Journal articles on the topic 'Binary stellar evolution'
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Batten, A. H. "Stellar evolution in binary systems." Reports on Progress in Physics 58, no. 8 (August 1, 1995): 885–928. http://dx.doi.org/10.1088/0034-4885/58/8/002.
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Chen, Xuefei, and Zhanwen Han. "Primordial binary evolution and blue stragglers." Proceedings of the International Astronomical Union 5, S266 (August 2009): 333–38. http://dx.doi.org/10.1017/s1743921309991220.
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AbstractBlue stragglers have been found in all populations. They are important in both stellar evolution and stellar population synthesis. Much evidence shows that blue stragglers are relevant to primordial binaries. Here, we summarize the links between binary evolution and blue stragglers, describe the characteristics of blue stragglers originating from different binary evolutionary channels and show their consequences for binary population synthesis, such as for the integrated spectral-energy distribution, the colour–magnitude diagram, their specific frequency, and their influence on colours, etc.
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Siess, L., R. G. Izzard, P. J. Davis, and R. Deschamps. "BINSTAR: a new binary stellar evolution code." Astronomy & Astrophysics 550 (February 2013): A100. http://dx.doi.org/10.1051/0004-6361/201220327.
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McMillan, Stephen L. W. "Star Cluster Simulations Including Stellar Evolution." Symposium - International Astronomical Union 208 (2003): 131–44. http://dx.doi.org/10.1017/s0074180900207092.
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The past few years have seen dramatic improvements in the scope and realism of star cluster simulations. Accurate treatments of stellar evolution, coupled with robust descriptions of all phases of binary evolution, have been incorporated self-consistently into several dynamical codes, allowing for the first time detailed study of the interplay between stellar dynamics and stellar physics. The coupling between evolution, dynamics, and the observational appearance of the cluster is particularly strong in young systems and those containing large numbers of primordial binary systems, and important inroads have been made in these areas, particularly in N-body simulations. I discuss some technical aspects of the current generation of N-body integrators, and describe some recent results obtained using these codes.
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Hatfull, Roger W. M., Natalia Ivanova, and James C. Lombardi. "Simulating a stellar contact binary merger – I. Stellar models." Monthly Notices of the Royal Astronomical Society 507, no. 1 (July 26, 2021): 385–97. http://dx.doi.org/10.1093/mnras/stab2140.
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ABSTRACT We study the initial conditions of a common envelope (CE) event resulting in a stellar merger. A merger’s dynamics could be understood through its light curve, but no synthetic light curve has yet been created for the full evolution. Using the smoothed particle hydrodynamics (SPH) code StarSmasher, we have created three-dimensional (3D) models of a 1.52 M⊙ star that is a plausible donor in the V1309 Sco progenitor. The integrated total energy profiles of our 3D models match their initial one-dimensional (1D) models to within a 0.1 per cent difference in the top 0.1 M⊙ of their envelopes. We have introduced a new method for obtaining radiative flux by linking intrinsically optically thick SPH particles to a single stellar envelope solution from a set of unique solutions. For the first time, we calculated our 3D models’ effective temperatures to within a few per cent of the initial 1D models, and found a corresponding improvement in luminosity by a factor of ≳106 compared to ray tracing. We let our highest resolution 3D model undergo Roche lobe overflow with a 0.16 M⊙ point-mass accretor (P ≃ 1.6 d) and found a bolometric magnitude variability amplitude of ∼0.3 – comparable to that of the V1309 Sco progenitor. Our 3D models are, in the top 0.1 M⊙ of the envelope and in terms of total energy, the most accurate models so far of the V1309 Sco donor star. A dynamical simulation that uses the initial conditions we presented in this paper can be used to create the first ever synthetic CE evolution light curve.
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Czesla, S., S. Terzenbach, R. Wichmann, and J. H. M. M. Schmitt. "Spot evolution in the eclipsing binary CoRoT 105895502." Astronomy & Astrophysics 623 (March 2019): A107. http://dx.doi.org/10.1051/0004-6361/201834516.
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Stellar activity is ubiquitous in late-type stars. The special geometry of eclipsing binary systems is particularly advantageous to study the stellar surfaces and activity. We present a detailed study of the 145 d CoRoT light curve of the short-period (2.17 d) eclipsing binary CoRoT 105895502. By means of light-curve modeling with Nightfall, we determine the orbital period, effective temperature, Roche-lobe filling factors, mass ratio, and orbital inclination of CoRoT 105895502 and analyze the temporal behavior of starspots in the system. Our analysis shows one comparably short-lived (≈40 d) starspot, remaining quasi-stationary in the binary frame, and one starspot showing prograde motion at a rate of 2.3° day−1, whose lifetime exceeds the duration of the observation. In the CoRoT band, starspots account for as much as 0.6% of the quadrature flux of CoRoT 105895502, however we cannot attribute the spots to individual binary components with certainty. Our findings can be explained by differential rotation, asynchronous stellar rotation, or systematic spot evolution.
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Eggleton, Peter P. "Combining Stellar Evolution and Stellar Dynamics." Symposium - International Astronomical Union 174 (1996): 213–22. http://dx.doi.org/10.1017/s0074180900001558.
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There seem to me to be four approaches to the problem of computing the evolution of star clusters. Firstly, one might assume that our knowledge of the evolution of stars can be condensed into a subroutine that can be added to an N-body code. This subroutine would mainly have to give the radius and the time-dependent mass of a star as a function of its initial mass and its age. Secondly, standing this on its head, one might assume that our knowledge of N-body evolution can be condensed into a subroutine that can be added to a stellar evolution code. This subroutine would determine, probably in a Monte-Carlo fashion, whether the star had picked up, or lost, a binary companion, or whether the orbit of its companion was significantly changed; the probabilities would be determined by simple analytic approximations to the time-dependent distribution functions of stars (and binaries) of different masses and ages, and by interaction cross-sections as functions of density and ‘temperature’. Thirdly, if the computing power is available, one might more simply unite an N-body code with a Stellar Evolution (SE) code, and follow both the dynamics and the internal evolution simultaneously. Fourthly, we might hope at some stage to put together simple analytic approximations both from N-body and from SE studies, to develop a unified simple model. I venture to say that it is only the last stage, if it is attainable, that would entitle us to say that we ‘understand’ the evolution of stellar clusters. ‘Understanding’, I think, means that we can extract some essential wisdom from large numerical simulations, and apply it on the back of the proverbial envelope.
