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Relevant bibliographies by topics / Binary stars; Eclipse mapping

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Academic literature on the topic 'Binary stars; Eclipse mapping'

Author: Grafiati

Published: 4 June 2021

Last updated: 14 February 2022

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Journal articles on the topic "Binary stars; Eclipse mapping"

1

Cameron, A. C. "Eclipse mapping of late-type close binary stars." Monthly Notices of the Royal Astronomical Society 287, no. 3 (May 21, 1997): 556–66. http://dx.doi.org/10.1093/mnras/287.3.556.

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Nuspl, J., and I. B. Bíró. "Eclipse Mapping of Non-Radial Pulsation in Binary Stars." International Astronomical Union Colloquium 185 (2002): 100–101. http://dx.doi.org/10.1017/s0252921100015669.

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AbstractWe review a slightly modified method of eclipse mapping, applicable to mode identification in eclipsing binaries containing a pulsating component. The observed light curve is used by the procedure without removing from it the badly determined eclipsing part.

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Kaitchuck, Ronald H. "How Does One Detect An Accretion Disk?" Symposium - International Astronomical Union 151 (1992): 175–83. http://dx.doi.org/10.1017/s007418090012217x.

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The history of the first detection of an accretion disk in a interacting binary system is presented. The nature of transient and permanent disks in Algol-type binaries is discussed as are the problems associated with the interpretation of emission line profiles from the disks in cataclysmic variable stars. The new technique of eclipse mapping from continuum photometry is reviewed. Some results of Doppler tomography of emission lines are presented.

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Latković, Olivera, and Attila Cséki. "Modeling non-radial oscillations on components of close binaries." Proceedings of the International Astronomical Union 9, S301 (August 2013): 447–48. http://dx.doi.org/10.1017/s1743921313014981.

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AbstractWe developed an advanced binary system model that includes stellar oscillations on one or both stars, with the goal of mode identification by fitting of the photometric light curves. The oscillations are modeled as perturbations of the local surface temperature and the local gravitational potential. In the case of tidally distorted stars, it is assumed that the pulsation axis coincides with the direction connecting the centers of the components rather than with the rotation axis. The mode identification method, originally devised by B. Bíró, is similar to eclipse mapping in that it utilizes the amplitude, phase and frequency modulation of oscillations during the eclipse; but the identification is achieved by grid-fitting of the observed light curve rather than by image reconstruction. The proposed model and the mode identification method have so far been tested on synthetic data with encouraging results.

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Lehmann, H., V. Tsymbal, F. Pertermann, A. Tkachenko, D. E. Mkrtichian, and N. A-thano. "Spectroscopic time-series analysis of R Canis Majoris." Astronomy & Astrophysics 615 (July 2018): A131. http://dx.doi.org/10.1051/0004-6361/201629914.

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R Canis Majoris is the prototype of a small group of Algol-type stars showing short orbital periods and low mass ratios. A previous detection of short-term oscillations in its light curve has not yet been confirmed. We investigate a new time series of high-resolution spectra with the aim to derive improved stellar and system parameters, to search for the possible impact of a third component in the observed spectra, to look for indications of activity in the Algol system, and to search for short-term variations in radial velocities. We disentangled the composite spectra into the spectra of the binary components. Then we analysed the resulting high signal-to-noise spectra of both stars. Using a newly developed program code based on an improved method of least-squares deconvolution, we were able to determine the radial velocities of both components also during primary eclipse. This allowed us to develop a better model of the system including the Rossiter–McLaughlin effect and to derive improved orbital parameters. Combining the results with those from spectrum analysis, we obtain accurate stellar and system parameters. We further deduce at least one oscillation frequency of 21.38 c d−1. It could be detected during primary eclipses only and confirms a previous photometric finding. Results point to an amplitude amplification of non-radial pulsation modes due to the eclipse mapping effect. The presence of a He I line in the spectra indicates mass transfer in the R CMa system. Calculations of its Roche geometry give evidence that the cool secondary component may fill its Roche lobe. No evidence of a third body in the system could be found in the observed spectra.

