scholarly journals FRIENDS OF HOT JUPITERS. I. A RADIAL VELOCITY SEARCH FOR MASSIVE, LONG-PERIOD COMPANIONS TO CLOSE-IN GAS GIANT PLANETS

2014 ◽  
Vol 785 (2) ◽  
pp. 126 ◽  
Author(s):  
Heather A. Knutson ◽  
Benjamin J. Fulton ◽  
Benjamin T. Montet ◽  
Melodie Kao ◽  
Henry Ngo ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Giant Planets ◽  
Hot Jupiters ◽  
Long Period ◽  
Gas Giant

scholarly journals Investigating the planet–metallicity correlation for hot Jupiters

2019 ◽  
Vol 491 (3) ◽  
pp. 4481-4487
Author(s):  
Ares Osborn ◽  
Daniel Bayliss
Keyword(s):  
Radial Velocity ◽  
Giant Planet ◽  
Giant Planets ◽  
Similar Process ◽  
Wide Field ◽  
Hot Jupiters ◽  
Galaxy Model ◽  
Gas Giant ◽  
Correlation Consistent

ABSTRACT We investigate the giant planet–metallicity correlation for a homogeneous, unbiased set of 217 hot Jupiters taken from nearly 15 yr of wide-field ground-based surveys. We compare the host star metallicity to that of field stars using the Besançon Galaxy model, allowing for a metallicity measurement offset between the two sets. We find that hot Jupiters preferentially orbit metal-rich stars. However, we find the correlation consistent, though marginally weaker, for hot Jupiters ($\beta =0.71^{+0.56}_{-0.34}$) than it is for other longer period gas giant planets from radial velocity surveys. This suggests that the population of hot Jupiters probably formed in a similar process to other gas giant planets, and differ only in their migration histories.

scholarly journals Detection of the nearest Jupiter analogue in radial velocity and astrometry data

2019 ◽  
Vol 490 (4) ◽  
pp. 5002-5016 ◽  
Author(s):  
Fabo Feng ◽  
Guillem Anglada-Escudé ◽  
Mikko Tuomi ◽  
Hugh R A Jones ◽  
Julio Chanamé ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Giant Planets ◽  
Velocity Data ◽  
Eccentric Orbit ◽  
Brown Dwarf ◽  
Nearby Star ◽  
Long Period ◽  
The Difference ◽  
Astrometric Data ◽  
Radial Velocity Data

ABSTRACT The presence of Jupiter is crucial to the architecture of the Solar system and models underline this to be a generic feature of planetary systems. We find the detection of the difference between the position and motion recorded by the contemporary astrometric satellite Gaia and its precursor Hipparcos can be used to discover Jupiter-like planets. We illustrate how observations of the nearby star ϵ Indi A giving astrometric and radial velocity data can be used to independently find the orbit of its suspected companion. The radial velocity and astrometric data provide complementary detections which allow for a much stronger solution than either technique would provide individually. We quantify ϵ Indi A b as the closest Jupiter-like exoplanet with a mass of 3 MJup on a slightly eccentric orbit with an orbital period of 45 yr. While other long-period exoplanets have been discovered, ϵ Indi A b provides a well-constrained mass and along with the well-studied brown dwarf binary in orbit around ϵ Indi A means that the system provides a benchmark case for our understanding of the formation of gas giant planets and brown dwarfs.

scholarly journals Formation of heavy element rich giant planets by giant impacts

2007 ◽  
Vol 3 (S249) ◽  
pp. 267-270
Author(s):  
H. Genda ◽  
M. Ikoma ◽  
T. Guillot ◽  
S. Ida
Keyword(s):  
Total Mass ◽  
Heavy Element ◽  
Theoretical Models ◽  
Impact Angle ◽  
Giant Planets ◽  
Hot Jupiters ◽  
Smoothed Particle ◽  
Giant Impacts ◽  
Gas Giant ◽  
Smoothed Particle Hydrodynamic

AbstractWe have performed the smoothed particle hydrodynamic (SPH) simulations of collisions between two gas giant planets. Changes in masses of the ice/rock core and the H/He envelope due to the collisions are investigated. The main aim of this study is to constrain the origin and probability of a class of extrasolar hot Jupiters that have much larger cores and/or higher core/envelope mass ratios than those predicted by theories of accretion of gas giant planets. A typical example is HD 149026b. Theoretical models of the interior of HD 149026b (Sato et al. 2005; Fortney et al. 2006; Ikoma et al. 2006) predict that the planet contains a huge core of 50-80 Earth masses relative to the total mass of 110 Earth masses. Our SPH simulations demonstrate that such a gas giant is produced by a collision with an impact velocity of typically more than 2.5 times escape velocity and an impact angle of typically less than 10 degrees, which results in an enormous loss of the envelope gas and complete accretion of both cores.

scholarly journals TWO NEW LONG-PERIOD GIANT PLANETS FROM THE MCDONALD OBSERVATORY PLANET SEARCH AND TWO STARS WITH LONG-PERIOD RADIAL VELOCITY SIGNALS RELATED TO STELLAR ACTIVITY CYCLES

2016 ◽  
Vol 818 (1) ◽  
pp. 34 ◽  
Author(s):  
Michael Endl ◽  
Erik J. Brugamyer ◽  
William D. Cochran ◽  
Phillip J. MacQueen ◽  
Paul Robertson ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Giant Planets ◽  
Stellar Activity ◽  
Long Period ◽  
Activity Cycles

scholarly journals Cool Jupiters greatly outnumber their toasty siblings: occurrence rates from the Anglo-Australian Planet Search