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Petrovic, Jelena. "The evolution of massive binary systems." Serbian Astronomical Journal, no. 201 (2020): 1–13. http://dx.doi.org/10.2298/saj2001001p.
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The evolution of massive stars in close binary systems is significantly different from single star evolution due to a series of interactions between the two stellar components. Such massive close binary systems are linked to various astrophysical phenomena, for example Wolf-Rayet stars, supernova type Ib and Ic, X-ray binaries and gamma-ray bursts. Also, the emission of gravitational waves, recently observed by the LIGO-Virgo detectors, is associated with mergers in binary systems containing compact objects, relics of massive stars - black holes and neutron stars. Evolutionary calculations of massive close binary systems were performed by various authors, but many aspects are not yet fully understood. In this paper, the main concepts of massive close binary evolution are reviewed, together with the most important parameters that can influence the final outcome of the binary system evolution, such as rotation, magnetic fields, stellar wind mass loss and mass accretion efficiency during interactions. An extensive literature overview of massive close binary models in the light of exciting observations connected with those systems is presented.
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Stairs, I. H. "Pulsars in Binary Systems: Probing Binary Stellar Evolution and General Relativity." Science 304, no. 5670 (April 23, 2004): 547–52. http://dx.doi.org/10.1126/science.1096986.
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Eldridge, J. J. "The things binaries do …" Astronomy & Geophysics 61, no. 2 (April 1, 2020): 2.24–2.29. http://dx.doi.org/10.1093/astrogeo/ataa029.
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Abstract Binary interactions change stellar evolutionary pathways and models of stellar populations – but they are largely ignored. Here J J Eldridge outlines some recent history around the development of stellar evolution and population models, and highlights the significant differences that arise when binary interactions are included.
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Glanz, Hila, and Hagai B. Perets. "Simulations of common envelope evolution in triple systems: circumstellar case." Monthly Notices of the Royal Astronomical Society 500, no. 2 (October 21, 2020): 1921–32. http://dx.doi.org/10.1093/mnras/staa3242.
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ABSTRACT The dynamical evolution of triple stellar systems could induce the formation of compact binaries and binary mergers. Common envelope (CE) evolution, which plays a major role in the evolution of compact binary systems, can similarly play a key role in the evolution of triples. Here, we use hydrodynamical simulations coupled with few-body dynamics to provide the first detailed models of the triple common envelope (TCE) evolution. We focus on the circumstellar case, where the envelope of an evolved giant engulfs a compact binary orbiting the giant, which then in-spirals into the core of the evolved star. Through our exploratory modelling, we find several possible outcomes of such TCE: the merger of the binary inside the third star’s envelope; the disruption of the in-spiralling binary following its plunge, leading to a chaotic triple dynamics of the stellar core and the two components of the former disrupted binary. The chaotic evolution typically leads to the in-spiral and merger of at least one of the former binary components with the core, and sometimes to the ejection of the second, or alternatively its further now-binary CE evolution. The in-spiral in TCE leads to overall slower in-spiral, larger mass ejection, and the production of more aspherical remnant, compared with a corresponding binary case of similar masses, due to the energy/momentum extraction from the inner-binary. We expect TCE to play a key role in producing various types of stellar-mergers and unique compact binary systems, and potentially induce transient electromagnetic and gravitational wave sources.
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Iwamoto, Nobuyuki, and Hideyuki Saio. "A Comparison of Stellar Evolution with Binary Systems." Astrophysical Journal 521, no. 1 (August 10, 1999): 297–301. http://dx.doi.org/10.1086/307518.
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Ishak, B. "The impact of binary stars on stellar evolution." Contemporary Physics 60, no. 2 (April 3, 2019): 196. http://dx.doi.org/10.1080/00107514.2019.1641158.
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Soker, Noam. "CLOSE STELLAR BINARY SYSTEMS BY GRAZING ENVELOPE EVOLUTION." Astrophysical Journal 800, no. 2 (February 18, 2015): 114. http://dx.doi.org/10.1088/0004-637x/800/2/114.
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Hurley, Jarrod R. "Models of M 67." Proceedings of the International Astronomical Union 2, no. 14 (August 2006): 442–43. http://dx.doi.org/10.1017/s1743921307011283.
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AbstractThe old open cluster M 67 is an ideal test case for current star cluster evolution models because of its dynamically evolved structure and rich stellar populations that show clear signs of interaction between stellar, binary and cluster evolution. Here we discuss a direct N-body model of M 67. This model of 12,000 single stars and 12,000 binaries is evolved from zero-age and takes full account of cluster dynamics as well as stellar and binary evolution. At an age of 4 Gyr the model cluster matches the mass and structure of M 67 as constrained by observations. We discuss the role of the primordial binary population and the cluster environment in shaping the nature of the stellar populations of M 67, with a focus on X-ray binaries and blue stragglers.
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Higl, J., L. Siess, A. Weiss, and H. Ritter. "An analysis of the TZ Fornacis binary system." Astronomy & Astrophysics 617 (September 2018): A36. http://dx.doi.org/10.1051/0004-6361/201833112.
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Context. TZ Fornacis (TZ For) is an evolved detached binary system that is difficult to model and interpret, but very useful for testing stellar evolution theory and physics. Aims. We aim to search for solutions that are self-consistent and to determine the necessary stellar physics input. We also check solutions found previously for their internal consistency and for reproducibility. Methods. We use both a single and a binary stellar evolution code, and take into account all known system properties. We determine the physical stellar parameters by imposing that the models match the known radii for identical stellar ages. The evolution has to be consistent with a binary system in classical Roche geometry. Results. We obtained two different solutions to model TZ For successfully. Both depend on avoiding a long evolution on the first giant branch and imply a sufficiently large convective core on the main sequence. TZ For can be modelled consistently as a detached binary system by invoking either a substantial amount of core overshooting or a tidally enhanced wind mass loss along the red giant branch. An evolution with Roche-lobe overflow can definitely be excluded. Conclusions. A comparison of our results with previous studies also reveals that in addition to uncertainties associated with the input physics, the modelling of overshooting by different algorithms can have a strong impact.
