scholarly journals Populations of Extrasolar Giant Planets from Transit and Radial Velocity Surveys

2018 ◽  
pp. 1-23
Author(s):  
Alexandre Santerne
Keyword(s):  
Radial Velocity ◽  
Giant Planets

scholarly journals Investigating the young solar system analog HD 95086

2018 ◽  
Vol 617 ◽  
pp. A76 ◽  
Author(s):  
G. Chauvin ◽  
R. Gratton ◽  
M. Bonnefoy ◽  
A.-M. Lagrange ◽  
J. de Boer ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Near Infrared ◽  
Scattered Light ◽  
Spectral Energy Distribution ◽  
Giant Planet ◽  
Giant Planets ◽  
Dual Band ◽  
Spectral Energy ◽  
Semi Major Axis ◽  
Integral Field Spectrograph

Context. HD 95086 (A8V, 17 Myr) hosts a rare planetary system for which a multi-belt debris disk and a giant planet of 4–5 MJup have been directly imaged. Aims. Our study aims to characterize the global architecture of this young system using the combination of radial velocity and direct imaging observations. We want to characterize the physical and orbital properties of HD 95086 b, search for additional planets at short and wide orbits and image the cold outer debris belt in scattered light. Methods. We used HARPS at the ESO 3.6 m telescope to monitor the radial velocity of HD 95086 over two years and investigate the existence of giant planets at less than 3 au orbital distance. With the IRDIS dual-band imager and the IFS integral field spectrograph of SPHERE at VLT, we imaged the faint circumstellar environment beyond 10 au at six epochs between 2015 and 2017. Results. We do not detect additional giant planets around HD 95086. We identify the nature (bound companion or background contaminant) of all point-like sources detected in the IRDIS field of view. None of them correspond to the ones recently discovered near the edge of the cold outer belt by ALMA. HD 95086 b is resolved for the first time in J-band with IFS. Its near-infrared spectral energy distribution is well fitted by a few dusty and/or young L7–L9 dwarf spectral templates. The extremely red 1–4 μm spectral distribution is typical of low-gravity objects at the L/T spectral type transition. The planet’s orbital motion is resolved between January 2015 and May 2017. Together with past NaCo measurements properly re-calibrated, our orbital fitting solutions favor a retrograde low to moderate-eccentricity orbit e = 0.2+0.3−0.2, with a semi-major axis ~52 au corresponding to orbital periods of ~288 yr and an inclination that peaks at i = 141°, which is compatible with a planet-disk coplanar configuration. Finally, we report the detection in polarimetric differential imaging of the cold outer debris belt between 100 and 300 au, consistent in radial extent with recent ALMA 1.3 mm resolved observations.

scholarly journals The likelihood of detecting young giant planets with high-contrast imaging and interferometry

2019 ◽  
Vol 490 (1) ◽  
pp. 502-512 ◽  
Author(s):  
A L Wallace ◽  
M J Ireland
Keyword(s):  
Radial Velocity ◽  
Near Infrared ◽  
Giant Planet ◽  
Giant Planets ◽  
Contrast Imaging ◽  
Distribution Models ◽  
High Contrast Imaging ◽  
Solar Type ◽  
Infrared Wavelengths ◽  
Core Accretion

ABSTRACT Giant planets are expected to form at orbital radii that are relatively large compared to transit and radial velocity detections (>1 au). As a result, giant planet formation is best observed through direct imaging. By simulating the formation of giant (0.3–5MJ) planets by core accretion, we predict planet magnitude in the near-infrared (2–4 μm) and demonstrate that, once a planet reaches the runaway accretion phase, it is self-luminous and is bright enough to be detected in near-infrared wavelengths. Using planet distribution models consistent with existing radial velocity and imaging constraints, we simulate a large sample of systems with the same stellar and disc properties to determine how many planets can be detected. We find that current large (8–10 m) telescopes have at most a 0.2 per cent chance of detecting a core-accretion giant planet in the L’ band and 2 per cent in the K band for a typical solar-type star. Future instruments such as METIS and VIKiNG have higher sensitivity and are expected to detect exoplanets at a maximum rate of 2 and 8 per cent, respectively.

scholarly journals The Pan-Pacific Planet Search – VIII. Complete results and the occurrence rate of planets around low-luminosity giants

2019 ◽  
Vol 491 (4) ◽  
pp. 5248-5257 ◽  
Author(s):  
Robert A Wittenmyer ◽  
R P Butler ◽  
Jonathan Horner ◽  
Jake Clark ◽  
C G Tinney ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Main Sequence ◽  
Giant Planets ◽  
Occurrence Rate ◽  
Velocity Measurements ◽  
Intermediate Mass ◽  
Giant Stars ◽  
Intermediate Mass Stars ◽  
Final Data ◽  
Solar Type

ABSTRACT Our knowledge of the populations and occurrence rates of planets orbiting evolved intermediate-mass stars lags behind that for solar-type stars by at least a decade. Some radial velocity surveys have targeted these low-luminosity giant stars, providing some insights into the properties of their planetary systems. Here, we present the final data release of the Pan-Pacific Planet Search (PPPS), a 5 yr radial velocity survey using the 3.9 m Anglo-Australian Telescope. We present 1293 precise radial velocity measurements for 129 stars, and highlight 6 potential substellar-mass companions, which require additional observations to confirm. Correcting for the substantial incompleteness in the sample, we estimate the occurrence rate of giant planets orbiting low-luminosity giant stars to be approximately 7.8$^{+9.1}_{-3.3}$ per cent. This result is consistent with the frequency of such planets found to orbit main-sequence A-type stars, from which the PPPS stars have evolved.

