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

Author: Grafiati

Published: 4 June 2021

Last updated: 14 February 2022

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1

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

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2

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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3

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 (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 uti

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5

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

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6

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 g

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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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8

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

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9

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-dimen

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von Boetticher, Alexander, Amaury H. M. J. Triaud, Didier Queloz, 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 ob

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11

Watson, C. A., and V. S. Dhillon. "The effect of star-spots on eclipse timings of binary stars." Monthly Notices of the Royal Astronomical Society 351, no. 1 (2004): 110–16. http://dx.doi.org/10.1111/j.1365-2966.2004.07763.x.

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12

Royer, Pierre, Gregor Rauw, Jean Manfroid, Eric Gosset, and Jean-Marie Vreux. "Narrow-band photometry of the eclipsing WN7+O binary WR 22." Symposium - International Astronomical Union 193 (1999): 94–95. http://dx.doi.org/10.1017/s0074180900205111.

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In the present paper, we discuss photometric observations of the February 1996 eclipse of the very massive WR+O binary WR 22. Our data were obtained with a set of narrow-band filters, specially designed for the study of WR stars.

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13

Shevchenko, Ivan I. "Habitable worlds of merging stars." International Journal of Astrobiology 19, no. 6 (2020): 500–504. http://dx.doi.org/10.1017/s1473550420000282.

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AbstractIt is shown that W UMa-type and SX Phe-type stellar populations are both perfectly and uniquely suited for maintaining hyper-effective biopolymer chain reactions (BCR) on their planets once the planet is in the stellar habitable zone. W UMa-type stars are known to be contact binaries, and SX Phe-type stars are presumably post-binaries, i.e., products of stellar mergers. In case of the contact binaries, the eclipse-driven periodic heating/cooling of planetary surfaces has period-amplitude parameters that perfectly satisfy stringent conditions for maintaining BCR-like reactions. In case

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Polzin, E. J., R. P. Breton, B. Bhattacharyya, D. Scholte, C. Sobey, and B. W. Stappers. "Study of spider pulsar binary eclipses and discovery of an eclipse mechanism transition." Monthly Notices of the Royal Astronomical Society 494, no. 2 (2020): 2948–68. http://dx.doi.org/10.1093/mnras/staa596.

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ABSTRACT We present a comparative study of the low-frequency eclipses of spider (compact and irradiating binary) PSRs B1957+20 and J1816+4510. Combining these data with those of three other eclipsing systems we study the frequency dependence of the eclipse duration. PSRs B1957+20 and J1816+4510 have similar orbital properties, but the companions to the pulsars have masses that differ by an order of magnitude. A dedicated campaign to simultaneously observe the pulsed and imaged continuum flux densities throughout the eclipses reveals many similarities between the excess material within the two

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15

Nasiroglu, Ilham, Krzysztof Goździewski, Aga Słowikowska, et al. "Searching for planets around eclipsing binary stars using timing method: NSVS 14256825." Proceedings of the International Astronomical Union 12, S330 (2017): 405–6. http://dx.doi.org/10.1017/s1743921317005658.

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AbstractWe present four new mid eclipse times and an updated O-C diagram of the short period eclipsing binary NSVS14256825. The new data follow the (O-C) trend and its model proposed in Nasiroglu et al. (2017). The (O-C) diagram shows quasi-periodic variations that can be explained with the presence of a brown-dwarf in a quasi-circular circumbinary orbit.

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16

Balona, L. A., and J. Cuypers. "An Extraordinary Early-Type Eclipsing Binary." International Astronomical Union Colloquium 139 (1993): 188. http://dx.doi.org/10.1017/s0252921100117270.

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HR 2680 (B5V) was used as a comparison star in a multi-site (ESO & SAAO) campaign organised in 1988 to observe Be stars. We found that the star is an eclipsing binary with a period of 8.1 days. The eclipse is partial with a depth of 0.18 mag. Radial velocity observations confirmed the period.A light variation with an amplitude of as much as 0.03 mag was seen outside the eclipse (Fig. 1). This variation can be interpreted as two oscillations with approximate periods of 1.19 and 1.28 days. Further photometric observations were obtained in 1989, 1990 and 1991 at SAAO. The multiperiodicity was

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17

Welsh, William F., and J. H. Wood. "Eclipse Mapping the Flickering in HT Cas." International Astronomical Union Colloquium 151 (1995): 300–301. http://dx.doi.org/10.1017/s0252921100035259.