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Toonen, S., S. Portegies Zwart, A. S. Hamers, and D. Bandopadhyay. "The evolution of stellar triples." Astronomy & Astrophysics 640 (July 31, 2020): A16. http://dx.doi.org/10.1051/0004-6361/201936835.
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Context. Many stars do not live alone, but instead have one or more stellar companions. Observations show that these binaries, triples, and higher-order multiples are common. While the evolution of single stars and binaries have been studied extensively, the same is not true for the evolution of stellar triples. Aims. To fill in this gap in our general understanding of stellar lives, we aim to systematically explore the long-term evolution of triples and to map out the most common evolutionary pathways that triples go through. We quantitatively study how triples evolve, which processes are the most relevant, and how this differs from binary evoluion. Methods. We simulated the evolution of several large populations of triples with a population synthesis approach. We made use of the triple evolution code TRES to simulate the evolution of each triple in a consistent way, including three-body dynamics (based on the secular approach), stellar evolution, and their mutual influences. We simulated the evolution of the system up until mass transfer starts, the system becomes dynamically unstable, or a Hubble time has passed. Results. We find that stellar interactions are common in triples. Compared to a binary population, we find that the fraction of systems that can undergo mass transfer is ∼2−3 times larger in triples. Moreover, while orbits typically reach circularisation before Roche-lobe overflow in binaries, this is no longer true in triples. In our simulations, about 40% of systems retain an eccentric orbit. Additionally, we discuss various channels of triple evolution in detail, such as those where the secondary or the tertiary is the first star to initiate a mass transfer event.
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Belczynski, K., A. Romagnolo, A. Olejak, J. Klencki, D. Chattopadhyay, S. Stevenson, M. Coleman Miller, J. P. Lasota, and Paul A. Crowther. "The Uncertain Future of Massive Binaries Obscures the Origin of LIGO/Virgo Sources." Astrophysical Journal 925, no. 1 (January 1, 2022): 69. http://dx.doi.org/10.3847/1538-4357/ac375a.
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Abstract The LIGO/Virgo gravitational-wave observatories have detected at least 50 double black hole (BH) coalescences. This sample is large enough to have allowed several recent studies to draw conclusions about the implied branching ratios between isolated binaries versus dense stellar clusters as the origin of double BHs. It has also led to the exciting suggestion that the population is highly likely to contain primordial BHs. Here we demonstrate that such conclusions cannot yet be robust because of the large current uncertainties in several key aspects of binary stellar evolution. These include the development and survival of a common envelope, the mass and angular-momentum loss during binary interactions, mixing in stellar interiors, pair-instability mass loss, and supernova outbursts. Using standard tools such as the rapid population synthesis codes StarTrack and COMPAS and the detailed stellar evolution code MESA, we examine as a case study the possible future evolution of Melnick 34, the most massive known binary star system (with initial component masses of 144 M ⊙ and 131 M ⊙). We show that, despite its fairly well-known orbital architecture, various assumptions regarding stellar and binary physics predict a wide variety of outcomes: from a close BH–BH binary (which would lead to a potentially detectable coalescence), through a wide BH–BH binary (which might be seen in microlensing observations), or a Thorne–Żytkow object, to a complete disruption of both objects by a pair-instability supernova. Thus, because the future of massive binaries is inherently uncertain, sound predictions about the properties of BH–BH systems formed in the isolated binary evolution scenario are highly challenging at this time. Consequently, it is premature to draw conclusions about the formation channel branching ratios that involve isolated binary evolution for the LIGO/Virgo BH–BH merger population.
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Tkachenko, A., K. Pavlovski, C. Johnston, M. G. Pedersen, M. Michielsen, D. M. Bowman, J. Southworth, V. Tsymbal, and C. Aerts. "The mass discrepancy in intermediate- and high-mass eclipsing binaries: The need for higher convective core masses." Astronomy & Astrophysics 637 (May 2020): A60. http://dx.doi.org/10.1051/0004-6361/202037452.
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Context. Eclipsing, spectroscopic double-lined binary star systems are excellent laboratories for calibrating theories of stellar interior structure and evolution. Their precise and accurate masses and radii measured from binary dynamics offer model-independent constraints and challenge current theories of stellar evolution. Aims. We aim to investigate the mass discrepancy in binary stars. This is the significant difference between stellar components’ masses measured from binary dynamics and those inferred from models of stellar evolution via positions of the components in the Teff − log g Kiel diagram. We study the effect of near-core mixing on the mass of the convective core of the stars and interpret the results in the context of the mass discrepancy. Methods. We fitted stellar isochrones computed from a grid of MESA stellar evolution models to a homogeneous sample of eleven high-mass binary systems. Two scenarios are considered where individual stellar components of a binary system are treated independent of each other and where they are forced to have the same age and initial chemical composition. We also study the effect of the microturbulent velocity and turbulent pressure on the atmosphere model structure and stellar spectral lines, and its link with the mass discrepancy. Results. We find that the mass discrepancy is present in our sample and that it is anti-correlated with the surface gravity of the star. No correlations are found with other fundamental and atmospheric parameters, including the stellar mass. The mass discrepancy can be partially accounted for by increasing the amount of near-core mixing in stellar evolution models. We also find that ignoring the microturbulent velocity and turbulent pressure in stellar atmosphere models of hot evolved stars results in the overestimation of their effective temperature by up to 8%. Together with enhanced near-core mixing, this can almost entirely account for the ∼30% mass discrepancy found for the evolved primary component of V380 Cyg. Conclusions. We find a strong link between the mass discrepancy and the convective core mass. The mass discrepancy can be solved by considering the combined effect of extra near-core boundary mixing and the consistent treatment in the spectrum analysis of hot evolved stars. Our binary modelling results in convective core masses between 17 and 35% of the stellar mass, which is in excellent agreement with the results from gravity-mode asteroseismology of single stars. This implies larger helium core masses near the end of the main sequence than have been anticipated so far.