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 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 The Solar Neighborhood XLVIII: Nine Giant Planets Orbiting Nearby K Dwarfs, and the CHIRON Spectrograph’s Radial Velocity Performance

2021 ◽  
Vol 162 (5) ◽  
pp. 176
Author(s):  
Leonardo A. Paredes ◽  
Todd J. Henry ◽  
Samuel N. Quinn ◽  
Douglas R. Gies ◽  
Rodrigo Hinojosa-Goñi ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Solar Neighborhood ◽  
Giant Planets

scholarly journals Evidence for a high mutual inclination between the cold Jupiter and transiting super Earth orbiting π Men

2020 ◽  
Vol 497 (2) ◽  
pp. 2096-2118 ◽  
Author(s):  
Jerry W Xuan ◽  
Mark C Wyatt
Keyword(s):  
Radial Velocity ◽  
Giant Planets ◽  
Spin Axis ◽  
Spin Orientation ◽  
Outer Planets ◽  
Mutual Inclination ◽  
General Relativistic ◽  
Invariable Plane ◽  
Gaia Dr2 ◽  
Protoplanetary Discs

ABSTRACT π Men hosts a transiting super Earth (P ≈ 6.27 d, m ≈ 4.82 M⊕, R ≈ 2.04 R⊕) discovered by TESS and a cold Jupiter (P ≈ 2093 d, msin I ≈ 10.02 MJup, e ≈ 0.64) discovered from radial velocity. We use Gaia DR2 and Hipparcos astrometry to derive the star’s velocity caused by the orbiting planets and constrain the cold Jupiter’s sky-projected inclination (Ib = 41°−65°). From this, we derive the mutual inclination (ΔI) between the two planets, and find that 49° < ΔI < 131° (1σ) and 28° < ΔI < 152° (2σ). We examine the dynamics of the system using N-body simulations, and find that potentially large oscillations in the super Earth’s eccentricity and inclination are suppressed by general relativistic precession. However, nodal precession of the inner orbit around the invariable plane causes the super Earth to only transit between 7 and 22 per cent of the time, and to usually be observed as misaligned with the stellar spin axis. We repeat our analysis for HAT-P-11, finding a large ΔI between its close-in Neptune and cold Jupiter and similar dynamics. π Men and HAT-P-11 are prime examples of systems where dynamically hot outer planets excite their inner planets, with the effects of increasing planet eccentricities, planet–star misalignments, and potentially reducing the transit multiplicity. Formation of such systems likely involves scattering between multiple giant planets or misaligned protoplanetary discs. Future imaging of the faint debris disc in π Men and precise constraints on its stellar spin orientation would provide strong tests for these formation scenarios.

scholarly journals The Planet Orbiting ρ Coronae Borealis

1999 ◽  
Vol 170 ◽  
pp. 162-165 ◽  
Author(s):  
R. W. Noyes ◽  
A. R. Contos ◽  
S. G. Korzennik ◽  
P. Nisenson ◽  
T. M. Brown ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Giant Planets ◽  
Orbital Parameters ◽  
Upper Limits ◽  
And Migration ◽  
The Times

AbstractContinuing precise radial velocity observations of ρ Coronae Borealis have allowed the determination of updated parameters of the 40-day orbit of its Jupiter-mass companion. This confirms the previously reported period and amplitude, and shows a small but marginally significant non-zero eccentricity. It also provides improved predictions for the times of possible transit of the companion in front of the star. The new data provide upper limits to the mass of a possible second companion to the system. The orbital parameters are discussed in the light of scenarios for the origin and migration of extra-solar giant planets.

scholarly journals 14 Her: A Likely Case of Planet–Planet Scattering

2021 ◽  
Vol 922 (2) ◽  
pp. L43
Author(s):  
Daniella C. Bardalez Gagliuffi ◽  
Jacqueline K. Faherty ◽  
Yiting Li ◽  
Timothy D. Brandt ◽  
Lauryn Williams ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Proper Motion ◽  
Motion Vector ◽  
Giant Planets ◽  
Middle Aged ◽  
Partial Phase ◽  
Current Configuration ◽  
Orbital Parameters ◽  
Long Term Trends

Abstract In this Letter, we measure the full orbital architecture of the two-planet system around the nearby K0 dwarf 14 Herculis. 14 Her (HD 145675, HIP 79248) is a middle-aged ( 4.6 − 1.3 + 3.8 Gyr) K0 star with two eccentric giant planets identified in the literature from radial velocity (RV) variability and long-term trends. Using archival RV data from Keck/HIRES in concert with Gaia-Hipparcos acceleration in the proper motion vector for the star, we have disentangled the mass and inclination of the b planet to 9.1 − 1.1 + 1.0 M Jup and 32.7 − 3.2 + 5.3 degrees. Despite only partial phase coverage for the c planet’s orbit, we are able to constrain its mass and orbital parameters as well to 6.9 − 1.0 + 1.7 M Jup and 101 − 33 + 31 degrees. We find that coplanarity of the b and c orbits is strongly disfavored. Combined with the age of the system and the comparable masses of its planets, this suggests that planet–planet scattering may be responsible for the current configuration of the system.

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.

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