Mergers prompted by dynamics in compact, multiple-star systems: a stellar-reduction case for the massive triple TIC 470710327. (arXiv:2204.10600v2 [astro-ph.SR] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Vigna_Gomez_A/0/1/0/all/0/1">Alejandro Vigna-Gómez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_B/0/1/0/all/0/1">Bin Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguilera_Dena_D/0/1/0/all/0/1">David R. Aguilera-Dena</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grishin_E/0/1/0/all/0/1">Evgeni Grishin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramirez_Ruiz_E/0/1/0/all/0/1">Enrico Ramirez-Ruiz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soares_Furtado_M/0/1/0/all/0/1">Melinda Soares-Furtado</a>
TIC 470710327, a massive compact hierarchical triple-star system, was
recently identified by NASA’s Transiting Exoplanet Survey Satellite (TESS). TIC
470710327 is comprised of a compact (1.10 d) circular eclipsing binary, with
total mass $approx 10.9-13.2 rm{M_{odot}}$, and a more massive ($approx
14-17 rm{M_{odot}}$) eccentric non-eclipsing tertiary in a $52.04$ d orbit.
Here we present a progenitor scenario for TIC 470710327 in which ‘2+2’
quadruple dynamics result in Zeipel-Lidov-Kozai (ZLK) resonances that lead to a
contact phase of the more massive binary. In this scenario, the two binary
systems should form in a very similar manner, and dynamics trigger the merger
of the more massive binary either during late phases of star formation or
several Myr after the zero-age main sequence (ZAMS), when the stars begin to
expand. Any evidence that the tertiary is a highly-magnetised ($sim 1-10$ kG),
slowly-rotating blue main-sequence star would hint towards a quadruple origin.
Finally, our scenario suggests that the population of inclined, compact
multiple-stellar systems is reduced into co-planar systems, via mergers, late
during star formation or early in the main sequence. The elucidation of the
origin of TIC 470710327 is crucial in our understanding of multiple
massive-star formation and evolution.
TIC 470710327, a massive compact hierarchical triple-star system, was
recently identified by NASA’s Transiting Exoplanet Survey Satellite (TESS). TIC
470710327 is comprised of a compact (1.10 d) circular eclipsing binary, with
total mass $approx 10.9-13.2 rm{M_{odot}}$, and a more massive ($approx
14-17 rm{M_{odot}}$) eccentric non-eclipsing tertiary in a $52.04$ d orbit.
Here we present a progenitor scenario for TIC 470710327 in which ‘2+2’
quadruple dynamics result in Zeipel-Lidov-Kozai (ZLK) resonances that lead to a
contact phase of the more massive binary. In this scenario, the two binary
systems should form in a very similar manner, and dynamics trigger the merger
of the more massive binary either during late phases of star formation or
several Myr after the zero-age main sequence (ZAMS), when the stars begin to
expand. Any evidence that the tertiary is a highly-magnetised ($sim 1-10$ kG),
slowly-rotating blue main-sequence star would hint towards a quadruple origin.
Finally, our scenario suggests that the population of inclined, compact
multiple-stellar systems is reduced into co-planar systems, via mergers, late
during star formation or early in the main sequence. The elucidation of the
origin of TIC 470710327 is crucial in our understanding of multiple
massive-star formation and evolution.
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