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Flickering is a well-known, though poorly understood, signature of accretion in cataclysmic variables. HT Cas is an excellent system in which to study flickering because its well determined characteristics allow a calibration of the experimental system (see Horne et al. 1991).Patterson (1981) argues that the flickering in HT Cas originates from regions very near the white dwarf. In U Gem, the flickering appears to be associated with the bright spot (Warner & Nather 1971). In RW Tri, the flickering occurs throughout the disk but is centrally concentrated (Horne & Stiening 1985); the sam

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18

Borkovits, T., S. A. Rappaport, T. Hajdu, et al. "TICs 167692429 and 220397947: the first compact hierarchical triple stars discovered with TESS." Monthly Notices of the Royal Astronomical Society 493, no. 4 (2020): 5005–23. http://dx.doi.org/10.1093/mnras/staa495.

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ABSTRACT We report the discovery and complex analyses of the first two compact hierarchical triple star systems discovered with TESS in or near its southern continuous viewing zone during Year 1. Both TICs 167692429 and 220397947 were previously unknown eclipsing binaries, and the presence of a third companion star was inferred from eclipse timing variations exhibiting signatures of strong third-body perturbations and, in the first system, also from eclipse depth variations. We carried out comprehensive analyses, including the simultaneous photodynamical modelling of TESS and archival ground-b

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19

Rodriguez, Joseph E., Joshua Pepper, and Keivan G. Stassun. "First Results from the Disk Eclipse Search with KELT (DESK) Survey." Proceedings of the International Astronomical Union 10, S314 (2015): 167–70. http://dx.doi.org/10.1017/s1743921315005931.

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AbstractUsing time-series photometry from the Kilodegree Extremely Little Telescope (KELT) exoplanet survey, we are looking for eclipses of stars by their protoplanetary disks, specifically in young stellar associations. To date, we have discovered two previously unknown, large dimming events around the young stars RW Aurigae and V409 Tau. We attribute the dimming of RW Aurigae to an occultation by its tidally disrupted disk, with the disruption perhaps resulting from a recent flyby of its binary companion. Even with the dynamical environment of RW Aurigae, the distorted disk material remains

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20

Hilditch, R. W., A. C. Cameron, G. Hill, S. A. Bell, and T. J. Harries. "Spectroscopy and eclipse-mapping of the mass-exchanging binary star V361 Lyr." Monthly Notices of the Royal Astronomical Society 291, no. 4 (1997): 749–62. http://dx.doi.org/10.1093/mnras/291.4.749.

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21

Reed, M. D., B. J. Brondel, and S. D. Kawaler. "Pulsating Stars in Close Binaries. I. Investigations of Eclipse Mapping and Oblique Pulsations." Astrophysical Journal 634, no. 1 (2005): 602–15. http://dx.doi.org/10.1086/491666.

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22

Gies, D. R. "O and B-star surface mapping." Symposium - International Astronomical Union 176 (1996): 121–28. http://dx.doi.org/10.1017/s0074180900083157.

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The massive O and B-type stars will be among the first targets of the new generation of long baseline optical interferometers (such as the CHARA Array, a 400-m diameter distributed array of five 1-m telescopes). Many of these objects are binary stars for which joint astrometric and spectroscopic observations will provide masses and distances (e.g., 15 Mon; Gies et al. 1993), but there is also great interest in resolving disks of single stars. Early interferometric observations have already resolved the flattened circumstellar disks around some Be stars (Quirrenbach et al. 1994).

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23

Krzesinski, J., A. Blokesz, M. Siwak, and G. Stachowski. "The quest for planets around subdwarfs and white dwarfs from Kepler space telescope fields." Astronomy & Astrophysics 642 (October 2020): A105. http://dx.doi.org/10.1051/0004-6361/202038121.