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Horne, Keith. "Tomography of Accretion Flows in Binary Stars and Active Galactic Nuclei." International Astronomical Union Colloquium 163 (1997): 14–26. http://dx.doi.org/10.1017/s0252921100042469.

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AbstractAstrotomography resolves accretion flows with micro-arcsecond angular resolution. Eclipses by a binary companion star slice up a disk surface, giving monochromatic maps of the disk, or spectra from any region of its surface. Doppler tomography maps emission-line regions from the changing velocity profile as the binary rotates, revealing radial and azimuthal structure, gas streams, irradiated companion stars, magnetic flows, and slingshot prominences. Echo mapping exploits time delays between the hard radiation from near the compact object at the focus of the flow, and softer emission generated by irradiation of regions farther out. The maximum entropy techniques for fitting intensity maps to data are currently being extended by incorporating local physics and mapping physical parameters such as temperature, density, surface density, and velocity dispersion.

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Lehmann, Holger, David Mkrtichian, and Andrew Tkachenko. "Spectroscopic eclipse mapping of oEA stars." Journal of Physics: Conference Series 118 (October 1, 2008): 012062. http://dx.doi.org/10.1088/1742-6596/118/1/012062.

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Rutten, René G. M. "Eclipse mapping and related techniques." Symposium - International Astronomical Union 176 (1996): 69–84. http://dx.doi.org/10.1017/s007418090008311x.

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Eclipse mapping is a technique to deduce spatial structure on very small angular scales in eclipsing cataclysmic variable stars (CVs). By analysing the eclipse light curve, information is obtained on the brightness structure of the accretion disk and of the compact mass-accreting object in these systems. This information would otherwise be well beyond the resolving power of any optical telescope. Since the development of the eclipse mapping technique by K. Horne, about one decade ago, it has now become an important tool in the study of CVs. Originally eclipse mapping was employed to construct brightness maps of accretion disks in broad spectral bands. Recently, maps of much higher spectral resolution have become available from which optical and UV spectra have been reconstructed in spatial detail across accretion disks. Such information is very important for our understanding of the physics of the accretion process.In this paper I will describe the eclipse mapping technique and review recent results. In conjunction, I will briefly highlight other techniques related to the mapping of surface structure in CVs.

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Schmitt, J. H. M. M. "Eclipse mapping at X-ray wavelengths." Symposium - International Astronomical Union 176 (1996): 85–94. http://dx.doi.org/10.1017/s0074180900083121.

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Stellar coronae cannot be spatially resolved, and yet stellar coronae are likely to exhibit a similar amount of structure as the solar corona. Currently, the only way to infer structure from spatially unresolved data is to look for rotational modulation of the X-ray emission or eclipses in the case of binary systems. I will discuss some of the observations obtained and critically review the methods used to infer structure from these data. Particular emphasis will be placed on the ill-conditioned nature of the inversion problem, that makes it next to impossible to infer the possibly three-dimensional structure of stellar coronae.

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von Boetticher, Alexander, Amaury H. M. J. Triaud, Didier Queloz, Sam Gill, Pierre F. L. Maxted, Yaseen Almleaky, David R. Anderson, et al. "The EBLM Project." Astronomy & Astrophysics 625 (May 2019): A150. http://dx.doi.org/10.1051/0004-6361/201834539.

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Measurements of the physical properties of stars at the lower end of the main sequence are scarce. In this context we report masses, radii and surface gravities of ten very-low-mass stars in eclipsing binary systems, with orbital periods of the order of several days. The objects probe the stellar mass-radius relation in the fully convective regime, M⋆ ≲ 0.35 M⊙, down to the hydrogen burning mass-limit, MHB ∼ 0.07 M⊙. The stars were detected by the WASP survey for transiting extra-solar planets, as low-mass, eclipsing companions orbiting more massive, F- and G-type host stars. We use eclipse observations of the host stars, performed with the TRAPPIST, Leonhard Euler and SPECULOOS telescopes, and radial velocities of the host stars obtained with the CORALIE spectrograph, to determine the physical properties of the low-mass companions. Surface gravities of the low-mass companions are derived from the eclipse and orbital parameters of each system. Spectroscopic measurements of the host star effective temperature and metallicity are used to infer the host star mass and age from stellar evolution models for solar-type stars. Masses and radii of the low-mass companions are then derived from the eclipse and orbital parameters of the binary systems. The objects are compared to stellar evolution models for low-mass stars, to test for an effect of the stellar metallicity and orbital period on the radius of low-mass stars in close binary systems. Measurements are found to be in good agreement with stellar evolution models; a systematic inflation of the radius of low-mass stars with respect to model predictions is limited to 1.6 ± 1.2%, in the fully convective low-mass regime. The sample of ten objects indicates a scaling of the radius of low-mass stars with the host star metallicity. No correlation between stellar radii and the orbital periods of the binary systems is determined. A combined analysis with thirteen comparable objects from the literature is consistent with this result.

