Extrasolar planets and brown dwarfs around A-F type stars

Borgniet, S.; Boisse, I.; Lagrange, Anne-Marie; Bouchy, F.; Arnold, L.; Díaz, R. F.; Galland, F.; Delorme, P.; Hébrard, G.; Santerne, A.; Ehrenreich, D.; Ségransan, D.; Bonfils, X.; Delfosse, X.; Santos, N. C.; Forveille, T.; Moutou, C.; Udry, S.; Eggenberger, A.; Pepe, F.; Astudillo, N.; Montagnier, G.

doi:10.1051/0004-6361/201321783

Cited by 29 publications

(51 citation statements)

References 49 publications

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“…3.1.1. The HD 113337 system Summary of first planet detection -We reported the detection of a giant planet orbiting around HD 113337 and characterized it in Borgniet et al (2014), hereafter BO14. HD 113337 (HIP 63584) is a F6V star with a 1.41 M stellar mass (Allende Prieto & Lambert, 1999), a slight infrared excess attributed to a cold debris disk (Rhee et al, 2007), and may be relatively young (possible age of 150 ± 100 Myr, see BO14).…”

Section: Giant Planetsmentioning

confidence: 99%

“…Most of the observations were made in the course of the SP4 program within the SOPHIE consortium (Bouchy et al, 2009). The first results of our SOPHIE survey, regarding the complex RV variations of HD 185395 and the detection of a ∼3 M Jup GP orbiting with a ∼320-day period around HD 113337, were presented in Desort et al (2009) and Borgniet et al (2014), respectively. This paper first presents our SOPHIE survey and its results, and then presents a statistical analysis combining our SOPHIE and HARPS targets from Paper IX to make a single, global study.…”

Section: Introductionmentioning

confidence: 99%

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Extrasolar planets and brown dwarfs around AF-type stars

Borgniet

Lagrange

Meunier

et al. 2017

A&A

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Context. The impact of the stellar mass on the giant planet properties is still to be fully understood. Main-Sequence (MS) stars more massive than the Sun remain relatively unexplored in radial velocity (RV) surveys, due to their characteristics that hinder classical RV measurements. Aims. Our aim is to characterize the close (up to ∼2 au) giant planet (GP) and brown dwarf (BD) population around AF MS stars and compare this population to stars with different masses. Methods. We used the SOPHIE spectrograph located on the 1.93m telescope at Observatoire de Haute-Provence to observe 125 northern, MS AF dwarfs. We used our dedicated SAFIR software to compute the RV and other spectroscopic observables. We characterized the detected substellar companions and computed the GP and BD occurrence rates combining the present SOPHIE survey and a similar HARPS survey. Results. We present new data on two known planetary systems around the F5-6V dwarfs HD 16232 and HD 113337. For the latter, we report an additional RV variation that might be induced by a second GP on a wider orbit. We also report the detection of fifteen binaries or massive substellar companions with high-amplitude RV variations or long-term RV trends. Based on 225 targets observed with SOPHIE and/or HARPS, we constraint the BD frequency within 2-3 au around AF stars to be below 4% (1σ). For Jupiter-mass GP within 2-3 au (periods ≤ 10 3 days), we found the occurrence rate to be 3.7 +3 −1 % around AF stars with masses < 1.5 M , and to be ≤ 6% (1σ) around AF stars with masses > 1.5 M . For periods smaller than 10 days, we find the GP occurrence rate to be below 3 or 4.5% (1σ), respectively. Our results are compatible with the GP frequency reported around FGK dwarfs and are compatible with a possible increase of GP orbital periods with the stellar mass as predicted by formation models. Description of the SOPHIE survey SampleOur SOPHIE sample is made of 125 AF MS dwarf stars with spectral types in the range A0V to F9V. We detail the physical properties of our sample in Appendix A. We selected our targets using the same selection process as for our HARPS survey (see more details in Lagrange et al., 2009, Paper IX and Appendix B). Briefly, our selection relies on the following criteria: i) the spectral type; ii) the distance to the Sun, and iii) the exclusion of known SB2 binary, chemically peculiar stars, or confirmed δ Scuti or γ Doradus pulsators. We ended up with 125 targets with B − V in the range -0.02 to 0.56, v sin i in the range 3 to 250 km.s −1 , and masses in the range 1 to 2.5 M (Fig. 1). Note that the exclusion of known pulsators results in a visible dichotomy between our ∼Aand ∼F-type targets. ObservationsWe observed our 125 SOPHIE targets mainly between November 2006 and April 2014. We made some additional observations later (2015)(2016) to complete our survey for the targets with the less data and to further monitor the most interesting targets. We acquired the SOPHIE spectra in high-resolution mode (R ∼75000), in the 3872-6943 Å wavelength range. As...