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Context. In this study, we independently test the presence of an exoplanet around the binary KIC 9472174, which is composed of a red dwarf and a pulsating type B subdwarf. We also present the results of our search for Jupiter-mass objects orbiting near to the eclipsing binary KIC 7975824, which is composed of a white dwarf and type B subdwarf, and the pulsating white dwarf KIC 8626021. Aims. The goal is to test analytical techniques and prepare the ground for a larger search for possible substellar survivors on tight orbits around post-common envelope binaries and stars at the end of their evo

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24

Pan, Tony, and Abraham Loeb. "Identifying stars of mass >150 M⊙ from their eclipse by a binary companion." Monthly Notices of the Royal Astronomical Society: Letters 425, no. 1 (2012): L91—L95. http://dx.doi.org/10.1111/j.1745-3933.2012.01308.x.

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25

Jorissen, A., J. Manfroid, and C. Sterken. "HD 46407: The First Eclipsing-Binary Barium Star." Symposium - International Astronomical Union 151 (1992): 411–14. http://dx.doi.org/10.1017/s0074180900122600.

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A long-term, high-accuracy, differential uvby monitoring of a sample of 19 barium stars revealed that HD 46407, a well known barium star with an orbital period of 458 d, is an eclipsing binary. The eclipse (of the companion by the barium star) was most clearly seen in November 1988, when a dip of 0.02 mag (in y) having a FWHM of about 10 d was recorded in the lightcurve. Confirmation of the eclipsing nature of HD 46407 was also obtained in February 1985 and in February 1990. A shallow secondary eclipse (extending over about 50% of the orbital period) seems to be present as well. The b – y inde

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Zhu, L. Y., S. B. Qian, E. G. Zhao, E. Fernández Lajús, and Z. T. Han. "Close-In Substellar Companions and the Formation of sdB-Type Close Binary Stars." Acta Polytechnica CTU Proceedings 2, no. 1 (2015): 183–87. http://dx.doi.org/10.14311/app.2015.02.0183.

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The sdB-type close binaries are believed to have experienced a common-envelope phase and may evolve into cataclysmic binaries (CVs). About 10% of all known sdB binaries are eclipsing binaries consisting of very hot subdwarf primaries and low-mass companions with short orbital periods. The eclipse profiles of these systems are very narrow and deep, which benefits the determination of high precise eclipsing times and makes the detection of small and close-in tertiary bodies possible. Since 2006 we have monitored some sdB-type eclipsing binaries to search for the close-in substellar companions by

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27

Li, M. C. A., N. J. Rattenbury, I. A. Bond, et al. "The first eclipsing binary catalogue from the MOA-II data base." Monthly Notices of the Royal Astronomical Society 470, no. 1 (2017): 539–50. http://dx.doi.org/10.1093/mnras/stx1280.

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Abstract We present the first catalogue of eclipsing binaries in two MOA (Microlensing Observations in Astrophysics) fields towards the Galactic bulge, in which over 8000 candidates, mostly contact and semidetached binaries of periods &lt;1 d, were identified. In this paper, the light curves of a small number of interesting candidates, including eccentric binaries, binaries with noteworthy phase modulations and eclipsing RS Canum Venaticorum type stars, are shown as examples. In addition, we identified three triple object candidates by detecting the light-travel-time effect in their eclips

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Kochukhov, O., C. Johnston, J. Labadie-Bartz, et al. "V772 Cas: an ellipsoidal HgMn star in an eclipsing binary." Monthly Notices of the Royal Astronomical Society 500, no. 2 (2020): 2577–89. http://dx.doi.org/10.1093/mnras/staa3472.

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ABSTRACT The late B-type star V772 Cas (HD 10260) was previously suspected to be a rare example of a magnetic chemically peculiar star in an eclipsing binary system. Photometric observations of this star obtained by the TESS satellite show clear eclipses with a period of 5.0137 d accompanied by a significant out-of-eclipse variation with the same period. High-resolution spectroscopy reveals V772 Cas to be an SB1 system, with the primary component rotating about a factor two slower than the orbital period and showing chemical peculiarities typical of non-magnetic HgMn chemically peculiar stars.

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29

Swayne, Matthew I., Pierre F. L. Maxted, Vedad Kunovac Hodžić, and Amaury H. M. J. Triaud. "The TESS light curve of the eccentric eclipsing binary 1SWASP J011351.29+314909.7 – no evidence for a very hot M-dwarf companion." Monthly Notices of the Royal Astronomical Society: Letters 498, no. 1 (2020): L15—L19. http://dx.doi.org/10.1093/mnrasl/slaa122.