2019 ◽  
Vol 492 (1) ◽  
pp. 377-383 ◽  
Author(s):  
Robert A Wittenmyer ◽  
Songhu Wang ◽  
Jonathan Horner ◽  
R P Butler ◽  
C G Tinney ◽  
...  
Keyword(s):  
Solar System ◽  
Radial Velocity ◽  
Planetary System ◽  
Planetary Systems ◽  
Giant Planets ◽  
Occurrence Rate ◽  
Hot Jupiters ◽  
The Past ◽  
Order Of Magnitude

ABSTRACT Our understanding of planetary systems different to our own has grown dramatically in the past 30 yr. However, our efforts to ascertain the degree to which the Solar system is abnormal or unique have been hindered by the observational biases inherent to the methods that have yielded the greatest exoplanet hauls. On the basis of such surveys, one might consider our planetary system highly unusual – but the reality is that we are only now beginning to uncover the true picture. In this work, we use the full 18-yr archive of data from the Anglo-Australian Planet Search to examine the abundance of ‘cool Jupiters’ – analogues to the Solar system’s giant planets, Jupiter and Saturn. We find that such planets are intrinsically far more common through the cosmos than their siblings, the hot Jupiters. We find that the occurrence rate of such ‘cool Jupiters’ is $6.73^{+2.09}_{-1.13}$ per cent, almost an order of magnitude higher than the occurrence of hot Jupiters (at $0.84^{+0.70}_{-0.20}$ per cent). We also find that the occurrence rate of giant planets is essentially constant beyond orbital distances of ∼1 au. Our results reinforce the importance of legacy radial velocity surveys for the understanding of the Solar system’s place in the cosmos.

scholarly journals NGTS-6b: an ultrashort period hot-Jupiter orbiting an old K dwarf

2019 ◽  
Vol 489 (3) ◽  
pp. 4125-4134 ◽  
Author(s):  
Jose I Vines ◽  
James S Jenkins ◽  
Jack S Acton ◽  
Joshua Briegal ◽  
Daniel Bayliss ◽  
...  
Keyword(s):  
Bulk Density ◽  
Small Population ◽  
Giant Planets ◽  
Gaseous Atmosphere ◽  
Next Generation ◽  
Evolutionary Mechanisms ◽  
Hot Jupiters ◽  
Gas Giant ◽  
Hot Jupiter

ABSTRACT We report the discovery of a new ultrashort period hot Jupiter from the Next Generation Transit Survey. NGTS-6b orbits its star with a period of 21.17 h, and has a mass and radius of $1.330^{+0.024}_{-0.028}$MJ and $1.271^{+0.197}_{-0.188}$RJ, respectively, returning a planetary bulk density of $0.711^{+0.214}_{-0.136}$ g cm−3. Conforming to the currently known small population of ultrashort period hot Jupiters, the planet appears to orbit a metal-rich star ([Fe/H] = +0.11 ± 0.09 dex). Photoevaporation models suggest the planet should have lost 5 per cent of its gaseous atmosphere over the course of the 9.6 Gyr of evolution of the system. NGTS-6b adds to the small, but growing list of ultrashort period gas giant planets, and will help us to understand the dominant formation and evolutionary mechanisms that govern this population.

scholarly journals Astrometric Constraints on the Masses of Long-period Gas Giant Planets in the TRAPPIST-1 Planetary System

2017 ◽  
Vol 154 (3) ◽  
pp. 103 ◽  
Author(s):  
Alan P. Boss ◽  
Alycia J. Weinberger ◽  
Sandra A. Keiser ◽  
Tri L. Astraatmadja ◽  
Guillem Anglada-Escude ◽  
...  
Keyword(s):  
Planetary System ◽  
Giant Planets ◽  
Long Period ◽  
Gas Giant ◽  
The Masses

scholarly journals How planet–planet scattering can create high-inclination as well as long-period orbits

2010 ◽  
Vol 6 (S276) ◽  
pp. 225-229 ◽  
Author(s):  
Sourav Chatterjee ◽  
Eric B. Ford ◽  
Frederic A. Rasio
Keyword(s):  
Major Axis ◽  
Theoretical Models ◽  
Giant Planets ◽  
Direct Imaging ◽  
Semi Major Axis ◽  
Hot Jupiters ◽  
Long Period ◽  
Outer Disk ◽  
Planetary Orbits ◽  
Core Accretion

AbstractRecent observations have revealed two new classes of planetary orbits. Rossiter-Mclaughlin (RM) measurements have revealed hot Jupiters in high-obliquity orbits. In addition, direct-imaging has discovered giant planets at large (~ 100 AU) separations via direct-imaging technique. Simple-minded disk-migration scenarios are inconsistent with the high-inclination (and even retrograde) orbits as seen in recent RM measurements. Furthermore, forming giant planets at large semi-major axis (a) may be challenging in the core-accretion paradigm. We perform many N-body simulations to explore the two above-mentioned orbital architectures. Planet–planet scattering in a multi-planet system can naturally excite orbital inclinations. Planets can also get scattered to large distances. Large-a planetary orbits created from planet–planet scattering are expected to have high eccentricities (e). Theoretical models predict that the observed long-period planets, such as Fomalhaut-b have moderate e ≈ 0.3. Interestingly, these are also in systems with disks. We find that if a massive-enough outer disk is present, a scattered planet may be circularized at large a via dynamical friction from the disk and repeated scattering of the disk particles.

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