scholarly journals The Peculiar Chemical Pattern of the WASP-160 Binary System: Signatures of Planetary Formation and Evolution?

2021 ◽  
Vol 162 (6) ◽  
pp. 291
Author(s):  
Emiliano Jofré ◽  
Romina Petrucci ◽  
Yilen Gómez Maqueo Chew ◽  
Ivan Ramírez ◽  
Carlos Saffe ◽  
...  
Keyword(s):  
Binary System ◽  
High Precision ◽  
Binary Stars ◽  
Contrast Imaging ◽  
Chemical Abundances ◽  
Transiting Planets ◽  
High Contrast Imaging ◽  
Chemical Pattern ◽  
Significant Deficit ◽  
Formation And Evolution

Abstract Wide binary stars with similar components hosting planets provide a favorable opportunity for exploring the star–planet chemical connection. We perform a detailed characterization of the solar-type stars in the WASP-160 binary system. No planet has been reported yet around WASP-160A, while WASP-160B is known to host a transiting Saturn-mass planet, WASP-160B b. For this planet, we also derive updated properties from both literature and new observations. Furthermore, using TESS photometry, we constrain the presence of transiting planets around WASP-160A and additional ones around WASP-160B. The stellar characterization includes, for the first time, the computation of high-precision differential atmospheric and chemical abundances of 25 elements based on high-quality Gemini-GRACES spectra. Our analysis reveals evidence of a correlation between the differential abundances and the condensation temperatures of the elements. In particular, we find both a small but significant deficit of volatiles and an enhancement of refractory elements in WASP-160B relative to WASP-160A. After WASP-94, this is the second stellar pair among the shortlist of planet-hosting binaries showing this kind of peculiar chemical pattern. Although we discuss several plausible planet formation and evolution scenarios for WASP-160A and B that could explain the observed chemical pattern, none of them can be conclusively accepted or rejected. Future high-precision photometric and spectroscopic follow-up, as well as high-contrast imaging observations, of WASP-160A and B might provide further constraints on the real origin of the detected chemical differences.

Enabling high-contrast imaging of binary stars with the Roman Space Telescope Coronagraph Instrument

2021 ◽  
Author(s):  
Eduardo Bendek ◽  
Ruslan Belikov ◽  
Dan Sirbu ◽  
Garreth Ruane ◽  
A. J. Eldorado Riggs ◽  
...  
Keyword(s):  
Binary Stars ◽  
High Contrast ◽  
Contrast Imaging ◽  
Space Telescope ◽  
High Contrast Imaging

How many suns are in the sky? Multiplicity surveys of exoplanet host stars

2018 ◽  
Vol 14 (S345) ◽  
pp. 316-317 ◽  
Author(s):  
M. Mugrauer ◽  
C. Ginski ◽  
N. Vogt ◽  
R. Neuhäuser ◽  
C. Adam
Keyword(s):  
Milky Way ◽  
Planet Formation ◽  
High Contrast ◽  
Contrast Imaging ◽  
Direct Imaging ◽  
High Contrast Imaging ◽  
Multiple Stars ◽  
First Results ◽  
Formation And Evolution ◽  
Host Stars

AbstractIn order to determine the true impact of stellar multiplicity on the formation and evolution of planets, we initiated direct imaging surveys to search for (sub)stellar companions of exoplanet host stars on close orbits, as their gravitational impact on the planet bearing disk at first and on formed planets afterwards is expected to be maximal. According to theory these are the most challenging environments for planet formation and evolution but might occur quite frequently in the milky way, due to the large number of multiple stars within our galaxy. On this poster we showed results, obtained so far in the course of our AO and Lucky-imaging campaigns of exoplanet host stars, conducted with NACO/ESO-VLT for southern and with AstraLux/CAHA2.2m for northern targets, respectively. In addition, we introduced our new high contrast imaging survey with SPHERE/ESO-VLT to search for close companions of southern exoplanet host stars, and presented some first results.

