Pulsation-driven Mass Loss from Massive Stars behind Stellar Mergers in Metal-poor Dense Clusters

Daisuke Nakauchi, Kohei Inayoshi, Kazuyuki Omukai

Research output: Contribution to journalArticlepeer-review

Abstract

The recent discovery of high-redshift (z > 6) supermassive black holes (SMBH) favors the formation of massive seed BHs in protogalaxies. One possible scenario is the formation of massive stars via runaway stellar collisions in a dense cluster, leaving behind massive BHs without significant mass loss. We study the pulsational instability of massive stars with the zero-age main-sequence (ZAMS) mass and metallicity, and discuss whether or not pulsation-driven mass loss prevents massive BH formation. In the MS phase, the pulsational instability excited by the-mechanism grows in. As the stellar mass and metallicity increase, the mass-loss rate increases to In the red supergiant (RSG) phase, the instability is excited by the κ-mechanism operating in the hydrogen ionization zone and grows more rapidly in The RSG mass-loss rate is almost independent of metallicity and distributes in the range of Conducting stellar structure calculations including feedback due to pulsation-driven winds, we find that the stellar models of can leave behind remnant BHs more massive than We conclude that massive merger products can seed monster SMBHs observed at.

Original languageEnglish
Article number81
JournalAstrophysical Journal
Volume902
Issue number1
DOIs
Publication statusPublished - 2020 Oct 10

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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