Statistical properties of brown dwarf companions: implications for different formation mechanisms

Ma, Bo; Ge, Jian

doi:10.1093/mnras/stu134

Cited by 139 publications

(232 citation statements)

References 127 publications

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“…This last one, HIP5158b, should probably be considered a planetary candidate given its minimum mass of 15 ± 10 M Jup . This increasing number of long-period BD companions reinforces the observation that the number of BDs increases with orbital period, as pointed out by Ma & Ge (2014). All our BD candidates have an eccentricity higher than 0.45 except for the lightest one, HD 209262b, with e = 0.35.…”

Section: Discussionsupporting

confidence: 89%

“…Tables 5-9 (RV data) are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/585/A46 (e.g., Grether & Lineweaver 2006;Sahlmann et al 2011;Ma & Ge 2014). Statistical properties of BD companions, such as frequency, separation, eccentricity, and mass ratio distribution, as well as the relation of these properties to their host stars, should permit us to distinguish between different formation and evolution models.…”

Section: Introductionmentioning

confidence: 99%

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The SOPHIE search for northern extrasolar planets

Bouchy

Ségransan

Díaz

et al. 2015

A&A

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Long-period brown dwarf companions detected in radial velocity surveys are important targets for direct imaging and astrometry to calibrate the mass-luminosity relation of substellar objects. Through a 20-yr radial velocity monitoring of solar-type stars that began with ELODIE and was extended with SOPHIE spectrographs, giant exoplanets and brown dwarfs with orbital periods longer than ten years are discovered. We report the detection of five new potential brown dwarfs with minimum masses between 32 and 83 M Jup orbiting solar-type stars with periods longer than ten years. An upper mass limit of these companions is provided using astrometric H data, high-angular resolution imaging made with PUEO, and a deep analysis of the cross-correlation function of the main stellar spectra to search for blend effects or faint secondary components. These objects double the number of known brown dwarf companions with orbital periods longer than ten years and reinforce the conclusion that the occurrence of such objects increases with orbital separation. With a projected separation larger than 100 mas, all these brown dwarf candidates are appropriate targets for high-contrast and high angular resolution imaging.

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Section: Discussionsupporting

confidence: 89%

Section: Introductionmentioning

confidence: 99%

The SOPHIE search for northern extrasolar planets

Bouchy

Ségransan

Díaz

et al. 2015

A&A

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“…These objects have orbital periods of less than 400 days and thus are rare members of the so-called brown-dwarf desert (Armitage & Bonnell 2002). The orbital periods probed by Kepler and our observations correspond to the "driest region" of this desert (Ma & Ge 2014;Ranc et al 2015). In spite of their very low number, we can derive a first measurement of their occurrence rate.…”

Section: Occurrence Rate Of Brown Dwarfs In the Brown-dwarf Desertmentioning

confidence: 58%

SOPHIE velocimetry ofKeplertransit candidates

Santerne

Moutou

Tsantaki

et al. 2016

A&A

269

263

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While giant extrasolar planets have been studied for more than two decades now, there are still some open questions as to their dominant formation and migration processes, as well as to their atmospheric evolution in different stellar environments. In this paper, we study a sample of giant transiting exoplanets detected by the Kepler telescope with orbital periods up to 400 days. We first defined a sample of 129 giant-planet candidates that we followed up with the SOPHIE spectrograph (OHP, France) in a 6-year radial velocity campaign. This allowed us to unveil the nature of these candidates and to measure a false-positive rate of 54.6 ± 6.5% for giant-planet candidates orbiting within 400 days of period. Based on a sample of confirmed or likely planets, we then derived the occurrence rates of giant planets in different ranges of orbital periods. The overall occurrence rate of giant planets within 400 days is 4.6 ± 0.6%. We recovered, for the first time in the Kepler data, the different populations of giant planets reported by radial velocity surveys. Comparing these rates with other yields, we find that the occurrence rate of giant planets is lower only for hot Jupiters but not for the longer-period planets. We also derive a first measurement of the occurrence rate of brown dwarfs in the brown-dwarf desert with a value of 0.29 ± 0.17%. Finally, we discuss the physical properties of the giant planets in our sample. We confirm that giant planets receiving moderate irradiation are not inflated, but we find that they are on average smaller than predicted by formation and evolution models. In this regime of low-irradiated giant planets, we find a possible correlation between their bulk density and the iron abundance of the host star, which needs more detections to be confirmed.

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“…In this sense, the Neptunian desert might be similar to the short-period brown-dwarf desert (e.g., Grether & Lineweaver 2006;Cheetham et al 2015;Bouchy et al 2016), in the range of ∼20−80 M Jup , which distinguishes between planets and stellar companions (e.g., Armitage & Bonnell 2002;Ma & Ge 2014;Brandt et al 2014;Thies et al 2015). The two deserts, which are located apart by a factor of 300 in mass, indicate three distinctive populations of short-period companions: stellar companions, Jovian planets, and super-Earth planets.…”

Section: Discussionmentioning

confidence: 99%

Dearth of short-period Neptunian exoplanets: A desert in period-mass and period-radius planes

Mazeh

Holczer

Faigler

2016

A&A

315

351

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A few studies have reported a significant dearth of exoplanets with Neptune mass and radius with orbital periods below 2-4 d. This cannot be explained by observational biases because many Neptunian planets with longer orbital periods have been detected. The existence of this desert is similar to the appearance of the so-called brown-dwarf desert that suggests different formation mechanisms of planets and stellar companions with short orbital periods. Similarly, the Neptunian desert might indicate different mechanisms of formation and evolution for hot Jupiters and short-period super-Earths. We here follow a previous study and examine the location and shape of the desert in both the period-mass and period-radius planes, using the currently available large samples of planets. The desert in the period-mass plane has a relatively sharp upper edge, with a planetary mass that is inversely proportional to the planetary orbital period, while the lower, somewhat blurred, boundary is located along masses that are apparently linearly proportional to the period. The desert in the period-radius plane of the transiting planets is less clear. It seems as if the radius along the upper boundary is inversely proportional to the period to the power of one-third, while the lower boundary shows a radius that is proportional to the period to the power of two-thirds. The combination of the two upper bounds of the desert, in the period-mass and period-radius planes, yields a planetary mass-radius relation of R p /R Jup (1.2 ± 0.3)(M p /M Jup ) 0.27 ± 0.11 for 0.1 M p /M Jup 1. The derived shape of the desert, which might extend up to periods of 5-10 d, could shed some light on the formation and evolution of close-in planets.

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Statistical properties of brown dwarf companions: implications for different formation mechanisms

Cited by 139 publications

References 127 publications

The SOPHIE search for northern extrasolar planets

The SOPHIE search for northern extrasolar planets

SOPHIE velocimetry ofKeplertransit candidates

Dearth of short-period Neptunian exoplanets: A desert in period-mass and period-radius planes

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