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Hurley, Jarrod R. "Cluster CMDs from N-body Simulations: Stellar and Binary Evolution on GRAPE." Symposium - International Astronomical Union 208 (2003): 113–22. http://dx.doi.org/10.1017/s0074180900207079.
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The Colour-Magnitude diagram (CMD) is an important observational tool for use in the study of star clusters. Thus it is important to include a consistent treatment of stellar and binary evolution in N-body codes to allow the generation and interaction of the full range of stellar populations. In this way realistic cluster models can be compared with observed cluster populations via the respective CMDs. Preliminary results of such an approach using the Aarseth NBODY4 code on the GRAPE-6 are presented here. In particular, by using a stellar evolution algorithm that includes metallicity as a free parameter, the stellar populations of clusters at various stages of evolution can be studied. Interesting formation cases directly influenced by the cluster environment are highlighted for various stellar sub-populations.
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Griffin, R. E. M., and Slavek Rucinski. "Binarity and Stellar Evolution." Proceedings of the International Astronomical Union 7, S285 (September 2011): 239–42. http://dx.doi.org/10.1017/s174392131200066x.
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AbstractModels of stellar evolution constitute an extremely powerful, and for the most part apparently very successful, tool for understanding the progression of a star through its lifetime as a fairly compact entity of incandescent gas. That success has led to stellar evolution theory becoming a crutch when an observer is faced with objects whose provenance or current state are in some way puzzling, but how safe a crutch? The validity of the theory is best checked by examining binary systems whose component parameters have been determined with high precision, but it can be (and needs to be) honed through the many challenges which non-conformist single stars and triple systems also present. Unfortunately the lever of observational parameters to constrain or challenge stellar evolution theory is not as powerful as it could be, because not all determinations of stellar parameters for the same systems agree to within the precisions claimed by their respective authors. What are the sources of bias—the data, the instrument or the techniques? The workshop was invited to discuss particularly challenging cases, and to attempt to identify how and where progress might be pursued.
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Patience, Jenny, and Gaspard Duchêne. "The Properties of Open Cluster Binaries Based on High-Resolution Imaging Surveys." Symposium - International Astronomical Union 200 (2001): 181–90. http://dx.doi.org/10.1017/s0074180900225205.
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With known properties such as age, distance and stellar density, young clusters provide ideal samples for binary star studies. We summarize recent results from high-resolution multiplicity surveys of IC 348, α Per, the Pleiades, the Hyades, and Praesepe. The statistics of the resolved companions are used to address binary star formation and evolution in clusters. Over the ranges of ages, densities and stellar masses covered by the clusters, it is found that the binary fraction is correlated with stellar density rather than age, and that both the binary fraction and binary mass ratio distribution depend upon mass. The impact of companions on X-ray emission and stellar rotation is also discussed.
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Stonkutė, E., R. P. Church, S. Feltzing, and J. A. Johnson. "Stellar multiplicity in the Milky Way Galaxy." Proceedings of the International Astronomical Union 13, S334 (July 2017): 366–67. http://dx.doi.org/10.1017/s1743921317007918.
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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.
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Bruzual, Gustavo, Gladis C. Magris, and Fabiola Hernández-Pérez. "Modeling low mass stellar populations." Proceedings of the International Astronomical Union 14, S344 (August 2018): 211–12. http://dx.doi.org/10.1017/s174392131800621x.
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AbstractModeling low mass stellar populations, like clusters and dwarf galaxies, with population synthesis models requires that we evaluate the role played by stochastic fluctuations in the sampling of the IMF on the spectro-photometric properties of these sparse populations. Interacting binaries may also modify the integrated spectra of these systems depending on the final product of the binary interaction and on the frequency of binary stars. In this work we compare the relative importance of stochastic fluctuations and binary evolution on low mass galaxy properties as a function of the population age and total mass. In most cases the effects of stochastic fluctuations dominate those produced by binary interactions. We explore and quantify the relative importance of these effects through cosmic times.
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Becker, S. A. "Cepheid Evolution." International Astronomical Union Colloquium 82 (1985): 104–25. http://dx.doi.org/10.1017/s0252921100109236.
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AbstractA review of the phases of stellar evolution relevant to Cepheid variables of both Types I and II is presented. Type I Cepheids arise as a result of normal post-main sequence evolutionary behavior of many stars in the intermediate to massive range of stellar masses. In contrast, Type II Cepheids generally originate from low-mass stars of low metalicity which are undergoing post core helium-burning evolution. Despite great progress in the past two decades, uncertainties still remain in such areas as how to best model convective overshoot, semiconvection, stellar atmospheres, rotation, and binary evolution as well as uncertainties in important physical parameters such as the nuclear reaction rates, opacity, and mass loss rates. The potential effect of these uncertainties on stellar evolution models is discussed. Finally, comparisons between theoretical predictions and observations of Cepheid variables are presented for a number of cases. The results of these comparisons show both areas of agreement and disagreement with the latter result providing incentive for further research.
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SIMÕES, F., and J. D. DO NASCIMENTO. "WHAT ROLE DOES CONVECTION PLAY IN THE SYNCHRONIZATION AND CIRCULARIZATION OF BINARIES WITH EVOLVED COMPONENTS?" International Journal of Modern Physics: Conference Series 18 (January 2012): 174–77. http://dx.doi.org/10.1142/s2010194512008409.
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Binary stars are important for understanding stellar structure and evolution. Binary systems with an evolved component give us an important constraint about the role played by convection on the characteristic time for tidal synchronization and circularization. On this study, we discuss about the role of convection in binary stars with evolved components. Base on a stellar sample composed by 260 binary stars with surface convective mass determined from evolutionary models computed with the Toulouse-Geneva Evolution Code (TGEC) as in do Nascimento et al. (2009). The stars with different convective deepening are represented in the Hertzsprung-Russell diagram (HR diagram). We are focused on the important question of how convection influence the evolution of the tidal synchronization and circularization of binary systems with an evolved component.
