Evidence for planet engulfment by the star HD82943

Israelian, G.; Santos, N. C.; Mayor, M.; Rebolo, R.

doi:10.1038/35075512

Cited by 175 publications

(191 citation statements)

References 19 publications

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“…In particular, we will start with the families of periodic orbits corresponding to the masses of the system HD 82943. Although the elements of this system have been revised several times, the fit given by Israelian et al (2001), that we shall use here, is enough for our purpose. The elements of this fit are: m 0 = 1.05M SUN , m 1 sin i = 0.88 MJ, m 2 sin i = 1.63 MJ, a 1 = 0.73 AU, a 2 = 1.16 AU, e 1 = 0.54 ± 0.05, and e 2 = 0.41 ± 0.08.…”

Section: Factors That Affect the Stability Of A Planetary Systemmentioning

confidence: 99%

“…In many planetary systems with two planets close to each other, the two planets are in mean motion resonance. Examples are: HD 82943 (Israelian et al 2001;Mayor et al 2004), Gliese 876 (Marcy et al 2001;Rivera and Lissauer 2001), at the 2:1 resonance and 55Cnc at the 3:1 resonance . Some of these systems have large eccentricities and are evidently stable.…”

Section: Introductionmentioning

confidence: 99%

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Symmetric and asymmetric librations in extrasolar planetary systems: a global view

Hadjidemetriou

2006

Celestial Mech Dyn Astr

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We present a global view of the resonant structure of the phase space of a planetary system with two planets, moving in the same plane, as obtained from the set of the families of periodic orbits. An important tool to understand the topology of the phase space is to determine the position and the stability character of the families of periodic orbits. The region of the phase space close to a stable periodic orbit corresponds to stable, quasi periodic librations. In these regions it is possible for an extrasolar planetary system to exist, or to be trapped following a migration process due to dissipative forces. The mean motion resonances are associated with periodic orbits in a rotating frame, which means that the relative configuration is repeated in space. We start the study with the family of symmetric periodic orbits with nearly circular orbits of the two planets. Along this family the ratio of the periods of the two planets varies, and passes through rational values, which correspond to resonances. At these resonant points we have bifurcations of families of resonant elliptic periodic orbits. There are three topologically different resonances: (1) the resonances (n + 1):n, (2:1, 3:2, …), (2) the resonances (2n + 1):(2n − 1), (3:1, 5:3, …) and (3) all other resonances. The topology at each one of the above three types of resonances is studied, for different values of the sum and of the ratio of the planetary masses. Both symmetric and asymmetric resonant elliptic periodic orbits exist. In general, the symmetric elliptic families bifurcate from the circular family, and the asymmetric elliptic families bifurcate from the symmetric elliptic families. The results are compared with the position of some observed extrasolar planetary systems. In some cases (e.g., Gliese 876) the observed system lies, with a very good accuracy, on the stable part of a family of resonant periodic orbits.

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Section: Factors That Affect the Stability Of A Planetary Systemmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Symmetric and asymmetric librations in extrasolar planetary systems: a global view

Hadjidemetriou

2006

Celestial Mech Dyn Astr

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“…This mechanism would be efficient only during the first 20-30 Myr or later when the surface convection layers of the star for the first time attains its minimum size configuration (Chavero et al 2010). Israelian et al (2001Israelian et al ( , 2003 found evidence of pollution, suggesting the infall of a planet, in HD 82943 (see, however, Mandell et al 2004;Ghezzi et al 2009). The self-enrichment scenario could lead to a relative overabundance of refractories, such as Si, Mg, Ca, Ti, and the iron-group elements, compared to volatiles, such as C, N, O, S, and Zn.…”

Section: Introductionmentioning

confidence: 99%

CNO behaviour in planet-harbouring stars

Suárez-Andrés

Israelian

Hernández

et al. 2016

A&A

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Context. Carbon, nitrogen, and oxygen (CNO) are key elements in stellar formation and evolution, and their abundances should also have a significant impact on planetary formation and evolution. Aims. We present a detailed spectroscopic analysis of 74 solar-type stars, 42 of which are known to harbour planets. We determine the nitrogen abundances of these stars and investigate a possible connection between N and the presence of planetary companions. Methods. We used VLT/UVES to obtain high-resolution near-UV spectra of our targets. Spectral synthesis of the NH band at 3360 Å was performed with the spectral synthesis codes MOOG and FITTING. Results. We identify several spectral windows from which accurate N abundance can be obtained. Nitrogen distributions for stars with and without planets show that planet hosts are nitrogen-rich when compared to single stars. However, given the linear trend between [N/Fe] vs. [Fe/H], this fact can be explained as being due to the metal-rich nature of planet hosts. Conclusions. We conclude that reliable N abundances can be derived for metal-rich solar type stars from the near UV molecular band at 3360 Å. We confirm a linear trend between [N/Fe] and metallicity expected from standard models of Galactic chemical evolution.

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“…Planet migration affects the star's angular momentum, which might also have an impact on log Li . Finally, the ingestion of a planet can increase the surface lithium abundance (e.g., Montalbán & Rebolo 2002;Israelian et al 2001).…”

Section: Introductionmentioning

confidence: 99%

Lithium depletion in solar-like stars: no planet connection

Baumann

Ramírez

Meléndez³

et al. 2010

A&A

167

188

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We have determined precise stellar parameters and lithium abundances in a sample of 117 stars with basic properties very similar to the Sun. This sample selection reduces biasing effects and systematic errors in the analysis. We estimate the ages of our sample stars mainly from isochrone fitting but also from measurements of rotation period and X-ray luminosity and test the connection between lithium abundance, age, and stellar parameters. We find strong evidence for increasing lithium depletion with age. Our sample includes 14 stars that are known to host planets and it does not support recent claims that planet-host stars have experienced more lithium depletion than stars without planets. We find the solar lithium abundance normal for a star of its age, mass, and metallicity. Furthermore, we analyze published data for 82 stars that were reported to support an enhanced lithium depletion in planet hosts. We show that those stars in fact follow an age trend very similar to that found with our sample and that the presence of giant planets is not related to low lithium abundances. Finally, we discuss the systematic biases that led to the incorrect conclusion of an enhanced lithium depletion in planet-host stars.

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Evidence for planet engulfment by the star HD82943

Cited by 175 publications

References 19 publications

Symmetric and asymmetric librations in extrasolar planetary systems: a global view

Symmetric and asymmetric librations in extrasolar planetary systems: a global view

CNO behaviour in planet-harbouring stars

Lithium depletion in solar-like stars: no planet connection

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