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ABSTRACT A 2014 study of the eclipsing binary star 1SWASPJ011351.29+314909.7 (J0113+31) reported an unexpectedly high effective temperature for the M-dwarf companion to the 0.95-M⊙ primary star. The effective temperature inferred from the secondary eclipse depth was ∼600 K higher than the value predicted from stellar models. Such an anomalous result questions our understanding of low-mass stars and might indicate a significant uncertainty when inferring properties of exoplanets orbiting them. We seek to measure the effective temperature of the M-dwarf companion using the light curve of J0113+3

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30

Reed, Phillip A. "The Effects of Eccentric Accretion Structures on the Light Curves of Interacting Algol-type Binary Stars." Proceedings of the International Astronomical Union 7, S282 (2011): 325–26. http://dx.doi.org/10.1017/s1743921311027736.

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AbstractThe light curves of many Algol-type binary stars are complicated with strange variations. Secular variations are due to the transient nature of the accretion structure, while the phase-dependent features, such as outside-of-eclipse dips, are likely geometrical effects of the accretion structure eclipsing the primary star. Presented here is a model of the ultraviolet light curve of R Arae that explains these variations through the combination of an eccentric accretion structure and the system's orbital inclination.The orbital period of R Ara is 4.4 days, which is too long to allow for d

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31

Wang, Jiaxin, Jianning Fu, Hubiao Niu, et al. "KIC 5359678: a detached eclipsing binary with starspots." Monthly Notices of the Royal Astronomical Society 504, no. 3 (2021): 4302–11. http://dx.doi.org/10.1093/mnras/stab1219.

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ABSTRACT We study the detached eclipsing binary, KIC 5359678, with starspot modulation using the high-quality Kepler photometry and LAMOST spectroscopy. The phoebe model, optimal for this binary, reveals that this system is a circular detached binary, composed of two F-type main-sequence stars. The masses and radii of the primary and the secondary are M1 = 1.31 ± 0.05 M⊙, R1 = 1.52 ± 0.04 R⊙, M2 = 1.12 ± 0.04 M⊙, and R2 = 1.05 ± 0.06 R⊙, respectively. The age of this binary is estimated to be about 2 Gyr, a value much longer than the synchronization time-scale of 17.8 Myr. The residuals of lig

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32

Garcia, Michael R., and Scott J. Kenyon. "Orbital Radial Velocity Curves of Symbiotic Stars." International Astronomical Union Colloquium 103 (1988): 27–32. http://dx.doi.org/10.1017/s0252921100103094.

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AbstractFor the past 6 years we have been measuring the radial velocity of the M-giant component of Symbiotics Stars with high dispersion echelle spectrographs. Because these velocities are based on the absorption line spectrum of the M-star, very reliable orbital radial velocity curves can be constructed. The orbital solutions derived from these velocity curves allow the approximate size of the binary to be determined, and also provide insight into the origin of the photometric variations seen in these stars. For most of the stars, the photometric variations are due to eclipse or reflection e

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Mitnyan, T., T. Borkovits, S. A. Rappaport, A. Pál, and P. F. L. Maxted. "TIC 278825952: a triply eclipsing hierarchical triple system with the most intrinsically circular outer orbit." Monthly Notices of the Royal Astronomical Society 498, no. 4 (2020): 6034–43. http://dx.doi.org/10.1093/mnras/staa2762.

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ABSTRACT We report the discovery of a compact triply eclipsing triple star system in the southern continuous viewing zone of the TESS space telescope. TIC 278825952 is a previously known, but unstudied circular eclipsing binary with a period of 4.781 d with a tertiary component in a wider, circular orbit of 235.55-d period that was found from three sets of third-body eclipses and from light travel-time effect dominated eclipse timing variations. We performed a joint photodynamical analysis of the eclipse timing variation curves, photometric data, and the spectral energy distribution, coupled w

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Borkovits, T., S. A. Rappaport, P. F. L. Maxted, et al. "BG Ind: the nearest doubly eclipsing, compact hierarchical quadruple system." Monthly Notices of the Royal Astronomical Society 503, no. 3 (2021): 3759–74. http://dx.doi.org/10.1093/mnras/stab621.