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Makino, Junichiro. "Black Hole Binary Mergers." Highlights of Astronomy 13 (2005): 339–42. http://dx.doi.org/10.1017/s1539299600015914.
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AbstractI overview the current understanding of the evolution of massive black hole (MBH) binaries in the center of the host stellar system. One of the main questions is whether the stellar dynamical effect can make the MBH binary hard enough that they can merge through gravitational wave radiation. So far, theories and numerical simulations suggested otherwise, since the hardening time scale becomes very long once ”loss cone” is depleted. I’ll present the result of recent simulations on this hardening time scale, and discuss its implication on the formation history of massive black holes.
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Chatterjee, Sourav, John M. Fregeau, Stefan Umbreit, and Frederic A. Rasio. "MONTE CARLO SIMULATIONS OF GLOBULAR CLUSTER EVOLUTION. V. BINARY STELLAR EVOLUTION." Astrophysical Journal 719, no. 1 (July 23, 2010): 915–30. http://dx.doi.org/10.1088/0004-637x/719/1/915.
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Jones, David. "Binary Central Stars of Planetary Nebulae." Galaxies 8, no. 2 (April 1, 2020): 28. http://dx.doi.org/10.3390/galaxies8020028.
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It is now clear that a vast majority of intermediate-mass stars have stellar and/or sub-stellar companions, therefore it is no longer appropriate to consider planetary nebulae as a single-star phenomenon, although some single, isolated stars may well lead to planetary nebulae. As such, while understanding binary evolution is critical for furthering our knowledge of planetary nebulae, the converse is also true: planetary nebulae can be valuable tools with which to probe binary evolution. In this brief review, I attempt to summarise some of our current understanding with regards to the role of binarity in the formation of planetary nebulae, and the areas in which continued study of planetary nebulae may have wider ramifications for our grasp on the fundaments of binary evolution.
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Hut, Piet. "Binary Formation and Interactions with Field Stars." Symposium - International Astronomical Union 113 (1985): 231–49. http://dx.doi.org/10.1017/s0074180900147412.
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Binaries provide an energy source in dense stellar systems. Exothermic gravitational interactions in star clusters can play a role similar to that of nuclear reactions in single stars. These gravitational interactions can be modeled in a laboratory setting, in the form of numerical binary-single star and binary-binary scattering experiments. Gravitational cross sections obtained this way can be applied to model star cluster evolution, just as nuclear cross sections are used as input data in stellar evolution calculations. References are given to detailed descriptions of gravitational cross sections, and a useful new example of an application is given: the rate at which hard binaries form in a homogeneous stellar background, as the solution of an integral equation describing the combined effects of creation, destruction, hardening and softening of binaries.
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Izzard, Robert, and Adam Jermyn. "Post-AGB Discs from Common-Envelope Evolution." Galaxies 6, no. 3 (September 11, 2018): 97. http://dx.doi.org/10.3390/galaxies6030097.
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Post-asymptotic giant branch (post-AGB) stars with discs are all binaries. Many of these binaries have orbital periods between 100 and 1000 days so cannot have avoided mass transfer between the AGB star and its companion, likely through a common-envelope type interaction. We report on preliminary results of our project to model circumbinary discs around post-AGB stars using our binary population synthesis code binary_c. We combine a simple analytic thin-disc model with binary stellar evolution to estimate the impact of the disc on the binary, and vice versa, fast enough that we can model stellar population and hence explore the rather uncertain parameter space involved with disc formation. We find that, provided the discs form with sufficient mass and angular momentum, and have an inner edge that is relatively close to the binary, they can both prolong the life of their parent post-AGB star and pump the eccentricity of orbits of their inner binaries.
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Tout, Christopher A., Amanda I. Karakas, John C. Lattanzio, Jarrod R. Hurley, and Onno R. Pols. "How Binary Stars affect Galactic Chemical Evolution." Symposium - International Astronomical Union 191 (1999): 447–52. http://dx.doi.org/10.1017/s0074180900203392.
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At least 60% of stars appear to be binary and about half of these are close enough to interact. Because of the enormous expansion on the AGB, many of these interactions will involve an AGB star and a relatively compact companion, anything from a low-mass main-sequence star to a degenerate remnant. Mass loss plays the dominant role in determining the lifetime and the extent of nuclear processing of the AGB phase. Binary interaction will increase the mass loss from the AGB star and curtail its evolution, either through Roche-lobe overflow, common-envelope evolution or the driving of an enhanced stellar wind. These processes will tend to reduce the metals, particularly carbon, returned to the inter-stellar medium. On the other hand merged systems or companions that accrete a substantial amount of mass themselves evolve into AGB stars that can synthesize and return more carbon than the two individuals would have alone. By synthesizing large populations of stars, with nucleosynthesis and binary interaction, we estimate a reduction in carbon yield owing to binary star evolution of as much as 15%.
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García, Federico, Adolfo Simaz Bunzel, Sylvain Chaty, Edward Porter, and Eric Chassande-Mottin. "Progenitors of low-mass binary black-hole mergers in the isolated binary evolution scenario." Astronomy & Astrophysics 649 (May 2021): A114. http://dx.doi.org/10.1051/0004-6361/202038357.
