Relevant bibliographies by topics / Binary stellar evolution

Academic literature on the topic 'Binary stellar evolution'

Author: Grafiati
Published: 10 December 2022
Last updated: 28 January 2023

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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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Dissertations / Theses on the topic "Binary stellar evolution"

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Pols, Onno Rudolf. "On the evolution of massive close binary stars in stellar populations." Amsterdam : Amsterdam : Sterrenkundig Instituut 'Anton Pannekoek' ; Universiteit van Amsterdam [Host], 1993. http://dare.uva.nl/document/91990.

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Barrett, James William. "Topics in astrostatistics : stellar binary evolution, gravitational-wave source modelling and stochastic processes." Thesis, University of Birmingham, 2018. http://etheses.bham.ac.uk//id/eprint/8203/.

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The effective use of statistical techniques is one of the cornerstones of modern astrophysics. In this thesis we use sophisticated statistical methodology to expand our understanding of astrophysics. In particular, we focus on the physics of coalescing binary black holes, and the observation of these events using gravitational-wave astronomy. We use Fisher matrices to explore how much we expect to learn from gravitational-wave observations, and then use machine learning techniques, including random forests and Gaussian processes, to facilitate an otherwise intractable Bayesian comparison of real observations to our model. Finally, we develop a technique based on Gaussian processes for characterising stochastic variability in time series data.
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Saffer, R. A., and J. Liebert. "Search for Close Binary Evolved Stars." Steward Observatory, The University of Arizona (Tucson, Arizona), 1988. http://hdl.handle.net/10150/623897.

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We report on a search for short -period binary systems composed of pairs of evolved stars. The search is being carried out concurrently with a program to characterize the kinematical properties of two different samples of stars. Each sample has produced one close binary candidate for which further spectroscopic observations are planned. We also recapitulate the discovery of a close detached binary system composed of two cool DA white dwarfs, and we discuss the null results of Ha observations of the suspected white dwarf /brown dwarf system G 29-38.
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Ohlmann, Sebastian Thomas [Verfasser], and Friedrich [Akademischer Betreuer] Röpke. "Hydrodynamics of the Common Envelope Phase in Binary Stellar Evolution / Sebastian Thomas Ohlmann ; Betreuer: Friedrich Röpke." Heidelberg : Universitätsbibliothek Heidelberg, 2016. http://d-nb.info/1180615891/34.

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Ohlmann, Sebastian T. [Verfasser], and Friedrich [Akademischer Betreuer] Röpke. "Hydrodynamics of the Common Envelope Phase in Binary Stellar Evolution / Sebastian Thomas Ohlmann ; Betreuer: Friedrich Röpke." Heidelberg : Universitätsbibliothek Heidelberg, 2016. http://nbn-resolving.de/urn:nbn:de:bsz:16-heidok-215131.

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Moran, Chris. "Using observations of detached double degenerate binaries to test theories of stellar evolution in close binary systems." Thesis, University of Southampton, 1999. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.310751.

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Douchin, Dimitri. "Estimation de la fraction binaire de nébuleuses planétaires." Thesis, Montpellier 2, 2014. http://www.theses.fr/2014MON20069/document.

