The unstable fate of the planet orbiting the A star in the HD 131399 triple stellar system

Veras, Dimitri; Mustill, Alexander J.; Gänsicke, B. T.

doi:10.1093/mnras/stw2821

Cited by 31 publications

(5 citation statements)

References 94 publications

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“…′′ 8 from the main component Aa, challenging its stability in the 3. ′′ 2 outer system where Ba,Bb is a close pair (Veras et al 2017). However, it turned out that this "planet" is actually a background star (Nielsen et al 2017).…”

Section: Planets In Hierarchical Multiple Systemsmentioning

confidence: 99%

The Updated Multiple Star Catalog

Tokovinin

2018

ApJS

153

120

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The catalog of hierarchical stellar systems with three or more components is an update of the original 1997 version of the MSC. For two thousand hierarchies, the new MSC provides distances, component's masses and periods, as well as supplementary information (astrometry, photometry, identifiers, orbits, notes). The MSC content and format are explained, its incompleteness and strong observational selection are stressed. Nevertheless, the MSC can be used for statistical studies and it is a valuable source for planning observations of multiple stars. Rare classes of stellar hierarchies found in the MSC (with 6 or 7 components, extremely eccentric orbits, planar and possibly resonant orbits, hosting planets) are briefly presented. High-order hierarchies have smaller velocity dispersion compared to triples and are often associated with moving groups. The paper concludes by the analysis of the ratio of periods and separations between inner and outer subsystems. In wide hierarchies, the ratio of semimajor axes, estimated statistically, is distributed between 3 and 300, with no evidence of dynamically unstable systems.

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Section: Planets In Hierarchical Multiple Systemsmentioning

confidence: 99%

The Updated Multiple Star Catalog

Tokovinin

2018

ApJS

153

120

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“…All these components dictate the planetary system architecture around the eventual white dwarf (Veras 2016). The current population of white dwarfs in fact primarily arises from A-star progenitors (Tremblay et al 2016), which highlights the importance of accurately determining their masses during the subgiant/giant branch for determining the fate of planetary systems (Veras et al 2017). Based on the reference asteroseismic mass derived in the previous section, we go on in this section to predict the evolution of the Jovian planet orbiting HD 212771 under the effects of tidal forces and stellar mass loss.…”

Section: Post-main-sequence Planetary System Evolutionmentioning

confidence: 99%

Weighing in on the masses of retired A stars with asteroseismology: K2 observations of the exoplanet-host star HD 212771

Campante

Veras

North

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Doppler-based planet surveys point to an increasing occurrence rate of giant planets with stellar mass. Such surveys rely on evolved stars for a sample of intermediate-mass stars (so-called retired A stars), which are more amenable to Doppler observations than their main-sequence progenitors. However, it has been hypothesised that the masses of subgiant and low-luminosity red-giant stars targeted by these surveystypically derived from a combination of spectroscopy and isochrone fitting -may be systematically overestimated. Here, we test this hypothesis for the particular case of the exoplanet-host star HD 212771 using K2 asteroseismology. The benchmark asteroseismic mass (1.45 +0.10 −0.09 M ⊙ ) is significantly higher than the value reported in the discovery paper (1.15 ± 0.08 M ⊙ ), which has been used to inform the stellar massplanet occurrence relation. This result, therefore, does not lend support to the above hypothesis. Implications for the fates of planetary systems are sensitively dependent on stellar mass. Based on the derived asteroseismic mass, we predict the post-mainsequence evolution of the Jovian planet orbiting HD 212771 under the effects of tidal forces and stellar mass loss. ⋆ Based on observations collected at La Silla Observatory (ESO, Chile) with the FEROS spectrograph at the 2.2-m telescope under programme 088.C-0892(A).†

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“…The stellar orbits could have evolved subsequently due to interactions with the natal disks or secular effects". Noticeably, Wagner et al (2016) and Veras et al (2017) have shown that the planet orbit may not be stable over the system lifetime, due to the high ratio between the planet-HD 131399 A separation and the HD 131399BC-HD 131399 A separation.…”

Section: Introductionmentioning

confidence: 99%

Discovery of a stellar companion to HD 131399A

Lagrange

Keppler

Beust

et al. 2017

A&A

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Context. The giant exoplanets imaged on wide orbits (≥10 au) around young stars challenge the classical theories of planet formation. The presence of perturbing bodies could have played a role in the dynamical evolution of the planets once formed. Aims. We aim to search for close companions to HD 131399, a star around which a giant planet has been discovered, at a projected separation of about 80 au. The star also appears to be a member of a wide (320 au) binary system. Methods. We recorded HARPS high resolution spectra in January 2017. Results. We find that HD 131399A is probably seen close to pole-on. We discover a low mass star companion that orbits with a period of about 10 days on a misaligned orbit. Even though the companion does not have an impact on the current dynamical evolution of the planet, it could have played a role in its setting and in clearing the circumstellar disk from which the planet may originate.

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The unstable fate of the planet orbiting the A star in the HD 131399 triple stellar system

Cited by 31 publications

References 94 publications

The Updated Multiple Star Catalog

The Updated Multiple Star Catalog

Weighing in on the masses of retired A stars with asteroseismology: K2 observations of the exoplanet-host star HD 212771

Discovery of a stellar companion to HD 131399A

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