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Context. The formation history, progenitor properties, and expected rates of the binary black holes discovered by the LIGO-Virgo collaboration via the gravitational-wave emission during their coalescence are a topic of active research. Aims. We aim to study the progenitor properties and expected rates of the two lowest-mass binary black hole mergers, GW151226 and GW170608, detected within the first two Advanced LIGO-Virgo observing runs, in the context of the classical isolated binary-evolution scenario. Methods. We used the publicly available 1D-hydrodynamic stellar-evolution code MESA, which we adapted to include the black-hole formation and the unstable mass transfer developed during the so-called common-envelope phase. Using more than 60 000 binary simulations, we explored a wide parameter space for initial stellar masses, separations, metallicities, and mass-transfer efficiencies. We obtained the expected distributions for the chirp mass, mass ratio, and merger time delay by accounting for the initial stellar binary distributions. We predicted the expected merger rates and compared them with those of the detected gravitational-wave events. We studied the dependence of our predictions with respect to the (as yet) unconstrained parameters inherent to binary stellar evolution. Results. Our simulations for both events show that while the progenitors we obtained are compatible over the entire range of explored metallicities, they show a strong dependence on the initial masses of the stars, according to stellar winds. All the progenitors we found follow a similar evolutionary path, starting from binaries with initial separations in the 30−200 R⊙ range experiencing a stable mass transfer interaction before the formation of the first black hole, followed by a second unstable mass-transfer episode leading to a common-envelope ejection that occurs either when the secondary star crosses the Hertzsprung gap or when it is burning He in its core. The common-envelope phase plays a fundamental role in the considered low-mass range: only progenitors experiencing such an unstable mass-transfer phase are able to merge in less than a Hubble time. Conclusions. We find integrated merger-rate densities in the range 0.2–5.0 yr−1 Gpc−3 in the Local Universe for the highest mass-transfer efficiencies explored here. The highest rate densities lead to detection rates of 1.2–3.3 yr−1, which are compatible with the observed rates. The common-envelope efficiency αCE has a strong impact on the progenitor populations. A high-efficiency scenario with αCE = 2.0 is favoured when comparing the expected rates with the observations.
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Rose, Sanaea C., Smadar Naoz, and Aaron M. Geller. "Companion-driven evolution of massive stellar binaries." Monthly Notices of the Royal Astronomical Society 488, no. 2 (July 8, 2019): 2480–92. http://dx.doi.org/10.1093/mnras/stz1846.
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ABSTRACT At least $70\, {\rm per\, cent}$ of massive OBA-type stars reside in binary or higher order systems. The dynamical evolution of these systems can lend insight into the origins of extreme phenomena such as X-ray binaries and gravitational wave sources. In one such dynamical process, the Eccentric Kozai–Lidov (EKL) mechanism, a third companion star alters the secular evolution of a binary system. For dynamical stability, these triple systems must have a hierarchical configuration. We explore the effects of a distant third companion’s gravitational perturbations on a massive binary’s orbital configuration before significant stellar evolution has taken place (≤10 Myr). We include tidal dissipation and general relativistic precession. With large (38 000 total) Monte Carlo realizations of massive hierarchical triples, we characterize imprints of the birth conditions on the final orbital distributions. Specifically, we find that the final eccentricity distribution over the range of 0.1–0.7 is an excellent indicator of its birth distribution. Furthermore, we find that the period distributions have a similar mapping for wide orbits. Finally, we demonstrate that the observed period distribution for approximately 10-Myr-old massive stars is consistent with EKL evolution.
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Hamilton, Chris, and Roman R. Rafikov. "Secular dynamics of binaries in stellar clusters – II. Dynamical evolution." Monthly Notices of the Royal Astronomical Society 488, no. 4 (August 5, 2019): 5512–35. http://dx.doi.org/10.1093/mnras/stz2026.
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AbstractDense stellar clusters are natural sites for the origin and evolution of exotic objects such as relativistic binaries (potential gravitational wave sources) and blue stragglers. We investigate the secular dynamics of a binary system driven by the global tidal field of an axisymmetric stellar cluster in which the binary orbits. In a companion paper we developed a general Hamiltonian framework describing such systems. The effective (doubly-averaged) Hamiltonian derived there encapsulates all information about the tidal potential experienced by the binary in its orbit around the cluster in a single parameter Γ. Here we provide a thorough exploration of the phase-space of the corresponding secular problem as Γ is varied. We find that for Γ > 1/5 the phase-space structure and the evolution of binary orbital elements are qualitatively similar to the Lidov–Kozai problem. However, this is only one of four possible regimes, because the dynamics are qualitatively changed by bifurcations at Γ = 1/5, 0, −1/5. We show how the dynamics are altered in each regime and calculate characteristics such as the secular evolution time-scale and maximum possible eccentricity. We verify the predictions of our doubly-averaged formalism numerically and find it to be very accurate when its underlying assumptions are fulfilled, typically meaning that the secular time-scale should exceed the period of the binary around the cluster by ≳10–102 (depending on the cluster potential and binary orbit). Our results may be relevant for understanding the nature of a variety of exotic systems harboured by stellar clusters.
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Li, Zhongmu, and Zhanwen Han. "The role of binary stars in stellar population synthesis." Proceedings of the International Astronomical Union 4, S252 (April 2008): 359–64. http://dx.doi.org/10.1017/s1743921308023211.
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AbstractMore than about 50% stars are in binaries, but the effects of binary evolution were not taken into account in most previous stellar population synthesis studies. In fact, binaries can affect the integrated peculiarities such as spectral energy distributions (SEDs), colours, and line-strength indices of populations. With the effects of binary stars taken into account, some new results for stellar population studies will be shown. We discuss how binaries affect the colours and Lick indices of simple stellar populations, and the measurement of stellar ages and metallicities.
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Wang, Long, Pavel Kroupa, Koh Takahashi, and Tereza Jerabkova. "The possible role of stellar mergers for the formation of multiple stellar populations in globular clusters." Monthly Notices of the Royal Astronomical Society 491, no. 1 (October 31, 2019): 440–54. http://dx.doi.org/10.1093/mnras/stz3033.
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ABSTRACT Many possible scenarios for the formation of multiple stellar populations (MSPs) in globular clusters (GCs) have been discussed so far, including the involvement of asymptotic giant branch stars, fast-rotating main-sequence stars, very massive main-sequence stars and mass-transferring massive binaries based on stellar evolution modelling. But self-consistent, dynamical simulations of very young GCs are usually not considered. In this work, we perform direct N-body modelling of such systems with total masses up to 3.2 × 105 M⊙, taking into account the observationally constrained primordial binary properties, and discuss the stellar mergers driven both by binary stellar evolution and dynamical evolution of GCs. The occurrence of stellar mergers is enhanced significantly in binary-rich clusters such that stars forming from the gas polluted by merger-driven ejection/winds would appear as MSPs. We thus emphasize that stellar mergers can be an important process that connects MSP formation with star cluster dynamics, and that multiple MSP formation channels can naturally work together. The scenario studied here, also in view of a possible top-heavy initial mass function, may be particularly relevant for explaining the high mass fraction of MSPs (the mass budget problem) and the absence of MSPs in young and low-mass star clusters.
