A 2+1+1 quadruple star system containing the most eccentric, low-mass, short-period, eclipsing binary known
| Autor: | E Han, S A Rappaport, A Vanderburg, B M Tofflemire, T Borkovits, H M Schwengeler, P Zasche, D M Krolikowski, P S Muirhead, M H Kristiansen, I A Terentev, M Omohundro, R Gagliano, T Jacobs, D LaCourse |
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| Jazyk: | angličtina |
| Rok vydání: | 2021 |
| Předmět: |
Earth and Planetary Astrophysics (astro-ph.EP)
general [Binaries] Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science low-mass [Stars] eclipsing [Binaries] late-type [Stars] FOS: Physical sciences Astronomy and Astrophysics close [Binaries] Solar and Stellar Astrophysics (astro-ph.SR) Astrophysics - Earth and Planetary Astrophysics |
| Zdroj: | Han, E, Rappaport, S A, Vanderburg, A, Tofflemire, B M, Borkovits, T, Schwengeler, H M, Zasche, P, Krolikowski, D M, Muirhead, P S, Kristiansen, M H, Terentev, I A, Omohundro, M, Gagliano, R, Jacobs, T & LaCourse, D 2022, ' A 2+1+1 quadruple star system containing the most eccentric, low-mass, short-period, eclipsing binary known ', Monthly Notices of the Royal Astronomical Society, vol. 510, no. 2, pp. 2448–2463 . https://doi.org/10.1093/mnras/stab3507 |
| Popis: | We present an analysis of a newly discovered 2+1 + 1 quadruple system with TESS containing an unresolved eclipsing binary (EB) as part of TIC 121088960 and a close neighbour TIC 121088959. The EB consists of two very low-mass M dwarfs in a highly eccentric (e = 0.709) short-period (P = 3.043 58 d) orbit. Given the large pixel size of TESS and the small separation (3${_{.}^{\prime\prime}}$9) between TIC 121088959 and TIC 121088960 we used light centroid analysis of the difference image between in-eclipse and out-of-eclipse data to show that the EB likely resides in TIC 121088960, but contributes only ∼10 per cent of its light. Radial velocity data were acquired with iSHELL at NASA’s Infrared Facility and the Coudé spectrograph at the McDonald 2.7-m telescope. For both images, the measured RVs showed no variation over the 11 d observational baseline, and the RV difference between the two images was 8 ± 0.3 km s−1. The similar distances and proper motions of the two images indicate that TIC 121088959 and TIC 121088960 are a gravitationally bound pair. Gaia’s large RUWE and astrometric_excess_noise parameters for TIC 121088960, further indicate that this image is the likely host of the unresolved EB and is itself a triple star. We carried out an SED analysis and calculated stellar masses for the four stars, all of which are in the M dwarf regime: 0.19 M⊙ and 0.14 M⊙ for the EB stars and 0.43 M⊙ and 0.39 M⊙ for the brighter visible stars, respectively. Lastly, numerical simulations show that the orbital period of the inner triple is likely the range 1–50 yr. |
| Databáze: | OpenAIRE |
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