Adelman, S. J.Çalışkan, H.Gulliver, A. F.Teker, Ayşegül2016-04-192016-04-192006-02http://hdl.handle.net/11413/1005We performed elemental abundances analyses of the mercury-manganese (HgMn) stars 53 Tau, beta Tau, and gamma Crv consistent with previous studies of similar stars in this series. The derived v sin i values for the last two stars are 59 and 32 km s(-1), respectively, both of which are greater than those of HgMn stars previously Studied. For 53 Tau this analysis using Selected wavelength regions replaces one performed with coadded photographic spectra. A stricter upper limit is placed on any Hg II lambda 3984 line. The abundances of beta Tau are usually greater than those of gamma Crv. But the later star has a Hg II lambda 3984 line which the former lacks. Our analysis of v Her, which was performed with spectrograms obtained with CCD detectors, is extended by using additional spectrograms to increase the range of wavelengths covered longward of lambda 4800. Minor changes in the derived abundances result.en-USstars : abundancesstars : individual : 53 Taustars : individual : beta Taustars : individual : gamma Crvstars : individual : upsilon Herstars : chemically peculiarsingly ionized siliconpeculiar b-starsA Type StarsOscillator-StrengthsTransition-ProbabilitiesRotational VelocitiesTerm SystemHgmn StarsY-IISolar AbundanceYıldız: BolluklarıYıldız : Bireysel: 53 TauYıldız : Bireysel : Beta TauYıldız : Bireysel : Gama CrvYıldız : Özgü KimyasalTek Başına Iyonize SilikonOsilatör-GüçlüGeçiş OlasılıklarıDönme HızlarıVadeli SistemGüneş BollukArticle235544100033235544100033