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Andronov, I. L. "Peculiarities of stellar evolution in binary and multiple systems." Astronomical School’s Report 2, no. 1 (2001): 58–76. http://dx.doi.org/10.18372/2411-6602.02.1058.
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Negu, Seblu Humne, and Solomon Belay Tessema. "Mass Transfer in Binary Stellar Evolution and Its Stability." International Journal of Astronomy and Astrophysics 05, no. 03 (2015): 222–41. http://dx.doi.org/10.4236/ijaa.2015.53026.
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Li, Zhongmu, and Caiyan Mao. "Evolution of Optical Binary Fraction in Sparse Stellar Systems." Astrophysical Journal 859, no. 1 (May 22, 2018): 36. http://dx.doi.org/10.3847/1538-4357/aabc09.
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Fregeau, John M., Natalia Ivanova, and Frederic A. Rasio. "EVOLUTION OF THE BINARY FRACTION IN DENSE STELLAR SYSTEMS." Astrophysical Journal 707, no. 2 (December 7, 2009): 1533–40. http://dx.doi.org/10.1088/0004-637x/707/2/1533.
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Torres, G. "Observational constraints from binary stars on stellar evolution models." EAS Publications Series 64 (2013): 87–94. http://dx.doi.org/10.1051/eas/1364012.
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Sicilia, Alex, Andrea Lapi, Lumen Boco, Mario Spera, Ugo N. Di Carlo, Michela Mapelli, Francesco Shankar, David M. Alexander, Alessandro Bressan, and Luigi Danese. "The Black Hole Mass Function Across Cosmic Times. I. Stellar Black Holes and Light Seed Distribution." Astrophysical Journal 924, no. 2 (January 1, 2022): 56. http://dx.doi.org/10.3847/1538-4357/ac34fb.
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Abstract This is the first paper in a series aimed at modeling the black hole (BH) mass function, from the stellar to the intermediate to the (super)massive regime. In the present work, we focus on stellar BHs and provide an ab initio computation of their mass function across cosmic times; we mainly consider the standard, and likely dominant, production channel of stellar-mass BHs constituted by isolated single/binary star evolution. Specifically, we exploit the state-of-the-art stellar and binary evolutionary code SEVN, and couple its outputs with redshift-dependent galaxy statistics and empirical scaling relations involving galaxy metallicity, star formation rate and stellar mass. The resulting relic mass function dN / dVd log m • as a function of the BH mass m • features a rather flat shape up to m • ≈ 50 M ⊙ and then a log-normal decline for larger masses, while its overall normalization at a given mass increases with decreasing redshift. We highlight the contribution to the local mass function from isolated stars evolving into BHs and from binary stellar systems ending up in single or binary BHs. We also include the distortion on the mass function induced by binary BH mergers, finding that it has a minor effect at the high-mass end. We estimate a local stellar BH relic mass density of ρ • ≈ 5 × 107 M ⊙ Mpc−3, which exceeds by more than two orders of magnitude that in supermassive BHs; this translates into an energy density parameter Ω• ≈ 4 × 10−4, implying that the total mass in stellar BHs amounts to ≲1% of the local baryonic matter. We show how our mass function for merging BH binaries compares with the recent estimates from gravitational wave observations by LIGO/Virgo, and discuss the possible implications for dynamical formation of BH binaries in dense environments like star clusters. We address the impact of adopting different binary stellar evolution codes (SEVN and COSMIC) on the mass function, and find the main differences to occur at the high-mass end, in connection with the numerical treatment of stellar binary evolution effects. We highlight that our results can provide a firm theoretical basis for a physically motivated light seed distribution at high redshift, to be implemented in semi-analytic and numerical models of BH formation and evolution. Finally, we stress that the present work can constitute a starting point to investigate the origin of heavy seeds and the growth of (super)massive BHs in high-redshift star-forming galaxies, that we will pursue in forthcoming papers.
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Gazeas, K. D., G. A. Loukaidou, P. G. Niarchos, S. Palafouta, D. Athanasopoulos, A. Liakos, S. Zola, A. Essam, and P. Hakala. "CoBiToM project – I. Contact binaries towards merging." Monthly Notices of the Royal Astronomical Society 502, no. 2 (January 29, 2021): 2879–92. http://dx.doi.org/10.1093/mnras/stab234.
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ABSTRACT Binary and multiple stellar systems are numerous in our solar neighbourhood with 80 per cent of the solar-type stars being members of systems with high order multiplicity. The Contact Binaries Towards Merging (CoBiToM) Project is a programme that focuses on contact binaries and multiple stellar systems, as a key for understanding stellar nature. The goal is to investigate stellar coalescence and merging processes, as the final state of stellar evolution of low-mass contact binary systems. Obtaining observational data of approximately 100 eclipsing binaries and multiple systems and more than 400 archival systems, the programme aspires to give insights for their physical and orbital parameters and their temporal variations, e.g. the orbital period modulation, spot activity etc. Gravitational phenomena in multiple-star environments will be linked with stellar evolution. A comprehensive analysis will be conducted, in order to investigate the possibility of contact binaries to host planets, as well as the link between inflated hot Jupiters and stellar mergers. The innovation of CoBiToM Project is based on a multimethod approach and a detailed investigation, that will shed light for the first time on the origin of stellar mergers and rapidly rotating stars. In this work, we describe the scientific rationale, the observing facilities to be used and the methods that will be followed to achieve the goals of CoBiToM Project and we present the first results as an example of the current research on evolution of contact binary systems.
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Daher, Christine Mazzola, Carles Badenes, Jamie Tayar, Marc Pinsonneault, Sergey E. Koposov, Kaitlin Kratter, Maxwell Moe, et al. "Stellar multiplicity and stellar rotation: insights from APOGEE." Monthly Notices of the Royal Astronomical Society 512, no. 2 (March 4, 2022): 2051–61. http://dx.doi.org/10.1093/mnras/stac590.