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ABSTRACT BG Ind is a well-studied, bright, nearby binary consisting of a pair of F stars in a 1.46-d orbit. We have discovered in the TESS light curve for TIC 229804573 (aka BG Ind), a second eclipsing binary in the system with a 0.53-d period. Our subsequent analyses of the recent TESS and archival ground-based photometric and radial velocity (RV) data reveal that the two binaries are gravitationally bound in a 721-d period, moderately eccentric orbit. We present the results of a joint spectro-photodynamical analysis of the eclipse timing variation curves of both binaries based on TESS and gr

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Kim, C. H., J. M. Kreiner, B. Zakrzewski, W. Ogłoza, H. W. Kim, and M. J. Jeong. "A Comprehensive Catalog of Galactic Eclipsing Binary Stars with Eccentric Orbits Based on Eclipse Timing Diagrams." Astrophysical Journal Supplement Series 235, no. 2 (2018): 41. http://dx.doi.org/10.3847/1538-4365/aab7ef.

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IJspeert, L. W., A. Tkachenko, C. Johnston, et al. "An all-sky sample of intermediate- to high-mass OBA-type eclipsing binaries observed by TESS." Astronomy & Astrophysics 652 (August 2021): A120. http://dx.doi.org/10.1051/0004-6361/202141489.

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Context. Intermediate- to high-mass stars are the least numerous types of stars, and they are less well understood than their more numerous low-mass counterparts in terms of their internal physical processes. Modelling the photometric variability of a large sample of main-sequence intermediate- to high-mass stars in eclipsing binary systems will help to improve the models for such stars. Aims. Our goal is to compose a homogeneously compiled sample of main-sequence intermediate- to high-mass OBA-type dwarfs in eclipsing binary systems from TESS photometry. We search for binaries with and withou

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Kochukhov, O., J. Labadie-Bartz, V. Khalack, and M. E. Shultz. "New eclipsing binaries with mercury–manganese stars." Monthly Notices of the Royal Astronomical Society: Letters 506, no. 1 (2021): L40—L44. http://dx.doi.org/10.1093/mnrasl/slab066.

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ABSTRACT Eclipsing binary stars are rare and extremely valuable astrophysical laboratories that make possible precise determination of fundamental stellar parameters. Investigation of early-type chemically peculiar stars in eclipsing binaries provides important information for understanding the origin and evolutionary context of their anomalous surface chemistry. In this study, we discuss observations of eclipse variability in six mercury–manganese (HgMn) stars monitored by the Transiting Exoplanet Survey Satellite (TESS) satellite. These discoveries double the number of known eclipsing HgMn s

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Bennett, Philip D., Graham M. Harper, Alexander Brown, and Jeffrey L. Linsky. "NLTE Radiative Transfer in the Extended Atmospheres and Winds of Cool Stars." Symposium - International Astronomical Union 210 (2003): 93–105. http://dx.doi.org/10.1017/s0074180900133285.

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The mechanism responsible for driving the ubiquitous winds of cool giant and supergiant stars remains to be established. To this end, we are constructing semi-empirical models of the extended outer atmospheres (‘chromospheres’) and winds of selected red supergiants. These models are constrained by analyses of the UV line spectra of single stars, and of red supergiants in binaries that eclipse their main-sequence companions: the ζ Aur and VV Cep stars. These detached binaries are well-separated, with no evidence of mass transfer. The C II] 2325 Å line profiles of the binaries are similar to tho

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Iglesias-Marzoa, Ramón, María J. Arévalo, Mercedes López-Morales, Guillermo Torres, Carlos Lázaro, and Jeffrey L. Coughlin. "Absolute dimensions of the low-mass eclipsing binary system NSVS 10653195." Astronomy & Astrophysics 627 (July 2019): A153. http://dx.doi.org/10.1051/0004-6361/201935516.

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Context. Low-mass stars in eclipsing binary systems show radii larger and effective temperatures lower than theoretical stellar models predict for isolated stars with the same masses. Eclipsing binaries with low-mass components are hard to find due to their low luminosity. As a consequence, the analysis of the known low-mass eclipsing systems is key to understand this behavior. Aims. We aim to investigate the mass–radius relation for low-mass stars and the cause of the deviation of the observed radii in low-mass detached eclipsing binary stars (LMDEB) from theoretical stellar models. Methods.