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Les nébuleuses planétaires (NP) sont le produit de l'évolution d'étoiles de masses intermédiaires après leur expansion sphérique à la fin de leurs vies. Il a été estimé observationnellement que 80 % des NP ont des formes non-sphériques. Une fraction si élevée est déroutante et a mobilisé la communauté de recherche sur les NP pendant plus de trente ans. Un scénario qui permettrait de justifier les formes observées serait que les étoiles progénitrices de noyaux de NP (NNP) ne sont pas simples, mais possèdent un compagnon. Les formes des nébuleuses seraient ainsi le résultat de l'interaction avec le compagnon. La fraction si élevée de NP non-sphériques impliquerait donc une fraction élevée de NNP binaires, faisant de la parité stellaire un canal de formation privilégié pour les NP. Après avoir présenté l'état de connaissance actuelle concernant la formation et la mise en forme des NP, je présente mes travaux visant à détecter un excès infrarouge qui serait la signature de la présence d'un compagnon orbitant le NNP. La première partie de ce projet consiste en l'analyse de données et photométrie acquises par moi-même. Dans la deuxième partie je présente une tentative d'utilisation de jeux de données d'archives : la campagne optique Sloan Digital Sky Survey Data Release 7 et la version étendue de la base de données assemblée par Frew (2008). Je présente aussi les résultats d'une analyse de vitesses radiales de spectres VLT/UVES pour 14 NNP dans le but de détecter des compagnons spectroscopiques. Finalement j'expose les détails d'une analyse de photométrie de données optiques dans le but de détecter des compagnons orbitant autour de NNP en utilisant la technique de variabilité photométrique. Le résultat principal de cette thèse réside dans les analyses d'excès infrarouge proche que je combine avec des données publiées précédemment. Je conclus que si la fraction détectée d'excès infrarouge proche est attribuée à la présence de compagnons stellaires, alors la fraction binaire de NNP est plus grande que celle attendue en se basant sur la population binaire de progéniteurs de la séquence principale et ainsi conclus que la multiplicité stellaire est un canal de formation privilégié pour la formation des NP. Je clos en soulignant la nécessité d'un échantillon d'étude d'environ 150 objets pour réduire l'incertitude sur la fraction binaire et appuyer les conclusions statistiques de ce résultat
Planetary nebulae (PNe) are the products of the evolution of intermediate mass stars that have expanded spherically at the end of their lives. Observationally, it has been estimated that 80% of them have non-spherical shapes. Such a high fraction is puzzling and has occupied the PN community for more than 30 years. One scenario that would allow to justify the observed shapes is that a comparable fraction of the progenitors of central stars of PN (CSPN) are not single, but possess a companion. The shape of the nebulae would then be the result of an interaction with this companion. The high fraction of non-spherical PNe would thus imply a high fraction of binary CSPN, making binarity a preferred channel for PN formation. After presenting the current state of knowledge regarding PN formation and shaping and reviewing the diverse efforts to find binaries in PNe, I present my work to detect a near-infrared excess that would be the signature of the presence of cool companions. The first part of the project consists in the analysis of data and photometry acquired and conducted by myself. The second part details an attempt to make use of archived datasets: the Sloan Digital Sky Survey Data Release 7 optical survey and the extended database assembled by Frew (2008). I also present results from a radial velocity analysis of VLT/UVES spectra for 14 objects aiming to the detection of spectroscopic companions. Finally I give details of the analysis of optical photometry data from our observations associated to the detection of companions around CSPN using the photometric variability technique. The main result of this thesis is from the near-infrared excess studies which I combine with previously-published data. I conclude that the if the detected red and NIR flux excess is indicative of a stellar companion then the binary fraction is larger than what we may expect based on the main-sequence progenitor population binary fraction and therefore conclude that binarity is a preferential channel for the formation of PN. I finish by underlining the need for a sample size of ∼ 150 objects to decrease the uncertainty on the PN population binary fraction and increase the statistical significance of this result
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Deschamps, Romain. "Evolution of low and intermediate mass stars in binary systems: a new look at Algol systems." Doctoral thesis, Universite Libre de Bruxelles, 2015. http://hdl.handle.net/2013/ULB-DIPOT:oai:dipot.ulb.ac.be:2013/209077.

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Despite being observed since the XVIIIth century, Algol systems and related objects are

still rather poorly understood. We know that they are composed by a generally B-A main sequence

star and a lighter but more evolved companion star. This paradox is explained by the transfer of mass

between the two stars, but new problems arose. In particular, I studied the mass-transfer driven spin-

up of the accreting star that drives the star to critical rotation and the puzzling, indirectly observed, non-conservative evolution.
Doctorat en Sciences
info:eu-repo/semantics/nonPublished

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Santos, Leonardo Augusto Gonçalves dos. "The rotational evolution of Sun-like stars and the influence of low-mass binary companions." Universidade de São Paulo, 2017. http://www.teses.usp.br/teses/disponiveis/14/14131/tde-22052018-174015/.

