행하였다. 실험 결과, 본 연구에서 제안한 방법이 다른 방법들보다 인식률이 우수함을 입증하였다. 입증하였다.

• 천문학회보
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• 제38권2호
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• pp.71.1-71.1
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• 2013

Among quadruples or higher multiplicity stars, only a few binary systems have been discovered. They are important targets to understand the formation and evolution of multiple stellar systems because we can obtain accurate stellar parameters from photometric and spectroscopic studies. We present the observational results of this kind of rare object 1SWASP J093010.78+533859.5, for which the doubly eclipsing feature had been detected previously from the SuperWASP photometric archive. Individual PSF photometry for two objects with a separation of about 1.9 arcsec was performed for the first time in this study. Our time-series photometric data show that the brighter object A is an Algol-type detached eclipsing binary with an orbital period of 1.3 days and the fainter B is a W UMa-type contact eclipsing binary with a period of 0.23 days. Using the high-resolution optical spectra, we obtained well-defined radial velocity variations of the system A. Furthermore, stationary spectral lines were detected and should have originated from the other stellar component, which was confirmed by the third object contribution from the light curve analysis. No spectral feature of the system B was detected, probably due to its faintness. We obtained the binary parameters and the absolute dimensions from each light curve synthesis. The primary and secondary components of the system A have a spectral type of K1 and K5 main sequences, respectively. Two components of system B have nearly the same type of K3 main sequence. Light variations at out of eclipses were appeared in both systems, interpreting as the effect of stellar spots on these late spectral type stars. We estimated the distances to the systems A and B individually. They may have similar distances of about 70 pc and seem to be gravitationally bound with a separation of about 130 AU. In conclusion, we suggest that 1SWASP J093010.78+533859.5 is a quintuple stellar system with a hierarchical structure of a triple system A(ab)c and a binary system B(ab).