CEMP star

In this article, we will delve into the fascinating world of CEMP star and its impact on today's society. From its origins to its relevance today, CEMP star has been the subject of study and interest by academics, researchers and enthusiasts from different disciplines. This article aims to analyze the influence of CEMP star on various aspects of our daily lives, as well as its role in shaping our culture, values ​​and beliefs. Through an interdisciplinary approach, we will explore the many facets of CEMP star, shedding light on its importance and meaning in the contemporary context.

Carbon-enhanced metal-poor stars, usually referred to as CEMP stars, are a class of chemically peculiar star. CEMP stars have > +1, which means compared to the Sun these stars have carbon enhanced at least ten times more than iron, and < -1, meaning that iron is less than a tenth that in the Sun.

These are further categorized by whether r-process or s-process elements are enhanced. CEMP-no stars have no enhancement. Some of these are the earliest formed in the Milky Way. The others are termed CEMP-r, CEMP-s, or CEMP-r/s.[1][2] Metal-poor stars are more likely to be CEMP stars, and once < -5.0, then all the stars are CEMP stars.[1]

Subdivisions

CEMP-r stars have > +1 and < 0.[1]

CEMP-s stars have > +1 and > +0.5[1] 80% of CEMP stars fall into this category.[1]

CEMP-r/s stars have between 0 and +0.5 so they are under the level for CEMP-s stars.[1]

CEMP-no stars have < 0.[1] About 20% of CEMP stars fall into this category.[1]

References

  1. ^ a b c d e f g h Catherine r. Kennedy (29 May 2014). "Carbon-Enhanced Metal-Poor Stars in the Milky Way" (PDF). Canberra. Archived from the original (PDF) on October 19, 2015. Retrieved 18 December 2016.
  2. ^ Carollo, Daniela; Freeman, Ken; Beers, Timothy; Placco, Vinicius; Tumlinson, Jason; Martell, Sarah (20 June 2014). "Carbon-Enhanced Metal-Poor Stars: CEMP-s and CEMP-no Sub-Classes in the Halo System of the Milky Way". The Astrophysical Journal. 788 (2): 180. arXiv:1401.0574. Bibcode:2014ApJ...788..180C. doi:10.1088/0004-637X/788/2/180. S2CID 59932382.


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