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The Solar Twin Planet Search program is an unprecedented eort that aimed to procure extrasolar planets in more than 70 stars extremely similar to the Sun. In the course of this program, hundreds of high-quality optical spectra were obtained for these stars using the HARPS spectrograph, which is fed by the ESO La Silla 3.6 m telescope. Beyond the search for exoplanets, the data are invaluable to study the physical properties of Sun-like stars. Particularly in this dissertation, we are interested in verifying if the Sun possesses a regular rotation for its age among stars that are strictly similar to it, how the rotation of solar twins evolve with age and if the rotation of Sun-like stars is influenced by the presence of stellar mass companions. Previous conclusions on the regularity of the Suns rotation have been conflicting, and this is the first time such a large sample of solar twins with high quality spectroscopic data is used to clarify this puzzle. Our results suggest that the Sun is indeed a regular rotator for its age, which favors the use of the solar rotation to calibrate gyrochronology -- the estimation of stellar ages from their rotation. However, these results also imply a rotational evolution process that saturates after the solar age, constituting a departure from the widely used Skumanich relation and posing a challenge for gyrochronology. We securely identified 18 binary or multiple systems in the solar twin sample, of which only three display enhanced rotation for their ages. I estimated the orbital parameters of the binaries from their radial velocity variations, and the results show that their spectroscopic companions lie at orbital periods varying from a few to several years. I conclude that the presence of red or brown dwarf companions at moderate to long orbital periods do not influence the evolution of rotation in these systems, and therefore the main stars should evolve as single in this regard. The peculiarities in HIP 19911, HIP 67620 and HIP 103983 can be fully explained by spectral contamination from their companions.
O programa The Solar Twin Planet Search é um esforço sem precedentes na procura de planetas extra-solares em mais de 70 estrelas extremamente similares ao Sol. Ao longo desse programa, centenas de espectros ópticos de alta qualidade foram obtidos com o espectrógrafo HARPS, que está instalado no telescópio de 3,6 m do Observatório de La Silla. Além da busca de exoplanetas, estes dados são úteis para estudar as propriedades físicas de estrelas como o Sol. Estamos interessados em verificar se o Sol possui uma rotação regular para sua idade quando comparado com estrelas estritamente similares a ele, como que a rotação de gêmeas solares evolui com o tempo e se a rotação dessas estrelas é influenciada pela presença de companheiras estelares. Conclusões anteriores na regularidade da rotação solar são conflitantes, e esta é a primeira vez que uma amostra grande de gêmeas solares com dados espectroscópicos de alta qualidade é usada para esclarecer essa questão. Nossos resultados sugerem que o Sol de fato rota regularmente para sua idade, o que favorece o uso da rotação solar para calibrar a girocronologia -- a estimativa de idades estelares a partir de sua rotação. No entanto, tais resultados também implicam em um processo de evolução rotacional que satura depois da idade solar, constituindo um desvio da amplamente usada relação de Skumanich e apresentando um desafio para a girocronologia. Nós identificamos 18 sistemas binários na amostra de gêmeas solares, das quais apenas três mostram rotações elevadas para suas idades. Os parâmetros orbitais das binárias foram estimados a partir da variação de suas velocidades radiais, e os resultados mostram que suas companheiras espectroscópicas possuem períodos orbitais variando de alguns poucos até muitos anos. Concluimos que a presença de companheiras do tipo anãs vermelhas ou marrons em períodos orbitais moderados não influenciam a evolução rotacional desses sistemas. As peculiaridades de HIP 19911, HIP 67620 e HIP 103983 podem ser completamente explicadas por contaminação espectral de suas companheiras.
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Karakas, Amanda I. (Amanda Irene) 1974. "Asymptotic giant branch stars : their influence on binary systems and the interstellar medium." Monash University, School of Mathematical Sciences, 2003. http://arrow.monash.edu.au/hdl/1959.1/5570.

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Books on the topic "Binary stellar evolution"

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Boffin, Henri M. J., and Giacomo Beccari. Impact of Binary Stars on Stellar Evolution. Cambridge University Press, 2019.

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Boffin, Henri M. J., and Giacomo Beccari. Impact of Binary Stars on Stellar Evolution. University of Cambridge ESOL Examinations, 2019.

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Boffin, Henri M. J., and Giacomo Beccari. Impact of Binary Stars on Stellar Evolution. Cambridge University Press, 2019.

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Beccari, Giacomo, and Henri M. J. Boffin, eds. The Impact of Binary Stars on Stellar Evolution. Cambridge University Press, 2019. http://dx.doi.org/10.1017/9781108553070.

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On the evolution, numbers, and characteristics of close-binary supersoft sources. [Washington, DC: National Aeronautics and Space Administration, 1996.

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Kopal, Zdenek. Binary and Multiple Stars as Tracers of Stellar Evolution: "Proceedings of the 69th Colloquium of the International Astronomical Union, Held in ... Ingramcontent, 2011.

