Boyajian’s Star B: The Co-moving Companion to KIC 8462852 A

Pearce, Logan; Kraus, Adam L.; Dupuy, Trent J.; Mann, Andrew W.; Huber, Daniel

doi:10.3847/1538-4357/abdd33

Cited by 8 publications

(2 citation statements)

References 47 publications

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“…Although a number of explanations have been proposed, none has been fully satisfactory (Wright & Sigurdsson 2016). For further discussions of this star, I refer the reader to Boyajian et al (2018) and Bodman et al (2018) and to Pearce et al (2021) for more recent references and a new hypothesis to explain the behavior.…”

Section: Introductionmentioning

confidence: 99%

A Search for Analogs of KIC 8462852 (Boyajian’s Star): A Proof of Concept and the First Candidates

Schmidt

2019

ApJ

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The seemingly normal F dwarf, KIC 8462852 (a.k.a. Boyajian's Star), has been observed to exhibit two types of behavior unique among known variable stars: infrequent episodes of small brightness dips and a long-term decline in brightness between the dips. No satisfactory mechanism has been found for this behavior, at least in part, because there is only one known example. To begin to rectify this, we have searched for other stars exhibiting similar dipping behavior using the Northern Sky Variability Survey and have used data from the All Sky Automated Survey for Supernovae to further investigate the behavior. Twenty-one stars are identified as possible dippers. Fifteen may be similar to Boyajian's star and the other six are likely to be more extreme examples of the same phenomenon. Using data from the Gaia Second Data Release we show that the dipper candidates are located in two restricted regions of the H-R diagram, near the main sequence with masses near 1 solar mass and in the red giant region near the evolutionary track for 2 solar mass stars. Stars in the former group are considered to be likely analogs to Boyajian's star and should be studied in more detail to gain insights into the dipping phenomenon.

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Section: Introductionmentioning

confidence: 99%

A Search for Analogs of KIC 8462852 (Boyajian’s Star): A Proof of Concept and the First Candidates

Schmidt

2019

ApJ

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“…However, the results of Mustill et al (2021) suggest that this is indeed plausible, in part due to the fact that the periastron distance of the binary is likely to be significantly smaller than the current projected separation (see Section 3.2). To this point, it is important to note that the orbits of wide binaries vary over time due to stellar flybys and interactions with the Galactic tide (Kaib et al 2013;Pearce et al 2021;Mustill et al 2021), such that even binaries with large semi-major axes (∼10 4 AU) may undergo periods where the periastron distance reaches as low as ∼100 AU, where dynamical interactions with inner planetary systems are greatly amplified (Kaib et al 2013;. Thus, the importance of the Kozai-Lidov effect in exciting planetary eccentricities cannot be discounted, even for very widely separated multi-star systems.…”

Section: Stellar Multiplicity and The Formation Of Highly Eccentric P...mentioning

confidence: 99%

An Edge-On Orbit for the Eccentric Long-Period Planet HR 5183 b

Venner,

Pearce,

Vanderburg

2021

Preprint

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The long-period giant planet HR 5183 b has one of the most extreme orbits among exoplanets known to date. In this work we use Hipparcos-Gaia astrometry to measure the orbital inclination of this planet for the first time. We measure 𝑖 = 89.9 +13.3• −13.5 , fully consistent with an edge-on orbit. The previously reported long orbital period and high eccentricity of HR 5183 b are supported by our results, with 𝑃 = 102 +84 −34 years and 𝑒 = 0.87 ± 0.04. We confirm that HIP 67291 forms a physically bound binary with HR 5183 at a projected separation of 15400 AU, and derive new constraints on the orbit of this pair. We combine our inclination measurements in an attempt to measure the mutual inclination between the planetary and binary orbits; while there is some evidence for misalignment, we conclude that this is not statistically significant. Further observations, especially the release of the full Gaia astrometric data, will allow for improved constraints on the planet-binary mutual inclination in this system. 52 ± 16% of known planets with eccentricities 𝑒 ≥ 0.8 are found in multiple star systems, a rate that we find to be greater than for the overall planet population to moderate significance (𝑝 = 0.0075). This supports the hypothesis that dynamical interactions with wide stellar companions plays an important role in the formation of highly eccentric exoplanets.

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TOI-858 B b: A hot Jupiter on a polar orbit in a loose binary

Hagelberg,

Nielsen,

Attia

et al. 2023

A&A

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We report the discovery of a hot Jupiter on a 3.28-day orbit around a 1.08 M⊙ G0 star that is the secondary component in a loose binary system. Based on follow-up radial velocity observations of TOI-858 B with CORALIE on the Swiss 1.2 m telescope and CHIRON on the 1.5 m telescope at the Cerro Tololo Inter-American Observatory (CTIO), we measured the planet mass to be 1.10−0.07+0.08 MJ. Two transits were further observed with CORALIE to determine the alignment of TOI-858 B b with respect to its host star. Analysis of the Rossiter-McLaughlin signal from the planet shows that the sky-projected obliquity is λ = 99.3−3.7+3.8°. Numerical simulations show that the neighbour star TOI-858 A is too distant to have trapped the planet in a Kozai–Lidov resonance, suggesting a different dynamical evolution or a primordial origin to explain this misalignment. The 1.15 M⊙ primary F9 star of the system (TYC 8501-01597-1, at ρ ~11″) was also observed with CORALIE in order to provide upper limits for the presence of aplanetary companion orbiting that star.

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Boyajian’s Star B: The Co-moving Companion to KIC 8462852 A

Cited by 8 publications

References 47 publications

A Search for Analogs of KIC 8462852 (Boyajian’s Star): A Proof of Concept and the First Candidates

A Search for Analogs of KIC 8462852 (Boyajian’s Star): A Proof of Concept and the First Candidates

An Edge-On Orbit for the Eccentric Long-Period Planet HR 5183 b

TOI-858 B b: A hot Jupiter on a polar orbit in a loose binary

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