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Hartman, N., R. S. Polidan, A. D. Welty, R. Wade, P. B. Etzel, and F. C. Bruhweiler. "The Unusual Short Period Binary V342 Aquilae; Does it Break the Evolutionary Theory Mold?" Highlights of Astronomy 11, no. 1 (1998): 372. http://dx.doi.org/10.1017/s1539299600021225.

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Analysis of the eclipsing (period=3.39 days) binary V342 Aquilae at visible wavelengths reveals that the system is heavily enshrouded with gas, masking the identity of the underlying stars. In the ultraviolet V342 Aquilae shows six times more attenuation at phases outside of eclipse than most Algols. It is likely, then, that V342 Aquilae is the most enshrouded short period Algol system known. Our ultraviolet spectra show very pronounced Fe II absorption lines arising from ground and metastable levels, indicating an extensive circumstellar gas envelope. The strength of this absorption shows bot

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Linnell, Albert P. "W Ursae Majoris Star Models: Observational Constraints." International Astronomical Union Colloquium 108 (1988): 213–14. http://dx.doi.org/10.1017/s0252921100093842.

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W Ursae Majoris stars can be understood as contact binary stars with a common envelope (Lucy 1968). They subdivide into two types: The A-type are earlier inspectral class than about F5, are believed to have radiative envelopes, and associate primary (deeper) eclipse minimum with transit eclipse. The W-type have spectral classes later than F5, are believed to have convectlve envelopes, and associate primary minimum with occultation eclipse. Controversy has surrounded the explanation of W-type light curves.Four distinct models have been introduced to describe the envelopes or photospheres of W U

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Saito, R. K., and R. Baptista. "Spectral mapping of V348 Puppis: spiral arms in the period gap★." Monthly Notices of the Royal Astronomical Society 457, no. 1 (2016): 198–211. http://dx.doi.org/10.1093/mnras/stv3007.

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Abstract We report the analysis of Hubble Space Telescope (HST) UV–optical spectroscopy of the nova-like variable V348 Puppis with eclipse mapping techniques. We measured the eclipse width at disc centre and determined a lower limit on the mass ratio of q &gt; 0.3, with a tight relation between q and the binary inclination i. For 0.31 ≤ q ≤ 0.6, we have 79$_{.}^{\circ}$5 ≤ i ≤ 88$_{.}^{\circ}$2. Simulations with 3D eclipse mapping give no support to the suggestion of self-shielding of the accretion disc of V348 Pup, indicating a geometrically thin disc. Eclipse maps reveal two structures i

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Neff, James E. "Chromospheric emission line mapping." Symposium - International Astronomical Union 176 (1996): 113–20. http://dx.doi.org/10.1017/s0074180900083145.

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Throughout its eighteen years of operation, the International Ultraviolet Explorer has afforded us the opportunity to make many new discoveries regarding the nature of the outer atmospheres of magnetically active, late-type stars. High-resolution spectra obtained continuously throughout the rotational cycle of rapidly-rotating stars have been used to map the spatial structure of the magnetic active regions in stellar chromospheres. The RS CVn-type binary system AR Lacertae has been observed intensively at 3 epochs, with additional observations with less complete phase coverage was obtained at

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McLaughlin, Kenneth W., and Janak Panthi. "Synchronous Rotation in the Eclipsing Binary 68 Herculis Inferred from Doppler Shifts in its Spectrum and Light Curve Modeling." Journal of the Iowa Academy of Science 121, no. 1-4 (2014): 5–15. http://dx.doi.org/10.17833/121-02.1.