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Tidal evolution and oscillations in binary stars: Third Granada workshop on stellar structure : proceedings of a workshop held in Granada, Spain, 26-28 May 2004. San Francisco, CA: Astronomical Society of the Pacific, 2006.

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Antonio, Claret, Giménez Alvaro, and Zahn Jean-Paul, eds. Tidal evolution and oscillations in binary stars: Third Granada workshop on stellar structure : proceedings of a workshop held in Granada, Spain, 26-28 May 2004. San Francisco, Calif: Astronomical Society of the Pacific, 2005.

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United States. National Aeronautics and Space Administration., ed. Collaborative observations of HDE 332077. [Washington, DC: National Aeronautics and Space Administration, 1995.

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Claret, Antonio. Tidal Evolution and Oscillations in Binary Stars: Third Granada Workshop on Stellar Structure: Proceedings of a Workshop Held in Granada, Spain, 26-28 (Astronomical Society of the Pacific Conference). Astronomical Society of the Pacific, 2005.

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Book chapters on the topic "Binary stellar evolution"

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Benacquista, Matthew. "Stellar Evolution Equations." In An Introduction to the Evolution of Single and Binary Stars, 47–61. New York, NY: Springer New York, 2012. http://dx.doi.org/10.1007/978-1-4419-9991-7_4.

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De Loore, C. W. H., and C. Doom. "Stellar Convection." In Structure and Evolution of Single and Binary Stars, 119–36. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2502-4_7.

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Benvenuto, Omar G., and Melina C. Bersten. "Close Binary Stellar Evolution and Supernovae." In Handbook of Supernovae, 1–22. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-20794-0_124-1.

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Benvenuto, Omar G., and Melina C. Bersten. "Close Binary Stellar Evolution and Supernovae." In Handbook of Supernovae, 649–70. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-21846-5_124.

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Benacquista, Matthew. "Stellar Birth." In An Introduction to the Evolution of Single and Binary Stars, 133–46. New York, NY: Springer New York, 2012. http://dx.doi.org/10.1007/978-1-4419-9991-7_10.

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Frankowski, Adam. "AGB Evolution in Binary Systems." In Post-AGB Objects as a Phase of Stellar Evolution, 173–80. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-015-9688-6_27.

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Eggleton, Peter P., and Ludmila G. Kiseleva. "Stellar and Dynamical Evolution within Triple Stars." In Evolutionary Processes in Binary Stars, 345–64. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-1673-9_17.

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Benacquista, Matthew. "Simple Stellar Models." In An Introduction to the Evolution of Single and Binary Stars, 107–18. New York, NY: Springer New York, 2012. http://dx.doi.org/10.1007/978-1-4419-9991-7_8.

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Pringle, J. E. "Binary Star Formation." In The Physics of Star Formation and Early Stellar Evolution, 437–48. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3642-6_12.

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De Loore, C. W. H., and C. Doom. "The Equations of Stellar Structure." In Structure and Evolution of Single and Binary Stars, 22–35. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2502-4_2.

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Conference papers on the topic "Binary stellar evolution"

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Lister, T. A., and Eric Stempels. "Long term evolution of surface features on the unusual close binary V361 Lyr." In COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099207.

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Marov, M. Ya, and I. I. Shevchenko. "Planets — a modern view." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.005.

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Abstract:
The modern view of planets goes far beyond the usual concept of the planets as bodies of the Solar system. The discovery ofexoplanets has immeasurably expanded the understanding of the architecture and properties of planetary systems. Majoradvances have been made in the study of the planets and minor bodies of the Solar system. However, no answers havebeen received to fundamental questions about the causes of various paths of evolution and formation of planetary naturalcomplexes. To give answers to these questions, research on exoplanets is called upon, of which more than 5000 have beendiscovered to date. Exoplanet studies provide an approach to solving the key problems of stellar-planetary cosmogony —the genesis and evolution of planets as byproduct of star formation. The most urgent problems concern the formation ofplanetary systems around stars of various spectral classes; the nature of hot Jupiters; the reasons for the predominanceof super-Earths and sub-Neptunes, which are absent in the Solar system; stability of planetary systems of binary stars,including circumbinary systems. Of particular interest are terrestrial planets with orbits in zones of “potential habitability”,studies of which open a new page in astrobiology.
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