CH star

If there is something that has always fascinated us, it is CH star. Since time immemorial, CH star has been an object of study, admiration and debate. Whether for its impact on history, its influence on culture, or its relevance in today's society, CH star continues to be a topic of great interest to academics, professionals, and the curious alike. In this article, we will thoroughly explore all aspects related to CH star, from its origins to its impact on the modern world. Through a thorough and enriching analysis, we hope to expand our knowledge and understanding of CH star, and perhaps even discover new facets that surprise us. Join us on this fascinating journey through CH star, and together we will unravel its mysteries and meanings. Do not miss it!

CH stars are particular type of carbon stars which are characterized by the presence of exceedingly strong absorption bands due to CH (methylidyne) in their spectra. They belong to the stellar population II, meaning they are metal poor and generally pretty middle-aged stars, and are under-luminous compared to the classical C–N carbon stars. The term 'CH star' was coined by Philip C. Keenan in 1942 as a sub-type of the C classification, which he used for carbon stars. The main molecular feature used in identifying the initial set of five CH stars lies in the Fraunhaufer G band.

In 1975, Yasuho Yamashita noted that some higher temperature carbon stars displayed the typical spectral characteristics of a CH star, but did not have the same kinematic properties. That is, they did not have the higher space velocities characteristic of the older stellar population. These were dubbed CH-like stars. Many CH stars are known to be members of binary star systems, and it is reasonable to believe this is (or was) the case for all CH stars. Like Barium stars, they are probably the result of a mass transfer from a former classical carbon star companion, now a degenerate white dwarf, to the current CH-classed star.

References

  1. ^ McClure, Robert D.; Woodsworth, A. W. (April 1, 1990), "The binary nature of the barium and CH stars. III - Orbital parameters", Astrophysical Journal, Part 1, 352: 709–723, Bibcode:1990ApJ...352..709M, doi:10.1086/168573.
  2. ^ Hearnshaw, John B. (2014), The Analysis of Starlight: Two Centuries of Astronomical Spectroscopy (2nd ed.), Cambridge University Press, p. 233, ISBN 978-1107782914.
  3. ^ Sperauskas, J.; et al. (July 2016), "The Binary Nature of CH-Like Stars", The Astrophysical Journal, 826 (1): 13, Bibcode:2016ApJ...826...85S, doi:10.3847/0004-637X/826/1/85, 85.
  4. ^ Goswami, Aruna (2005). "CH stars at high Galactic latitudes". Monthly Notices of the Royal Astronomical Society. 359 (2): 531–544. arXiv:astro-ph/0507202. Bibcode:2005MNRAS.359..531G. doi:10.1111/j.1365-2966.2005.08917.x. S2CID 14521922.

External links

  • David Darling. "CH star". Retrieved 2 January 2009.
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