Low-cost high-precision PIAA optics for high contrast imaging with exo-planet coronagraphs

2010 ◽  
Author(s):  
Kunjithapatham Balasubramanian ◽  
Stuart B. Shaklan ◽  
Laurent Pueyo ◽  
Daniel W. Wilson ◽  
Olivier Guyon
Keyword(s):  
High Precision ◽  
Low Cost ◽  
High Contrast ◽  
Contrast Imaging ◽  
High Contrast Imaging

scholarly journals MID-INFRARED HIGH-CONTRAST IMAGING OF HD 114174 B: AN APPARENT AGE DISCREPANCY IN A “SIRIUS-LIKE” BINARY SYSTEM

2014 ◽  
Vol 783 (2) ◽  
pp. L25 ◽  
Author(s):  
Christopher T. Matthews ◽  
Justin R. Crepp ◽  
Andrew Skemer ◽  
Philip M. Hinz ◽  
Alexandros Gianninas ◽  
...  
Keyword(s):  
Binary System ◽  
High Contrast ◽  
Contrast Imaging ◽  
Mid Infrared ◽  
High Contrast Imaging ◽  
Apparent Age ◽  
Age Discrepancy

scholarly journals Direct Imaging of Exoplanets Living an Exciting Life

2015 ◽  
Vol 10 (S314) ◽  
pp. 213-219
Author(s):  
G. Chauvin
Keyword(s):  
Physical Properties ◽  
Imaging Techniques ◽  
Formation Mechanisms ◽  
Contrast Imaging ◽  
The Past ◽  
High Contrast Imaging ◽  
Nearby Stars ◽  
Formation And Evolution ◽  
Observing Techniques

AbstractWith the development of high contrast imaging techniques and instruments, vast efforts have been devoted during the past decades to detect and characterize lighter, cooler and closer companions to nearby stars, and ultimately image new planetary systems. Complementary to other planet-hunting techniques, this approach has opened a new astrophysical window to study the physical properties and the formation mechanisms of brown dwarfs and planets. In this review, I will briefly describe the different observing techniques and strategies used, the main samples of targeted nearby stars, finally the main results obtained so far about exoplanet discoveries characterization of their physical properties, and study of their occurrence and possible formation and evolution mechanisms.

Diamond turned high precision PIAA optics and four mirror PIAA system for high contrast imaging of exo-planets

2011 ◽  
Author(s):  
Kunjithapatham Balasubramanian ◽  
Eric Cady ◽  
Laurent Pueyo ◽  
Xin An ◽  
Stuart Shaklan ◽  
...  
Keyword(s):  
High Precision ◽  
High Contrast ◽  
Contrast Imaging ◽  
High Contrast Imaging

scholarly journals SPOTS: The Search for Planets Orbiting Two Stars

2018 ◽  
Vol 619 ◽  
pp. A43 ◽  
Author(s):  
R. Asensio-Torres ◽  
M. Janson ◽  
M. Bonavita ◽  
S. Desidera ◽  
C. Thalmann ◽  
...  
Keyword(s):  
Binary Stars ◽  
Imaging Techniques ◽  
Contrast Imaging ◽  
Direct Imaging ◽  
Upper Limit ◽  
High Contrast Imaging ◽  
Survey Results ◽  
Low Mass ◽  
Best Fit ◽  
Observational Program

Binary stars constitute a large percentage of the stellar population, yet relatively little is known about the planetary systems orbiting them. Most constraints on circumbinary planets (CBPs) so far come from transit observations with the Kepler telescope, which is sensitive to close-in exoplanets but does not constrain planets on wider orbits. However, with continuous developments in high-contrast imaging techniques, this population can now be addressed through direct imaging. We present the full survey results of the Search for Planets Orbiting Two Stars (SPOTS) survey, which is the first direct imaging survey targeting CBPs. The SPOTS observational program comprises 62 tight binaries that are young and nearby, and thus suitable for direct imaging studies, with VLT/NaCo and VLT/SPHERE. Results from SPOTS include the resolved circumbinary disk around AK Sco, the discovery of a low-mass stellar companion in a triple packed system, the relative astrometry of up to 9 resolved binaries, and possible indications of non-background planetary-mass candidates around HIP 77911. We did not find any CBP within 300 AU, which implies a frequency upper limit on CBPs (1–15 MJup) of 6–10% between 30–300 AU. Coupling these observations with an archival dataset for a total of 163 stellar pairs, we find a best-fit CBP frequency of 1.9% (2–15 MJup) between 1 and 300 AU with a 10.5% upper limit at a 95% confidence level. This result is consistent with the distribution of companions around single stars.

