An eccentric companion at the edge of the brown dwarf desert orbiting the 2.4<i>M</i><sub>⊙</sub>giant star HIP 67537

Jones, M. I.; Brahm, R.; Wittenmyer, Robert A.; Drass, H.; Jenkins, James S.; Melo, C.; Vos, J.; Rojo, P.

doi:10.1051/0004-6361/201630278

Cited by 34 publications

(50 citation statements)

References 90 publications

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“…These authors estimated the upper limit of the occurrence rate of BDs around these stars to be below 4%. An occurrence rate of 1.6% for BDs around intermediate-mass giant and main-sequence stars was estimated by Jones et al [236], which is slightly higher than the rate around lower mass stars. A similar occurrence rate of about 2% for BDs orbiting white dwarfs (these are typically progeny of AF-type main sequence stars) was determined by Girven et al [237] 29 , again giving a tentative evidence that BD formation might be more efficient around massive stars.…”

Section: Very Massive Giants and Metallicitymentioning

confidence: 78%

“…A similar occurrence rate of about 2% for BDs orbiting white dwarfs (these are typically progeny of AF-type main sequence stars) was determined by Girven et al [237] 29 , again giving a tentative evidence that BD formation might be more efficient around massive stars. Interestingly, the parent stars of the BD candidates detected in Jones et al [236] are metal-rich. According to the CA model of Mordasini et al [19] the formation of super-massive planets and BDs are possible in massive and metal-rich disks at large distances.…”

Section: Very Massive Giants and Metallicitymentioning

confidence: 89%

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Heavy Metal Rules. I. Exoplanet Incidence and Metallicity

Adibekyan

2019

Geosciences

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Discovery of only handful of exoplanets required to establish a correlation between giant planet occurrence and metallicity of their host stars. More than 20 years have already passed from that discovery, however, many questions are still under lively debate: What is the origin of that relation? what is the exact functional form of the giant planet -metallicity relation (in the metal-poor regime)?, does such a relation exist for terrestrial planets? All these question are very important for our understanding of the formation and evolution of (exo)planets of different types around different types of stars and are subject of the present manuscript. Besides making a comprehensive literature review about the role of metallicity on the formation of exoplanets, I also revisited most of the planet -metallicity related correlations reported in the literature using a large and homogeneous data provided by the SWEET-Cat catalog. This study lead to several new results and conclusions, two of which I believe deserve to be highlighted in the abstract: i) The hosts of sub-Jupiter mass planets (∼0.6 -0.9 M ) are systematically less metallic than the hosts of Jupiter-mass planets. This result might be related to the longer disk lifetime and higher amount of planet building materials available at high metallicities, which allow a formation of more massive Jupiter-like planets. ii) Contrary to the previous claims, our data and results do not support the existence of a breakpoint planetary mass at 4 M above and below which planet formation channels are different. However, the results also suggest that planets of the same (high) mass can be formed through different channels depending on the (disk) stellar mass i.e. environmental conditions.

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Section: Very Massive Giants and Metallicitymentioning

confidence: 78%

Section: Very Massive Giants and Metallicitymentioning

confidence: 89%

Heavy Metal Rules. I. Exoplanet Incidence and Metallicity

Adibekyan

2019

Geosciences

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“…The close BD occurrence rate for solar-mass stars is estimated to be <1% for P < 5 yr (or sma 3 au; see Grether & Lineweaver 2006) and around 0.6% for P 1 yr (Sahlmann et al 2011;Grieves et al 2017). Jones et al (2017) have found an occurrence rate of 1.2 1.5 −0.4 % for BD companions within 5 au around evolved intermediate-mass giant stars off the main-sequence (1.6 2 −0.5 % when restricted to stars ≥1.5 M ), A87, page 17 of 30 A&A 621, A87 (2019) 1-13 1-10 84 0 0.2 0.5 0-1.8 0-3 ≤1.8 (Jupiters) 71 0 0.4 1.4 0-4.5 0-7.6 ≤4.5 95 0 0.1 0.9 0-2.8 0-4.8 ≤2.8 10-100 72 0 0.4 0.6 0-2.1 0-3.5 ≤2.1 49 0 1 2 0-6.5 0-11 ≤6.5 91 0 0.1 0.9 0-2.9 0-5 ≤2.9 100-1000 58 4 2.9 3.1 2.2-5.5 1.2-7.9 3.1 +2.4 −0.9 30 0 2.3 3.2 0-10.4 0-17.7 ≤10.4 82 4 0.9 4.1 2.9-7.1 1.6-10.2 4.1 +3 −1.2 1-100 78 0 0.3 0.6 0-1.9 0-3.2 ≤1.9 60 0 0.7 1.6 0-5.3 0-9 ≤5.3 93 0 0.1 0.9 0-2.9 0-4.9 ≤2.9 1-1000 71 4 1.6 2.5 1.8-4.5 1-6.4 2.5 +2 −0.7 50 0 1 2 0-6.3 0-10.8 ≤6.3 89 4 0.5 3.7 2.6-6.5 1.5-9.3 3.7 +2.8 −1.1 0.3-1 (Saturns) 1-10 76 0 0.3 1.1 0-3.5 0-6 ≤3.5 10-100 56 0 0.8 1.5 0-4.8 0-8.2 ≤4.8 100-1000 31 0 2.2 2.7 0-8.6 0-14.7 ≤8.6 1-100 66 0 0.5 1.3 0-4.1 0-6.9 ≤4.1 1-1000 54 0 0.8 1.5 0-4.9 0-8.4 ≤4.9…”

