scholarly journals Evidence of Rocky Planet Engulfment in the Wide Binary System HIP 71726/HIP 71737

2021 ◽  
Vol 922 (2) ◽  
pp. 129
Author(s):  
Jhon Yana Galarza ◽  
Ricardo López-Valdivia ◽  
Jorge Meléndez ◽  
Diego Lorenzo-Oliveira
Keyword(s):  
Binary System ◽  
Binary Stars ◽  
Binary Systems ◽  
Wide Binary ◽  
Chemical Abundances ◽  
Lithium Abundance ◽  
Fundamental Parameters ◽  
Refractory Elements ◽  
Star Binary ◽  
Li Content

Abstract Binary stars are supposed to be chemically homogeneous, as they are born from the same molecular cloud. However, high-precision chemical abundances show that some binary systems display chemical differences between the components, which could be due to planet engulfment. In this work, we determine precise fundamental parameters and chemical abundances for the binary system HIP 71726/HIP 71737. Our results show that the pair is truly conatal, coeval, and comoving. We also find that the component HIP 71726 is more metal-rich than HIP 71737 in the refractory elements such as iron, with Δ[Fe/H] = 0.11 ± 0.01 dex. Moreover, HIP 71726 has a lithium abundance 1.03 dex higher than HIP 71737, which is the largest difference in Li detected in twin-star binary systems with ΔT eff ≤ 50 K. The ingestion of 9.8 − 1.6 + 2.0 M ⊕ of rocky material fully explains both the enhancement in refractory elements and the high Li content observed in HIP 71726, thereby reinforcing the planet-engulfment scenario in some binary systems.

scholarly journals Sub-Milliarcsecond Optical Astrometry and Binary Stars

1995 ◽  
Vol 166 ◽  
pp. 193-202
Author(s):  
J.T. Armstrong
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Optical Interferometry ◽  
Light Curves ◽  
Spectroscopic Binaries ◽  
Indirect Methods ◽  
Fundamental Parameters ◽  
Long Baseline

Long-baseline optical interferometry has made it possible to measure the visual orbits of binary stars with major axes as small as 5 mas and errors of ≲ 100 μas. Interferometers now nearing completion will extend these values to ≳ 500 μas and σa ∼ 10 μas. Observations of double-lined spectroscopic binaries with current interferometers have already yielded some mass estimates with precisions rivaling those from fitting the light curves of eclipsing double-lined systems. Luminosity estimates based on combined visual interferometric observations and velocity curves are often more precise than those from more indirect methods based on estimates of Teff. New interferometers now coming into operation will make it possible to measure fundamental parameters in dozens to hundreds of binary systems.

scholarly journals A noninteracting low-mass black hole–giant star binary system

Science ◽  
2019 ◽  
Vol 366 (6465) ◽  
pp. 637-640 ◽  
Author(s):  
Todd A. Thompson ◽  
Christopher S. Kochanek ◽  
Krzysztof Z. Stanek ◽  
Carles Badenes ◽  
Richard S. Post ◽  
...  
Keyword(s):  
Black Hole ◽  
Binary System ◽  
Orbital Period ◽  
Binary Systems ◽  
Photometric Variability ◽  
Giant Star ◽  
Massive Neutron Star ◽  
The Galaxy ◽  
Low Mass ◽  
Star Binary

Black hole binary systems with companion stars are typically found via their x-ray emission, generated by interaction and accretion. Noninteracting binaries are expected to be plentiful in the Galaxy but must be observed using other methods. We combine radial velocity and photometric variability data to show that the bright, rapidly rotating giant star 2MASS J05215658+4359220 is in a binary system with a massive unseen companion. The system has an orbital period of ~83 days and near-zero eccentricity. The photometric variability period of the giant is consistent with the orbital period, indicating star spots and tidal synchronization. Constraints on the giant’s mass and radius imply that the unseen companion is 3.3−0.7+2.8 solar masses, indicating that it is a noninteracting low-mass black hole or an unexpectedly massive neutron star.

scholarly journals Stellar multiplicity in the Milky Way Galaxy

2017 ◽  
Vol 13 (S334) ◽  
pp. 366-367
Author(s):  
E. Stonkutė ◽  
R. P. Church ◽  
S. Feltzing ◽  
J. A. Johnson
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Milky Way ◽  
Galactic Disc ◽  
Chemical Abundances ◽  
Milky Way Galaxy ◽  
The Galaxy ◽  
Tentative Evidence ◽  
Evolution Algorithm ◽  
Binary Evolution

