期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 511, 期 4, 页码 4710-4723出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stab3619
关键词
binaries(including multiple): close; stars: individual: TIC 470710327; stars: massive
资金
- LSSTC, NSF Cybertraining [1829740]
- Brinson Foundation
- Moore Foundation
- UK Science and Technology Facilities Council (STFC) [ST/R505006/1, ST/S000488]
- European Research Council (ERC) under the European Union [865624]
- NOVA
- European Research Council under the European Union [670519:MAMSIE]
- Research Foundation Flanders [G0A2917N]
- Netherlands Research Council NWO [VENI 639.041.645]
- NAWI Graz
- FWO PhD fellowship [11E1721N]
- IAC from the Spanish Ministry of Science, Innovation and Universities (MCIU) [P/308614]
- NASA [NAS 5-26555]
- NASA Office of Space Science [NNX13AC07G]
- NASA Explorer Program
- Research Foundation -Flanders (FWO), Belgium
- Research Council of KU Leuven, Belgium
- Fonds National de la Recherche Scientifique (F.R.S.-FNRS), Belgium
- Royal Observatory of Belgium
- Observatoire de Geneve, Switzerland
- Thuringer Landessternwarte Tautenburg, Germany
- European Research Council (ERC) [865624] Funding Source: European Research Council (ERC)
We report the discovery and analysis of a massive, compact, hierarchical triple star system identified by citizen scientists in data obtained by NASA's TESS. Follow-up observations and dynamical modeling reveal that the system is comprised of three OB stars, with a compact eclipsing binary and a non-eclipsing tertiary star. The non-eclipsing tertiary star is more massive than the combined mass of the inner binary, suggesting future phases of mass transfer and potential evolution into a double neutron star or a Thorne-Zytkow object.
We report the discovery and analysis of a massive, compact, hierarchical triple system (TIC 470710327) initially identified by citizen scientists in data obtained by NASA's Transiting Exoplanet Survey Satellite (TESS). Spectroscopic follow-up observations obtained with the hermes spectrograph, combined with eclipse-timing variations (ETVs), confirm that the system is comprised of three OB stars, with a compact 1.10 d eclipsing binary and a non-eclipsing tertiary on a 52.04 d orbit. Dynamical modelling of the system (from radial velocity and ETVs) reveal a rare configuration wherein the tertiary star (O9.5-B0.5V; 14-17 M-circle dot) is more massive than the combined mass of the inner binary (10.9-13.2 M-circle dot). Given the high mass of the tertiary, we predict that this system will undergo multiple phases of mass transfer in the future, and likely end up as a double neutron star gravitational wave progenitor or an exotic Thorne-Zytkow object. Further observational characterization of this system promises constraints on both formation scenarios of massive stars as well as their exotic evolutionary end-products.
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