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Section: Giant Planetsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Extrasolar planets and brown dwarfs around AF-type stars

Borgniet

Lagrange

Meunier

et al. 2017

A&A

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“…8 in Jones et al 2014), which curiously is the same interval where no planets are observed around giants, suggests that these planets might be destroyed when stars evolve to the red giant branch. Intriguingly, the first results of a survey to search for planets around earlier A-F type dwarfs (e.g., Galland et al 2005b;Lagrange et al 2009) have revealed planets with orbital eccentricities above 0.2 (Galland et al 2005a;Desort et al 2008;Borgniet et al 2014). It will be interesting to see more results from this ongoing survey.…”

Section: Eccentricitymentioning

confidence: 99%

Stellar parameters and chemical abundances of 223 evolved stars with and without planets

Jofré

Petrucci

Saffe

et al. 2015

A&A

128

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Aims. We present fundamental stellar parameters, chemical abundances, and rotational velocities for a sample of 86 evolved stars with planets (56 giants; 30 subgiants), and for a control sample of 137 stars (101 giants; 36 subgiants) without planets. The analysis was based on both high signal-to-noise and resolution echelle spectra. The main goals of this work are i) to investigate chemical differences between evolved stars that host planets and those of the control sample without planets; ii) to explore potential differences between the properties of the planets around giants and subgiants; and iii) to search for possible correlations between these properties and the chemical abundances of their host stars. Implications for the scenarios of planet formation and evolution are also discussed. Methods. The fundamental stellar parameters (T eff , log g, [Fe/H], ξ t ) were computed homogeneously using the FUNDPAR code. The chemical abundances of 14 elements (Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Zn, and Ba) were obtained using the MOOG code. Rotational velocities were derived from the full width at half maximum of iron isolated lines. Results. In agreement with previous studies, we find that subgiants with planets are, on average, more metal-rich than subgiants without planets by ∼0.16 dex. The [Fe/H] distribution of giants with planets is centered at slightly subsolar metallicities and there is no metallicity enhancement relative to the [Fe/H] distribution of giants without planets. Furthermore, contrary to recent results, we do not find any clear difference between the metallicity distributions of stars with and without planets for giants with M > 1.5 M . With regard to the other chemical elements, the analysis of the [X/Fe] distributions shows differences between giants with and without planets for some elements, particularly V, Co, and Ba. Subgiants with and without planets exhibit similar behavior for most of the elements. On the other hand, we find no evidence of rapid rotation among the giants with planets or among the giants without planets. Finally, analyzing the planet properties, some interesting trends might be emerging: i) multi-planet systems around evolved stars show a slight metallicity enhancement compared with single-planet systems; ii) planets with a 0.5 AU orbit subgiants with [Fe/H] > 0 and giants hosting planets with a 1 AU have [Fe/H] < 0; iii) higher-mass planets tend to orbit more metal-poor giants with M ≤ 1.5 M , whereas planets around subgiants seem to follow the planet-mass metallicity trend observed on dwarf hosts; iv) [X/Fe] ratios for Na, Si, and Al seem to increase with the mass of planets around giants; v) planets orbiting giants show lower orbital eccentricities than those orbiting subgiants and dwarfs, suggesting a more efficient tidal circularization or the result of the engulfment of close-in planets with larger eccentricities.

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“…However, some recent programs have been monitoring also more massive stars, such as evolved subgiants and giants (e.g., Hatzes et al 2006;Döllinger et al 2009;Niedzielski et al 2009;Johnson et al 2011;Sato et al 2013) as well as A-F-type mainsequence stars (e.g., Galland et al 2005;Guenther et al 2009;Hartmann et al 2010;Borgniet et al 2014). One of our targets was the roAp star HD 42659.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

A radial-velocity survey of Ap stars with HARPS

Hartmann

Hatzes

2015

A&A

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Context. Chemically peculiar Ap stars are main-sequence stars of spectral type B8-F3 which show large overabundances of some chemical elements (e.g., Si, Sr, Cr), especially of rare-earth elements, compared to normal A-type stars. Furthermore, they have strong, global magnetic fields and low rotational velocities. Some Ap stars exhibit high-overtone, low-degree, non-radial p-mode pulsations with periods of 6-24 min and are called rapidly oscillating Ap (roAp) stars. Interestingly, no roAp star is known to be a spectroscopic binary (SB), while many non-oscillating Ap (noAp) stars are found in SB systems. Aims. The goal of this survey was to carry out a systematic search for sub-stellar and stellar companions around Ap stars. Methods. Between 2004 and 2009, we observed 65 chemically peculiar stars with the HARPS spectrograph at the 3.6-m telescope at the European Southern Observatory (La Silla, Chile). The radial-velocity (RV) measurements were obtained using a new software called HARPS-TERRA which is based on a least-squares matching of each individual spectrum to a high signal-to-noise ratio template for each star. Results. We find significant variability with a period of 93.2 days and a semi-amplitude of 11.85 km s −1 in the RVs of HD 42659, a star of our sample that belongs to the group of roAp stars. This variability is caused by a stellar companion with a minimum mass of 0.47 M in a slightly eccentric (e = 0.146) orbit at a separation of 0.55 AU.Conclusions. This detection makes HD 42659 the first confirmed SB around a roAp star in a relatively close orbit. It shows that tidal interactions in binaries do not necessarily inhibit pulsations in Ap stars.

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Extrasolar planets and brown dwarfs around A-F type stars

Cited by 29 publications

References 49 publications

Extrasolar planets and brown dwarfs around AF-type stars

Extrasolar planets and brown dwarfs around AF-type stars

Stellar parameters and chemical abundances of 223 evolved stars with and without planets

A radial-velocity survey of Ap stars with HARPS

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