AbstractWe present our models of the effect of binaries on high-resolution spectroscopic surveys. We want to determine how many binary stars will be observed, whether unresolved binaries will contaminate measurements of chemical abundances, and how we can use spectroscopic surveys to better constrain the population of binary stars in the Galaxy. Using a rapid binary-evolution algorithm that enables modelling of the most complex binary systems we generate a series of large binary populations in the Galactic disc and evaluate the results. As a first application we use our model to study the binary fraction in APOGEE giants. We find tentative evidence for a change in binary fraction with metallicity.

scholarly journals Discovery of an M-type companion to the Herbig Ae Star V1787 Ori

2020 ◽  
Vol 501 (1) ◽  
pp. 1243-1252
Author(s):  
R Arun ◽  
Blesson Mathew ◽  
Sridharan Rengaswamy ◽  
P Manoj ◽  
Mayank Narang ◽  
...  
Keyword(s):  
Binary System ◽  
Adaptive Optics ◽  
Spectral Type ◽  
Template Matching ◽  
Binary Systems ◽  
Mass Ratio ◽  
Wide Binary ◽  
Star Forming ◽  
Low Mass ◽  
Low Mass Ratio

ABSTRACT The intermediate-mass Herbig Ae star V1787 Ori is a member of the L1641 star-forming region in the Orion A molecular cloud. We report the detection of an M-type companion to V1787 Ori at a projected separation of 6.66 arcsec (corresponding to 2577 au), from the analysis of VLT/NACO adaptive optics Ks-band image. Using astrometric data from Gaia DR2, we show that V1787 Ori A and B share similar distance (d ∼ 387 pc) and proper motion, indicating that they are physically associated. We estimate the spectral type of V1787 Ori B to be M5 ± 2 from colour–spectral type calibration tables and template matching using SpeX spectral library. By fitting PARSEC models in the Pan-STARRS colour–magnitude diagram, we find that V1787 Ori B has an age of 8.1$^{+1.7}_{-1.5}$ Myr and a mass of 0.39$^{+0.02}_{-0.05}$ M⊙. We show that V1787 Ori is a pre-main-sequence wide binary system with a mass ratio of 0.23. Such a low-mass ratio system is rarely identified in Herbig Ae/Be binary systems. We conclude this work with a discussion on possible mechanisms for the formation of V1787 Ori wide binary system.

scholarly journals Discovery of a Sirius-like binary system with a very strongly magnetic white dwarf

2020 ◽  
Vol 634 ◽  
pp. L10 ◽  
Author(s):  
John D. Landstreet ◽  
Stefano Bagnulo
Keyword(s):  
Binary System ◽  
White Dwarf ◽  
White Dwarfs ◽  
Optical Spectrum ◽  
Binary Systems ◽  
Main Sequence ◽  
High Mass ◽  
Wide Binary ◽  
Linear Polarisation ◽  
The Continuum

Non-interacting binary systems containing a magnetic white dwarf and a main-sequence star are considered extremely rare, perhaps non-existent. In the course of a search of magnetic fields in high-mass white dwarfs we have discovered a Sirius-like wide binary system composed of a main-sequence G0 star and an M ∼ 1.1 M⊙ white dwarf with a huge (hundreds of MG) magnetic field. This star, WDS J03038+0608B, shows a circular polarisation amplitude of 5% in the continuum, with no evidence of variability on a 1 d timescale, little or no linear polarisation in the blue part of the spectrum, and about 2% linear polarisation in the red part of the optical spectrum. A search in the literature reveals the existence of four more binary systems that include a magnetic white dwarf and a non-degenerate companion; three such systems passed unremarked in previous studies. We estimate that up to a few percent of magnetic white dwarfs may be found to occur in wide binary pairs. However, at least four of the five known binary systems with a magnetic white dwarf are too widely separated to be expected to evolve into systems experiencing Roche-lobe overflow, and cannot be considered as progenitors of magnetic cataclysmic variable (AM Her and DQ Her) systems.

