A Definition for Giant Planets Based on the Mass–density Relationship

Hatzes, A. P.; Rauer, H.

doi:10.1088/2041-8205/810/2/l25

Cited by 147 publications

(121 citation statements)

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“…Since the mass and radius measurements for both planets are affected in the same way by the systematic uncertainties of the stellar parameters, the diversity of exoplanets (e.g., Hatzes & Rauer 2015) cannot be entirely explained by problems in the determination of the stellar parameters. As shown in Fig.…”

Section: Discussionmentioning

confidence: 99%

K2-106, a system containing a metal-rich planet and a planet of lower density

Guenther

Barragán

Dai

et al. 2017

A&A

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Aims. Planets in the mass range from 2 to 15 M ⊕ are very diverse. Some of them have low densities, while others are very dense. By measuring the masses and radii, the mean densities, structure, and composition of the planets are constrained. These parameters also give us important information about their formation and evolution, and about possible processes for atmospheric loss. Methods. We determined the masses, radii, and mean densities for the two transiting planets orbiting K2-106. The inner planet has an ultra-short period of 0.57 days. The period of the outer planet is 13.3 days. . Conclusions. Since the system contains two planets of almost the same mass, but different distances from the host star, it is an excellent laboratory to study atmospheric escape. In agreement with the theory of atmospheric-loss processes, it is likely that the outer planet has a hydrogen-dominated atmosphere. The mass and radius of the inner planet is in agreement with theoretical models predicting an iron core containing 80 +20 −30 % of its mass. Such a high metal content is surprising, particularly given that the star has an ordinary (solar) metal abundance. We discuss various possible formation scenarios for this unusual planet.

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Section: Discussionmentioning

confidence: 99%

K2-106, a system containing a metal-rich planet and a planet of lower density

Guenther

Barragán

Dai

et al. 2017

A&A

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“…This casts doubts on the proposed distinction between BDs and planets, which is thought to be connected to different formation mechanisms. Hatzes & Rauer (2015) proposed that objects in the mass range 0.3-62 M Jup follow the same relationship on the observed mass-density plot, so they should be considered to belong to one and the same class of celestial objects. Based on planet population synthesis, Mordasini et al (2009) showed that the core-accretion mechanism proposed for giant planet formation may produce planets not only more massive than 13M Jup , i.e., above the deuterium burning limit (Burrows et al 2001), but also in the 20-40M Jup range.…”

Section: The Sample Of Brown Dwarfs Transiting Main Sequence Starsmentioning

confidence: 99%

EPIC 219388192b—An Inhabitant of the Brown Dwarf Desert in the Ruprecht 147 Open Cluster

Nowak

Πάλλη

Gandolfi

et al. 2017

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We report the discovery of EPIC 219388192b, a transiting brown dwarf in a 5.3 day orbit around a member star of Ruprecht 147, the oldest nearby open cluster association, which was photometrically monitored by K2 during its Campaign 7. We combine the K2 time-series data with ground-based adaptive optics imaging and high-resolution spectroscopy to rule out false positive scenarios and determine the main parameters of the system. EPIC 219388192b has a radius of 1.01 0.03 R e , effective temperature T eff =5850± 85K, and iron abundance [Fe/H]=0.03±0.08dex. Its age, spectroscopic distance, and reddening are consistent with those of Ruprecht 147, corroborating its cluster membership. EPIC 219388192b is the first mature brown dwarf with precise determinations of mass, radius, and age, and serves as benchmark for evolutionary models in the substellar regime.

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“…Radial velocity measurements 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/608/A129 around 2 R Jup (Sato et al 2005;Anderson et al 2010), a range in size which also corresponds to late M dwarfs with masses lower than ∼0.2 M (Chabrier & Baraffe 1997;Baraffe et al 1998Baraffe et al , 2015Dotter et al 2008;Demory et al 2009;Díaz et al 2014;Hatzes & Rauer 2015;Chen & Kipping 2017). To further the comparison, gas giants, brown dwarfs, and very low-mass stars also have similar temperatures in addition to similar sizes.…”

Section: Introductionmentioning

confidence: 99%

The EBLM Project

Triaud

Martin

Ségransan

et al. 2017

A&A

125

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We present 2271 radial velocity measurements taken on 118 single-line binary stars, taken over eight years with the CORALIE spectrograph. The binaries consist of F/G/K primaries and M dwarf secondaries. They were initially discovered photometrically by the WASP planet survey, as their shallow eclipses mimic a hot Jupiter transit. The observations we present permit a precise characterisation of the binary orbital elements and mass function. With modelling of the primary star, this mass function is converted to a mass of the secondary star. In the future, this spectroscopic work will be combined with precise photometric eclipses to draw an empirical mass/radius relation for the bottom of the mass sequence. This has applications in both stellar astrophysics and the growing number of exoplanet surveys around M dwarfs. In particular, we have discovered 34 systems with a secondary mass below 0.2 M , and so we will ultimately double the number of known very low-mass stars with well-characterised masses and radii. The quality of our data combined with the amplitude of the Doppler variations mean that we are able to detect eccentricities as small as 0.001 and orbital periods to sub-second precision. Our sample can revisit some earlier work on the tidal evolution of close binaries, extending it to low mass ratios. We find some exceptional binary systems that are eccentric at orbital periods below three days, while our longest circular orbit has a period of 10.4 days. Amongst our systems, we note one remarkable architecture in J1146-42 that boasts three stars within one astronomical unit. By collating the EBLM binaries with published WASP planets and brown dwarfs, we derive a mass spectrum with twice the resolution of previous work. We compare the WASP/EBLM sample of tightly bound orbits with work in the literature on more distant companions up to 10 AU. We note that the brown dwarf desert appears wider, as it carves into the planetary domain for our short-period orbits. This would mean that a significantly reduced abundance of planets begins at ∼3 M Jup , well before the deuterium-burning limit. This may shed light on the formation and migration history of massive gas giants.

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A Definition for Giant Planets Based on the Mass–density Relationship

Cited by 147 publications

References 28 publications

K2-106, a system containing a metal-rich planet and a planet of lower density

K2-106, a system containing a metal-rich planet and a planet of lower density

EPIC 219388192b—An Inhabitant of the Brown Dwarf Desert in the Ruprecht 147 Open Cluster

The EBLM Project

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