Precession of the nodes in some triple stellar systems.

Mazeh, T.; Shaham, J.

doi:10.1086/182110

Cited by 184 publications

(269 citation statements)

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“…About 20-30 % of the Kepler binaries are in fact fairly tight triple systems (Rappaport et al 2013), which is compatible with what is found in the 100 pc solar neighbourhood (Tokovinin et al 2006), and Gaia will easily identify these triple-star systems. It is likely that tertiary stars, if close enough, will disrupt any circumbinary protoplanetary discs, and hence inhibit planet formation (Mazeh & Shaham 1979). This effectively increases the planet rate to ∼13 %.…”

Section: Resultsmentioning

confidence: 99%

Gaia's potential for the discovery of circumbinary planets

Sahlmann

Triaud

Martin

2014

Monthly Notices of the Royal Astronomical Society

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The abundance and properties of planets orbiting binary stars -circumbinary planets -are largely unknown because they are difficult to detect with currently available techniques. Results from the Kepler satellite and other studies indicate a minimum occurrence rate of circumbinary giant planets of ∼10 %, yet only a handful are presently known. Here, we study the potential of ESA's Gaia mission to discover and characterise extrasolar planets orbiting nearby binary stars by detecting the binary's periodic astrometric motion caused by the orbiting planet. We expect that Gaia will discover hundreds of giant planets around binaries with FGK dwarf primaries within 200 pc of the Sun, if we assume that the giant planet mass distribution and abundance are similar around binaries and single stars. If on the other hand all circumbinary gas giants have masses lower than two Jupiter masses, we expect only four detections. Gaia is critically sensitive to the properties of giant circumbinary planets and will therefore make the detailed study of their population possible. Gaia's precision is such that the distribution in mutual inclination between the binary and planetary orbital planes will be obtained. It also possesses the capacity to establish the frequency of planets across the H-R diagram, both as a function of mass and of stellar evolutionary state from pre-main sequence to stellar remnants. Gaia's discoveries can reveal whether a second epoch of planetary formation occurs after the red-giant phase.

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Section: Resultsmentioning

confidence: 99%

Gaia's potential for the discovery of circumbinary planets

Sahlmann

Triaud

Martin

2014

Monthly Notices of the Royal Astronomical Society

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“…If it is real, a possible explanation which we are proposing here is that circumbinary planets form or migrated preferentially close to the dynamical stability limits (Martin et al 2013), but they are strongly affected by evaporation effects and then reduced to compact remnants, making their detection challenging. An alternative hypothesis, also mentioned in Welsh et al (2014), is that the closest binary systems (P < 3−5 d) do not form circumbinary planets at all, possibly because they very often have tertiary stellar companions (Tokovinin et al 2006) that may have played a role in the tightening of the orbit of the inner binary (e.g., through Kozai interactions, see Mazeh & Shaham 1979). This evolution is expected to be disruptive for circumbinary planets.…”

Section: Discussionmentioning

confidence: 99%

Effects of X-ray and extreme UV radiation on circumbinary planets

Sanz-Forcada

Desidera

Micela

2014

A&A

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Context. Several circumbinary planets have recently been discovered. The orbit of a planet around a binary stellar system poses several dynamic constraints. In addition to these constraints, the effects that radiation from the host stars may have on the planet atmospheres must be considered. We here evaluate these effects. Because of the configuration of a close binary system, these stars have a high rotation rate, even for old stars. The fast rotation of close, tidally locked binaries causes a permanent state of high stellar activity and copious XUV radiation. The accumulated effects are stronger than for normal exoplanets around single stars and cause a faster evaporation of their atmospheres. Aims. We evaluate the effects that stellar radiation has on the evaporation of exoplanets around binary systems and on the survival of these planets. Methods. We considered the X-ray and EUV spectral ranges (XUV, 1-912 Å) to account for the photons that are easily absorbed by a planet atmosphere that is mainly composed of hydrogen. A more complex atmospheric composition is expected to absorb this radiation more efficiently. We used direct X-ray observations to evaluate the energy in the X-rays range and coronal models to calculate the (nondetectable) EUV part of the spectrum. Results. We considered in this problem different configurations of stellar masses, and a resonance of 4:1 and 3:1. The simulations show that exoplanets orbiting close binary systems in a close orbit will suffer strong photoevaporation that may cause a total loss of atmosphere in a short time. We also applied our models to the best real example, Kepler-47 b, to estimate the current mass-loss rates in circumbinary planets and the accumulated effects over the time. Conclusions. A binary system of two solar-like stars will be highly efficient in evaporating the atmosphere of the planet (less than 6 Gyr in our case). These systems will be difficult to find, even if they are dynamically stable. Still, planets may orbit around binary systems of low mass stars for wider orbits. Currently known circumbinary planets are not substantially affected by thermal photoevaporation processes, unless Kepler-47 b has an inflated atmosphere. The distribution of the orbital periods of circumbinary planets is shifted to much longer periods than the average of Kepler planets, which supports a scenario of strong photoevaporation in close-in circumbinary planets.

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“…Changes in the eccentricity have been examined numerically by Mazeh & Shaham (1979) and both analytically and numerically by Sö derhjelm (1984). Their results showed that even if the short-period system attained a circular orbit, its eccentricity would be modulated.…”

Section: Discussionmentioning

confidence: 99%

The Quadruple System μ Orionis: Three-dimensional Orbit and Physical Parameters

Fekel¹,

Scarfe²,

Barlow³

et al. 2002

The Astronomical Journal

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The star l Orionis is a spectroscopic visual quadruple system in which each visual component is a shortperiod spectroscopic binary. The visual orbit has a period of 18.644 yr, a high eccentricity of 0.7426, and a high inclination of 96=2. The visual primary consists of an Am star and probably a G or early K dwarf that orbit each other in a nearly circular orbit with a period of 4.4475858 days. The visual secondary consists of a pair of F5: V stars in a circular orbit with a period of 4.7835361 days. While the masses of the two stars are nearly identical and the magnitude difference between the pair is close to zero, the projected rotational velocities differ by almost a factor of 2. The orbit for the B subsystem is not coplanar with the visual orbit, while that for the A subsystem is probably not coplanar as well. The orbital parallax of 0>02107 AE 0>00018 is more accurate than that obtained from the Hipparcos observations and corresponds to a distance of 47.5 AE 0.4 pc. A comparison with evolutionary tracks indicates that the Am star is near the end of its main-sequence evolution.

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Precession of the nodes in some triple stellar systems.

Cited by 184 publications

References 0 publications

Gaia's potential for the discovery of circumbinary planets

Gaia's potential for the discovery of circumbinary planets

Effects of X-ray and extreme UV radiation on circumbinary planets

The Quadruple System μ Orionis: Three-dimensional Orbit and Physical Parameters

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