scholarly journals Evolutionary Trends in Wide Binary Systems

1982 ◽  
Vol 69 ◽  
pp. 81-103
Author(s):  
Peter van de Kamp
Keyword(s):  
Stellar Evolution ◽  
White Dwarf ◽  
Binary Stars ◽  
Binary Systems ◽  
Main Sequence ◽  
Evolutionary Trends ◽  
Wide Binary ◽  
The Past ◽  
Past Half Century ◽  
Past Half

Zdenek Kopal has kindly invited me, and I have accepted, to “instruct the theoreticians on known facts”. He also asked me to express my opinion on the relative evolutionary stages of components.I am essentially an observing astronomer, occupied with stars in our immediate neighborhood, say within 10 or at most some 25 parsec, i.e., the lower main sequence and the white dwarf degenerate branch.I hope that I may perhaps contribute by surveying and reporting some relevant data. I shall touch on a number of topics, limited because of selection and lack of knowledge. My contributions to binary stars lie in the realm of parallaxes, mass-ratios and masses, – and for the past half century, perturbations, interpreted as unseen companions, stellar and otherwise. I shall briefly report on some results, and I shall be wondering and hoping that some trace of stellar evolution may possibly be present in these results. After having witnessed for more than half a century my own astronomical evolution, the time has come for me to become more aware of theoretical, evolutionary and cosmological aspects of the cosmic material, I have been playing with so long.

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.

scholarly journals A Search for RR Lyraes in Wide Binary Systems

1989 ◽  
Vol 111 ◽  
pp. 283-283
Author(s):  
Charles F. Prosser
Keyword(s):  
System Identification ◽  
Binary System ◽  
Proper Motion ◽  
Binary Systems ◽  
Plate Material ◽  
Velocity Measurements ◽  
Wide Binary ◽  
Rr Lyrae ◽  
The Galaxy

AbstractRR Lyraes that have nearby visual companions may be examined to decide if they do indeed belong to a real binary system. Identification of RR Lyraes in binary systems could lead to the determination of physical characteristics of the variable and to an understanding of the history and evolution of such systems in the Galaxy. Where possible, proper motion analysis, using astrograph plates from the Lick Proper Motion Program, for some visual binaries has been done and has enabled the rejection of some variables from consideration. The variables which have been shown not to be physically associated with their visual companions are YZ Cap, V445 Oph, BH Peg, and TX Vir. EZ Lyr, RW Ari, and V494 Sco still remain possible cases requiring relative radial velocities between the variable and companion. Limited plate material has meant that one must resort to radial velocity measurements for the RR Lyrae and close companion in order to determine the nature of the pair.

Mass Ratios in Wide Binary Stars

1997 ◽  
Vol 485 (2) ◽  
pp. 785-788 ◽  
Author(s):  
Mauri J. Valtonen
Keyword(s):  
Binary Stars ◽  
Wide Binary ◽  
Mass Ratios

scholarly journals X-ray and UV emission of the ultrashort-period, low-mass eclipsing binary system BX Trianguli

2018 ◽  
Vol 619 ◽  
pp. A138
Author(s):  
V. Perdelwitz ◽  
S. Czesla ◽  
J. Robrade ◽  
T. Pribulla ◽  
J. H. M. M. Schmitt
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Binary Systems ◽  
Uv Light ◽  
Close Binary ◽  
Eclipsing Binary ◽  
X Ray ◽  
Uv Emission ◽  
Low Mass ◽  
Orbital Modulation

Context.Close binary systems provide an excellent tool for determining stellar parameters such as radii and masses with a high degree of precision. Due to the high rotational velocities, most of these systems exhibit strong signs of magnetic activity, postulated to be the underlying reason for radius inflation in many of the components. Aims.We extend the sample of low-mass binary systems with well-known X-ray properties. Methods.We analyze data from a singular XMM-Newton pointing of the close, low-mass eclipsing binary system BX Tri. The UV light curve was modeled with the eclipsing binary modeling tool PHOEBE and data acquired with the EPIC cameras was analyzed to search for hints of orbital modulation. Results.We find clear evidence of orbital modulation in the UV light curve and show that PHOEBE is fully capable of modeling data within this wavelength range. Comparison to a theoretical flux prediction based on PHOENIX models shows that the majority of UV emission is of photospheric origin. While the X-ray light curve does exhibit strong variations, the signal-to-noise ratio of the observation is insufficient for a clear detection of signs of orbital modulation. There is evidence of a Neupert-like correlation between UV and X-ray data.

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