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ABSTRACT We measure rotational broadening in spectra taken by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey to characterize the relationship between stellar multiplicity and rotation. We create a sample of 2786 giants and 24 496 dwarfs with stellar parameters and multiple radial velocities from the APOGEE pipeline, projected rotation speeds vsin i determined from our own pipeline, and distances, masses, and ages measured by Sanders & Das. We use the statistical distribution of the maximum shift in the radial velocities, ΔRVmax, as a proxy for the close binary fraction to explore the interplay between stellar evolution, rotation, and multiplicity. Assuming that the minimum orbital period allowed is the critical period for Roche Lobe overflow and rotational synchronization, we calculate theoretical upper limits on expected vsin i and ΔRVmax values. These expectations agree with the positive correlation between the maximum ΔRVmax and vsin i values observed in our sample as a function of log(g). We find that the fast rotators in our sample have a high occurrence of short-period [log(P/d) ≲ 4] companions. We also find that old, rapidly rotating main-sequence stars have larger completeness-corrected close binary fractions than their younger peers. Furthermore, rapidly rotating stars with large ΔRVmax consistently show differences of 1–10 Gyr between the predicted gyrochronological and measured isochronal ages. These results point towards a link between rapid rotation and close binarity through tidal interactions. We conclude that stellar rotation is strongly correlated with stellar multiplicity in the field, and caution should be taken in the application of gyrochronology relations to cool stars.
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Li, Z. M., C. Y. Mao, L. Chen, and Q. Zhang. "Binary Star Stellar Population Synthesis Model For Astrophysical Studies." Proceedings of the International Astronomical Union 9, S298 (May 2013): 422. http://dx.doi.org/10.1017/s1743921313006881.
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AbstractBinary stars possibly exists in most galaxies and star clusters. Their evolution can lead to significant change in stellar population studies. Binary star to fit group (BS2fit: ∞) has built up a binary star stellar population synthesis model and used it in a few works. This page is to introduce the model and its possible applications.
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Statler, Thomas S., Jeremiah P. Ostriker, and Haldan N. Cohn. "Evolution of Globular Clusters by Tidally-Captured Binaries through Core Collapse." Symposium - International Astronomical Union 126 (1988): 667–68. http://dx.doi.org/10.1017/s0074180900043527.
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We present calculations of globular cluster evolution performed by a modified Fokker-Planck approach, in which binaries formed by tidal capture are followed explicitly, along with subsequent heating mechanisms. The cluster is simulated by a two component model, using the cross sections of Press and Teukolsky (1977) for tidal capture, those of Hut (1984) for the single-binary encounters and for distant binary-binary encounters, and those of Mikkola (1983) for the strong binary-binary encounters. The initial state of the cluster is a Plummer model with N = 3 × 105 and scale radius ro = 1.13 pc. All stars are identical, with mass M∗ = 0.7M⊙ and R∗ = 0.57R⊙. This gives an initial core radius rc = 0.8 pc, and one-dimensional dispersion σ = 11.6 km s-1. All binaries are assumed to be identical, with separation a = 2.5R∗. There are no binaries in the cluster initially. Additional important effects, such as tidal truncation, tidal shocks, stellar evolution and mass loss, and stellar mergers, are not included.
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Taylor, J. H. "Binary Pulsars: Observations and Implications." Symposium - International Astronomical Union 125 (1987): 383–92. http://dx.doi.org/10.1017/s0074180900161005.
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The Galaxy contains a large number of neutron stars in gravitation-ally bound binary systems. Among the most fruitful of these to study have been the binary radio pulsars, of which seven are now known. Unlike the “accretion-powered” neutron stars located in mass-exchanging X-ray binary systems, the “rotation-powered” binary radio pulsars are found in dynamically simple, clean systems in which both stellar components have already completed their nuclear evolution, thereby shedding their atmospheres and most of their mass. In such circumstances the orbital parameters of the system and the rotational parameters of the pulsar can be determined with high precision from analysis of pulse timing data. These measurements constrain the component masses and yield an estimate of the pulsar's magnetic dipole moment, which turns out to be an essential parameter in understanding the evolution of the systems. In this paper I review the known facts concerning binary pulsars, and then briefly discuss some implications for our understanding of the place of neutron stars in stellar evolution.
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Patel, Ruskin, and Kaloyan Penev. "Constraining tidal quality factor using spin period in eclipsing binaries." Monthly Notices of the Royal Astronomical Society 512, no. 3 (March 11, 2022): 3651–61. http://dx.doi.org/10.1093/mnras/stac203.
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ABSTRACT Evolution of binary objects under the influence of tides drastically affects the expected observational properties of the system. With the discovery of a large number of close-in hot Jupiter systems and eclipsing binaries from missions such as Kepler and Transiting Exoplanet Survey Satellite, it has become imperative to understand the extent of tidal influence on their formation and observed properties. In the case of binary systems, an efficient tidal dissipation can lead to either spin-up or spin-down of the stars and/or spin–orbit synchronization, depending upon the exchange of angular momentum between the star and the orbit. We combine the eclipsing binary systems from the Kepler mission with stellar and orbital parameters available in the literature to create a catalogue of 41 eclipsing binaries suitable for analysis of tidal dissipation. Empirically, the efficiency of tidal dissipation is parametrized using a modified tidal quality factor ($Q_{\star }^{\prime }$). We find constraints on $Q_{\star }^{\prime }$ using the observed rotation period of the primary star in the eclipsing binary systems. We calculate detailed evolutions of binary systems under the combined influence of tides, stellar evolution, and loss of stellar angular momentum to magnetic winds, and perform Markov chain Monte Carlo simulations to account for the uncertainties in the observed data. Our analysis shows that $\log _{10}{Q^{\prime }_{\star }}=7.818\pm 0.035$ can reproduce the observed primary star spin in almost all systems in our sample.
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Mathieu, Robert D. "Disks in the Pre-Main Sequence Binary Environment." Symposium - International Astronomical Union 151 (1992): 21–30. http://dx.doi.org/10.1017/s0074180900122028.
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