Eclipse timing variations to detect possible Trojan planets in binary systems

Schwarz, Richard P.; Bazsó, Ákos; Funk, B.; Zechner, R.

doi:10.1093/mnras/stv1823

Cited by 7 publications

(7 citation statements)

References 42 publications

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“…Despite the absence of discoveries of Trojan planets around main-sequence stars (but see Goździewski & Konacki 2006), the problem has received renewed attention in terms of planet formation and evolution ( Leleu, Robutel & Correia 2015), and detections by transit photometry (Ford & Gaudi 2006;Ford & Holman 2007;Janson 2013;Vokrouhlický & Nesvorný 2014;Placek et al 2015) and binary eclipses (Schwarz et al 2015).…”

Section: O -O R B I Ta L Dy Na M I C Smentioning

confidence: 99%

Dynamical mass and multiplicity constraints on co-orbital bodies around stars

Veras

Marsh

Gänsicke

2016

Mon. Not. R. Astron. Soc.

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Objects transiting near or within the disruption radius of both main-sequence (e.g. KOI 1843) and white dwarf (WD 1145+017) stars are now known. Upon fragmentation or disintegration, these planets or asteroids may produce co-orbital configurations of nearly equal mass objects. However, as evidenced by the co-orbital objects detected by transit photometry in the WD 1145+017 system, these bodies are largely unconstrained in size, mass, and total number (multiplicity). Motivated by potential future similar discoveries, we perform N-body simulations to demonstrate if and how debris masses and multiplicity may be bounded due to second-to-minute deviations and the resulting accumulated phase shifts in the osculating orbital period amongst multiple co-orbital equal point masses. We establish robust lower and upper mass bounds as a function of orbital period deviation, but find the constraints on multiplicity to be weak. We also quantify the fuzzy instability boundary, and show that mutual collisions occur in less than 5, 10, and 20 per cent of our simulations for masses of 10 21 , 10 22 , and 10 23 kg. Our results may provide useful initial rough constraints on other stellar systems with multiple co-orbital bodies.

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Section: O -O R B I Ta L Dy Na M I C Smentioning

confidence: 99%

Dynamical mass and multiplicity constraints on co-orbital bodies around stars

Veras

Marsh

Gänsicke

2016

Mon. Not. R. Astron. Soc.

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“…Several techniques have been proposed to detect these bodies; these involve transit timing variations (e.g., Schwarz et al 2015;Ford & Holman 2007;Vokrouhlický & Nesvorný 2014;Haghighipour et al 2013), transits (e.g., Janson 2013; Hippke & Angerhausen 2015), and radial velocity (Ford & Gaudi 2006;Leleu et al 2015). These techniques have been used in previous attempts to detect these bodies, especially with Kepler data (e.g., Hippke & Angerhausen 2015;Janson 2013) and archival radial velocity (e.g., Ford & Holman 2007;Madhusudhan & Winn 2009).…”

Section: Introductionmentioning

confidence: 99%

The TROY project: Searching for co-orbital bodies to known planets

Lillo-Box

Barrado

Figueira

et al. 2018

A&A

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Context. The detection of Earth-like planets, exocomets or Kuiper belts show that the different components found in the solar system should also be present in other planetary systems. Trojans are one of these components and can be considered fossils of the first stages in the life of planetary systems. Their detection in extrasolar systems would open a new scientific window to investigate formation and migration processes. Aims. In this context, the main goal of the TROY project is to detect exotrojans for the first time and to measure their occurrence rate (η-Trojan). In this first paper, we describe the goals and methodology of the project. Additionally, we used archival radial velocity data of 46 planetary systems to place upper limits on the mass of possible trojans and investigate the presence of co-orbital planets down to several tens of Earth masses. Methods. We used archival radial velocity data of 46 close-in (P < 5 days) transiting planets (without detected companions) with information from high-precision radial velocity instruments. We took advantage of the time of mid-transit and secondary eclipses (when available) to constrain the possible presence of additional objects co-orbiting the star along with the planet. This, together with a good phase coverage, breaks the degeneracy between a trojan planet signature and signals coming from additional planets or underestimated eccentricity. Results. We identify nine systems for which the archival data provide >1σ evidence for a mass imbalance between L4 and L5. Two of these systems provide >2σ detection, but no significant detection is found among our sample. We also report upper limits to the masses at L4/L5 in all studied systems and discuss the results in the context of previous findings.

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“…2. Other, more exotic orbits in binaries have been considered, such as trojan planets near L4 and L5 (Dvorak 1986;Schwarz et al 2015) and halo orbits near L1, L2 and L3 (Howell 1983). No such planets have been discovered though.…”

Section: Orbital Configurationsmentioning

confidence: 99%

Populations of Planets in Multiple Star Systems

Martin

2018

Handbook of Exoplanets

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Astronomers have discovered that both planets and binaries are abundant throughout the Galaxy. In combination, we know of over 100 planets in binary and higher-order multi-star systems, in both circumbinary and circumstellar configurations. In this chapter we review these findings and some of their implications for the formation of both stars and planets. Most of the planets found have been circumstellar, where there is seemingly a ruinous influence of the second star if sufficiently close ( 50 AU). Hosts of hot Jupiters have been a particularly popular target for binary star studies, showing an enhanced rate of stellar multiplicity for moderately wide binaries (beyond ∼ 100 AU). This was thought to be a sign of Kozai-Lidov migration, however recent studies have shown this mechanism to be too inefficient to account for the majority of hot Jupiters. A couple of dozen circumbinary planets have been proposed around both main sequence and evolved binaries. Around main sequence binaries there are preliminary indications that the frequency of gas giants is as high as those around single stars. There is however a conspicuous absence of circumbinary planets around the tightest main sequence binaries with periods of just a few days, suggesting a unique, more disruptive formation history of such close stellar pairs.

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Eclipse timing variations to detect possible Trojan planets in binary systems

Cited by 7 publications

References 42 publications

Dynamical mass and multiplicity constraints on co-orbital bodies around stars

Dynamical mass and multiplicity constraints on co-orbital bodies around stars

The TROY project: Searching for co-orbital bodies to known planets

Populations of Planets in Multiple Star Systems

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