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Dissertations / Theses on the topic "Binary stars; Eclipse mapping"

1

Billington, Ian Michael. "Images of accretion discs in cataclysmic variables." Thesis, University of Oxford, 1995. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.308377.

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Ioannou, Zacharias. "Multiwavelength studies of accretion discs and coronae in interacting binary stars." Thesis, Keele University, 2000. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.327632.

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Kube, Jens. "Indirect imaging of cataclysmic variable stars." Doctoral thesis, [S.l.] : [s.n.], 2002. http://webdoc.sub.gwdg.de/diss/2002/kube/kube.pdf.

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Books on the topic "Binary stars; Eclipse mapping"

1

Ake, Thomas B., and Elizabeth Griffin, eds. Giants of Eclipse: The ζ Aurigae Stars and Other Binary Systems. Cham: Springer International Publishing, 2015. http://dx.doi.org/10.1007/978-3-319-09198-3.

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Ake, Thomas B., and Elizabeth Griffin. Giants of Eclipse: The ζ Aurigae Stars and Other Binary Systems. Springer, 2014.

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Book chapters on the topic "Binary stars; Eclipse mapping"

1

Huber, Daniel. "Asteroseismology of Eclipsing Binary Stars." In Giants of Eclipse: The ζ Aurigae Stars and Other Binary Systems, 169–94. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-09198-3_7.

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Nha, IL-Seong. "Atmospheric Eclipsing Binary Zeta Aurigae in the 1987-1988 Eclipse." In Evolutionary Processes in Interacting Binary Stars, 399–402. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2542-0_58.

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Airapetian, Vladimir S., and Manfred Cuntz. "Atmospheric Heating and Wind Acceleration in Cool Evolved Stars." In Giants of Eclipse: The ζ Aurigae Stars and Other Binary Systems, 123–56. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-09198-3_5.

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Griffin, R. Elizabeth, and Thomas B. Ake. "The ζ Aurigae Binaries." In Giants of Eclipse: The ζ Aurigae Stars and Other Binary Systems, 1–14. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-09198-3_1.

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Griffin, R. Elizabeth, Joel A. Eaton, Thomas B. Ake, and Klaus-Peter Schröder. "Observing and Analyzing the ζ Aurigae Systems." In Giants of Eclipse: The ζ Aurigae Stars and Other Binary Systems, 15–84. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-09198-3_2.

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Bennett, Philip D., and Wendy Hagen Bauer. "The Special Case of VV Cephei." In Giants of Eclipse: The ζ Aurigae Stars and Other Binary Systems, 85–106. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-09198-3_3.

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Stencel, Robert E. "ϵ Aurigae: A Two Century Long Dilemma Persists." In Giants of Eclipse: The ζ Aurigae Stars and Other Binary Systems, 107–21. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-09198-3_4.

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Kloppenborg, Brian, and Gerard van Belle. "Optical Interferometry of Giants and Supergiants." In Giants of Eclipse: The ζ Aurigae Stars and Other Binary Systems, 157–68. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-09198-3_6.

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Williams, P. M., K. A. Van Der Hucht, T. A. Th Spoelstra, and J. P. Swaanenvelt. "Radio Light-Curves and Circumstellar Mapping of the Colliding Wind Binary WR140." In Wolf-Rayet Stars: Binaries, Colliding Winds, Evolution, 504–5. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-011-0205-6_105.

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