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The Oosterhoff period groups and multiple populations in globular clusters
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  • The Oosterhoff period groups and multiple populations in globular clusters
  • The Oosterhoff period groups and multiple populations in globular clusters
저자명
Jang. Sohee,Lee. Young-Wook,Joo. Seok-Joo,Na. Chongsam
간행물명
천문학회보
권/호정보
2014년|39권 1호|pp.82-82 (1 pages)
발행정보
한국천문학회
파일정보
정기간행물|ENG|
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이 논문은 한국과학기술정보연구원과 논문 연계를 통해 무료로 제공되는 원문입니다.
서지반출

기타언어초록

The presence of multiple populations is now well-established in most globular clusters (GCs) in the Milky Way. In light of this progress, here we suggest a new model explaining the origin of the Sandage period-shift and the difference in mean period of type ab RR Lyrae variables (<Pab>) between the two Oosterhoff groups. In our models, while matching the observed color-magnitude diagrams, the difference in <Pab> is naturally reproduced as the instability strip is occupied by different subpopulations with increasing metallicity. The instability strip in the metal-poor group II clusters is populated by second generation stars (G2) with enhanced helium and CNO abundances, while the RR Lyraes in the metal-rich group I clusters are mostly produced by first generation stars (G1) without these enhancements. This population shift within the instability strip can create the observed period-shift between the two groups, since both helium and CNO abundances play a role in increasing the period of RR Lyrae variables. The presence of more metal-rich Oosterhoff group III clusters having RR Lyraes with longest <Pab> can also be reproduced, if more helium-rich third generation stars (G3) are present in these GCs.