Section: Results From the Combined Sophie + Harps Surveymentioning

confidence: 99%

Extrasolar planets and brown dwarfs around AF-type stars

Borgniet

Lagrange

Meunier

et al. 2019

A&A

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Context. The impact of stellar mass on the properties of giant planets is still not fully understood. Main-sequence (MS) stars more massive than the Sun remain relatively unexplored in radial velocity (RV) surveys, due to their characteristics which 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 1.93 m 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 15 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 constrain the BD frequency within 2–3 au around AF stars to be below 4% (1σ). For Jupiter-mass GPs within 2–3 au (periods ≤103 days), we find the occurrence rate to be 3.7−1+3% around AF stars with masses <1.5 M⊙, and to be ≤6% (1σ) around AF stars with masses >1.5 M⊙. For periods shorter than 10 days, we find the GP occurrence rate to be below 3 and 4.5% (1σ), respectively. Our results are compatible with the GP frequency reported around FGK dwarfs and are compatible with a possible increase in GP orbital periods with stellar mass as predicted by formation models.

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“…Omiya et al 2009;Johnson et al 2010;Reffert et al 2015;Jones et al 2017). When Paper I was published, only 6 substellar companions 9 were known around stars more massive than ∼ 1.78 M and they presented much higher masses on average than for lower mass stars (see Fig.…”

Section: Discussionmentioning

confidence: 99%

Planets around evolved intermediate-mass stars

Mena

Santos

Silva

et al. 2018

A&A

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Aims. The aim of this work is to search for planets around intermediate-mass stars in open clusters by using data from an extensive survey with more than 15 years of observations. Methods. We obtain high-precision radial velocities (RV) with the HARPS spectrograph for a sample of 142 giant stars in 17 open clusters. We fit Keplerian orbits when a significant periodic signal is detected. We also study the variation of stellar activity indicators and line-profile variations to discard stellar-induced signals.Results. We present the discovery of a periodic RV signal compatible with the presence of a planet candidate in the 1.15 Gyr open cluster IC4651 orbiting the 2.06 M star No. 9122. If confirmed, the planet candidate would have a minimum mass of 7.2M J and a period of 747 days. However, we also find that the FWHM of the CCF varies with a period close to the RV, casting doubts on the planetary nature of the signal. We also provide refined parameters for the previously discovered planet around NGC2423 No. 3 but show evidence that the BIS of the CCF is correlated with the RV during some of the observing periods. This fact advises us that this might not be a real planet and that the RV variations could be caused by stellar activity and/or pulsations. Finally, we show that the previously reported signal by a brown dwarf around NGC4349 No. 127 is presumably produced by stellar activity modulation. Conclusions. The long-term monitoring of several red giants in open clusters has allowed us to find periodic RV variations in several stars. However, we also show that the follow-up of this kind of stars should last more than one orbital period to detect long-term signals of stellar origin. This work warns that although it is possible to detect planets around red giants, large-amplitude, long-period RV modulations do exist in such stars that can mimic the presence of an orbiting planetary body. Therefore, we need to better understand how such RV modulations behave as stars evolve along the Red Giant Branch and perform a detailed study of all the possible stellar-induced signals (e.g. spots, pulsations, granulation) to comprehend the origin of RV variations.

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An eccentric companion at the edge of the brown dwarf desert orbiting the 2.4M_⊙giant star HIP 67537

Cited by 34 publications

References 90 publications

Heavy Metal Rules. I. Exoplanet Incidence and Metallicity

Heavy Metal Rules. I. Exoplanet Incidence and Metallicity

Extrasolar planets and brown dwarfs around AF-type stars

Planets around evolved intermediate-mass stars

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An eccentric companion at the edge of the brown dwarf desert orbiting the 2.4M⊙giant star HIP 67537

Cited by 34 publications

References 90 publications

Heavy Metal Rules. I. Exoplanet Incidence and Metallicity

Heavy Metal Rules. I. Exoplanet Incidence and Metallicity

Extrasolar planets and brown dwarfs around AF-type stars

Planets around evolved intermediate-mass stars

Contact Info

Product

Resources

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An eccentric companion at the edge of the brown dwarf desert orbiting the 2.4M_⊙giant star HIP 67537