scholarly journals High-precision analysis of binary stars with planets

2019 ◽  
Vol 625 ◽  
pp. A39 ◽  
Author(s):  
C. Saffe ◽  
E. Jofré ◽  
P. Miquelarena ◽  
M. Jaque Arancibia ◽  
M. Flores ◽  
...  
Keyword(s):  
Binary System ◽  
High Precision ◽  
Binary Stars ◽  
Planet Formation ◽  
Giant Planet ◽  
Dynamical Evolution ◽  
Terrestrial Planet ◽  
Condensation Temperature ◽  
The Sun ◽  
First Time

Aims. We explore for the first time the probable chemical signature of planet formation in the remarkable binary system HD 106515. Star A hosts a massive long-period planet with ~9 MJup detected by radial velocity, while there is no planet detected at the B star. We also refine stellar and planetary parameters by using non-solar-scaled opacities when modelling the stars. Methods. We carried out a simultaneous determination of stellar parameters and abundances by applying for the first time non-solar-scaled opacities in this binary system, in order to reach the highest possible precision. We used a line-by-line strictly differential approach, using the Sun and then the A star as reference. Stellar parameters were determined by imposing an ionization and excitation balance of Fe lines, with an updated version of the FUNDPAR program, ATLAS12 model atmospheres, and the MOOG code. Opacities for an arbitrary composition were calculated through the opacity sampling method. The chemical patterns were compared with solar-twins condensation temperature Tc trends from the literature and also mutually between both stars. We take the opportunity to compare and discuss the results of the classical solar-scaled method and the high-precision procedure applied here. Results. Stars A and B in the binary system HD 106515 do not seem to be depleted in refractory elements, which is different when comparing the Sun with solar twins. The terrestrial planet formation would have been less efficient in the stars of this binary system. Together with HD 80606/7, this is the second binary system that does not seem to present a (terrestrial) signature of planet formation, when both systems host an eccentric giant planet. This is in agreement with numerical simulations, where the early dynamical evolution of eccentric giant planets clears out most of the possible terrestrial planets in the inner zone. We refined the stellar mass, radius, and age for both stars and found a notable difference of ~78% in R⋆ compared to previous works. We also refined the planet mass to mp sini = 9.08 ± 0.20 MJup, which differs by ~6% compared with the literature. In addition, we showed that the non-solar-scaled solution is not compatible with the classical solar-scaled method, and some abundance differences are comparable to non-local thermodynamic equilibrium (NLTE) or galactic chemical evolution (GCE) effects especially when using the Sun as reference. Therefore, we encourage the use of non-solar-scaled opacities in high-precision studies such as the detection of Tc trends.

scholarly journals Dynamical Mass of the Young Substellar Companion HD 984 B

2022 ◽  
Vol 163 (2) ◽  
pp. 50
Author(s):  
Kyle Franson ◽  
Brendan P. Bowler ◽  
Timothy D. Brandt ◽  
Trent J. Dupuy ◽  
Quang H. Tran ◽  
...  
Keyword(s):  
Giant Planet ◽  
Radial Velocities ◽  
Proper Motions ◽  
Brown Dwarf ◽  
Contrast Imaging ◽  
Mass Measurements ◽  
Dynamical Mass ◽  
High Contrast Imaging ◽  
Formation And Evolution ◽  
Model Independent

Abstract Model-independent masses of substellar companions are critical tools to validate models of planet and brown dwarf cooling, test their input physics, and determine the formation and evolution of these objects. In this work, we measure the dynamical mass and orbit of the young substellar companion HD 984 B. We obtained new high-contrast imaging of the HD 984 system with Keck/NIRC2 that expands the baseline of relative astrometry from 3 to 8 yr. We also present new radial velocities of the host star with the Habitable-Zone Planet Finder spectrograph at the Hobby-Eberly Telescope. Furthermore, HD 984 exhibits a significant proper motion difference between Hipparcos and Gaia EDR3. Our joint orbit fit of the relative astrometry, proper motions, and radial velocities yields a dynamical mass of 61 ± 4 M Jup for HD 984 B, placing the companion firmly in the brown dwarf regime. The new fit also reveals a higher eccentricity for the companion (e = 0.76 ± 0.05) compared to previous orbit fits. Given the broad age constraint for HD 984, this mass is consistent with predictions from evolutionary models. HD 984 B’s dynamical mass places it among a small but growing list of giant planet and brown dwarf companions with direct mass measurements.

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