The 'second parameter': A memory from the globular cluster formation epoch

Noam Soker*, Ron Hadar

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

13 Scopus citations

Abstract

We study the correlations between the distribution of stars on the horizontal branch (HB), the HB morphology, and some other properties of globular clusters (GCs) in a large sample of GCs. We strengthen previous results that a general correlation exists only between HB morphology and metallicity. Correlations with other properties, e.g. central density and core radius, exist only for GCs within a narrow metallicity range. We conjecture that the lack of correlations with present properties of GCs (besides metallicity) is because the variation of the HB morphologies between GCs having similar metallicities is caused by a process, or processes, the effect of which was determined at the formation time of GCs. This process (or processes) is historically termed the 'second parameter', metallicity being the 'first parameter'. We then argue that the 'planet second parameter' model, where the presence of planets and to a lesser degree brown dwarfs and low-mass main-sequence stars is the 'second parameter', fits this conjecture. This is because the processes that determine the presence of planets and their properties occur during the formation epoch of the star and its circumstellar disc.

Original languageEnglish
Pages (from-to)213-217
Number of pages5
JournalMonthly Notices of the Royal Astronomical Society
Volume324
Issue number1
DOIs
StatePublished - 11 Jun 2001
Externally publishedYes

Keywords

  • Binaries: close
  • Globular clusters: general
  • Planetary systems
  • Stars: horizontal branch

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