Decoupling of a giant planet from its disk in an inclined binary system

The binary system 16 Cygni is key in studies of the planet-star chemical composition connection, as only one of the stars is known to host a planet. This allows us to better assess the possible influence of planet interactions on the chemical composition of stars that are born from the same cloud and thus should have a similar abundance pattern. In our previous work, we found clear abundance differences for elements with Z ≤ 30 between both components of this system and a trend of these abundances as a function of the condensation temperature (Tc), which suggests a spectral chemical signature related to planet formation. In this work we show that our previous findings are still consistent even if we include more species, such as the volatile N and neutron capture elements (Z > 30). We report a slope with Tc of 1.56 ± 0.24 × 10−5 dex K−1, that is good agreement with our previous work. We also performed some tests using ARES and iSpec to measure automatically the equivalent width and found Tc slopes in reasonable agreement with our results as well. In addition, we determined abundances for Li and Be by spectral synthesis, finding that 16 Cyg A is richer not only in Li but also in Be, when compared to its companion. This may be evidence of planet engulfment, indicating that the Tc trend found in this binary system may be a chemical signature of planet accretion in the A component, rather than an imprint of the giant planet rocky core formation on 16 Cyg B.

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Discovery of a stellar companion to HD 131399A

Astronomy and Astrophysics ◽

10.1051/0004-6361/201730978 ◽

2017 ◽

Vol 608 ◽

pp. L9 ◽

Cited By ~ 1

Author(s):

A.-M. Lagrange ◽

M. Keppler ◽

H. Beust ◽

L. Rodet ◽

N. Meunier ◽

...

Keyword(s):

High Resolution ◽

Binary System ◽

Planet Formation ◽

Giant Planet ◽

Dynamical Evolution ◽

Young Stars ◽

Circumstellar Disk ◽

Mass Star ◽

Low Mass

Context. The giant exoplanets imaged on wide orbits (≥10 au) around young stars challenge the classical theories of planet formation. The presence of perturbing bodies could have played a role in the dynamical evolution of the planets once formed. Aims. We aim to search for close companions to HD 131399, a star around which a giant planet has been discovered, at a projected separation of about 80 au. The star also appears to be a member of a wide (320 au) binary system. Methods. We recorded HARPS high resolution spectra in January 2017. Results. We find that HD 131399A is probably seen close to pole-on. We discover a low mass star companion that orbits with a period of about 10 days on a misaligned orbit. Even though the companion does not have an impact on the current dynamical evolution of the planet, it could have played a role in its setting and in clearing the circumstellar disk from which the planet may originate.

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HIGH PRECISION ABUNDANCES IN THE 16 Cyg BINARY SYSTEM: A SIGNATURE OF THE ROCKY CORE IN THE GIANT PLANET

The Astrophysical Journal ◽

10.1088/2041-8205/790/2/l25 ◽

2014 ◽

Vol 790 (2) ◽

pp. L25 ◽

Cited By ~ 59

Author(s):

Marcelo Tucci Maia ◽

Jorge Meléndez ◽

Iván Ramírez

Keyword(s):

Binary System ◽

High Precision ◽

Giant Planet ◽

System A

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High-precision analysis of binary stars with planets

Astronomy and Astrophysics ◽

10.1051/0004-6361/201935352 ◽

2019 ◽

Vol 625 ◽

pp. A39 ◽

Cited By ~ 1

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.

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High temperature 27Al NMR time resolved study. Application to the CaO-Al2O3 binary system

Journal de Chimie Physique ◽

10.1051/jcp/1995921871 ◽

1995 ◽

Vol 92 ◽

pp. 1871-1876 ◽

Cited By ~ 6

Author(s):

B Touzo ◽

D Trumeau ◽

D Massiot ◽

I Farnan ◽

JP Coutures

Keyword(s):

High Temperature ◽

Binary System ◽

27Al Nmr ◽

Time Resolved ◽

Study Application

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Non-standard methods for converting numbers from one number system to another

Informatics in school ◽

10.32517/2221-1993-2020-19-9-28-30 ◽

2020 ◽

Vol 1 (9) ◽

pp. 28-30

Author(s):

D. M. Zlatopolski

Keyword(s):

Binary System ◽

Maximum Degree ◽

Number System ◽

Binary Form ◽

Binary Number ◽

Standard Methods ◽

Optimal Variant ◽

Decimal System ◽

Large Numbers ◽

Independent Work

The article describes a number of little-known methods for translating natural numbers from one number system to another. The first is a method for converting large numbers from the decimal system to the binary system, based on multiple divisions of a given number and all intermediate quotients by 64 (or another number equal to 2n ), followed by writing the last quotient and the resulting remainders in binary form. Then two methods of mutual translation of decimal and binary numbers are described, based on the so-called «Horner scheme». An optimal variant of converting numbers into the binary number system by the method of division by 2 is also given. In conclusion, a fragment of a manuscript from the beginning of the late 16th — early 17th centuries is published with translation into the binary system by the method of highlighting the maximum degree of number 2. Assignments for independent work of students are offered.

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