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Our differential photometry of the eclipsing binary 68 Herculis through V- and R-filters shows periodic minima consistent with a previously established period. As a function of its orbital motion, we report spectra over a limited wavelength range encompassing H-alpha 656.3 nm and helium 667.8 nm lines. Doppler shifts of both stars were resolved in H-alpha, while only the more massive star rendered the helium line with Doppler shifts that agree with the radial velocity we derive for it from the H-alpha profile. Sinusoidal curve-fits to the orbital dependence of the radial velocities imply circu

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Conroy, Kyle E., Andrej Prša, Keivan G. Stassun, Jerome A. Orosz, Daniel C. Fabrycky, and William F. Welsh. "KEPLERECLIPSING BINARY STARS. IV. PRECISE ECLIPSE TIMES FOR CLOSE BINARIES AND IDENTIFICATION OF CANDIDATE THREE-BODY SYSTEMS." Astronomical Journal 147, no. 2 (2014): 45. http://dx.doi.org/10.1088/0004-6256/147/2/45.

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Borkovits, T., S. A. Rappaport, T. G. Tan, et al. "The compact triply eclipsing triple star TIC 209409435 discovered with TESS." Monthly Notices of the Royal Astronomical Society 496, no. 4 (2020): 4624–36. http://dx.doi.org/10.1093/mnras/staa1817.

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ABSTRACT We report the discovery in TESS Sectors 3 and 4 of a compact triply eclipsing triple star system. TIC 209409435 is a previously unknown eclipsing binary with a period of 5.717 d, and the presence of a third star in an outer eccentric orbit of 121.872-d period was found from two sets of third-body eclipses and from eclipse timing variations. The latter exhibits signatures of strong third-body perturbations. After the discovery, we obtained follow-up ground-based photometric observations of several binary eclipses as well as another of the third-body eclipses. We carried out comprehensi

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Getley, A. K., B. Carter, R. King, and S. O’Toole. "Stability of planetary, single M dwarf, and binary star companions to Kepler detached eclipsing binaries and a possible five-body system." Monthly Notices of the Royal Astronomical Society 498, no. 3 (2020): 4356–64. http://dx.doi.org/10.1093/mnras/staa2532.

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ABSTRACT In this study, we identify 11 Kepler systems (KIC 5255552, 5653126, 5731312, 7670617, 7821010, 8023317, 10268809, 10296163, 11519226, 11558882, and 12356914) with a flip-flop effect in the eclipse timing variations O − C diagrams of the systems, report on what these systems have in common and whether these systems are dynamically stable. These systems have previously reported high eccentric binary stars with highly eccentric third bodies/outer companions. We find that all of the additional bodies in the system are dynamically stable for the configurations previously reported and are t

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Carmo, A., C. E. Ferreira Lopes, A. Papageorgiou, et al. "Recovering variable stars in large surveys: EAup Algol-type class in the Catalina Survey." Monthly Notices of the Royal Astronomical Society 498, no. 2 (2020): 2833–44. http://dx.doi.org/10.1093/mnras/staa2518.

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ABSTRACT The discovery and characterization of Algol eclipsing binaries (EAs) provide an opportunity to contribute for a better picture of the structure and evolution of low-mass stars. However, the cadence of most current photometric surveys hinders the detection of EAs since the separation between observations is usually larger than the eclipse(s) duration and hence few measurements are found at the eclipses. Even when those objects are detected as variable, their periods can be missed if an appropriate oversampling factor is not used in the search tools. In this paper, we apply this approac

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Mimica, P., and K. Pavlovski. "Reconstruction of an Accretion Disk Image in AU Mon from CoRoT Photometry." Proceedings of the International Astronomical Union 7, S282 (2011): 63–64. http://dx.doi.org/10.1017/s1743921311026901.

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AbstractThe long-period binary system AU Mon was photometrically observed on-board the CoRoT satellite in a continuous run of almost 60 days long which has covered almost 5 complete cycles. Unprecedented sub milimag precision of CoRoT photometry reveals all complexity of its light variations in this, still active mass-transfer binary system. We present images of an accretion disk reconstructed by eclipse mapping, and an optimization of intensity distribution along disk surface. Time resolution and accurate CoRoT photometric measurements allow precise location of spatial distribution of ‘hot’ s

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Valio, Adriana. "Study of stellar activity through transit mapping of starspots." Proceedings of the International Astronomical Union 6, S273 (2010): 96–103. http://dx.doi.org/10.1017/s1743921311015079.

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AbstractDuring the eclipse of a planet, spots and other features on the surface of the host star may be occulted. This will cause small variations in the light curve of the star. Detailed studies of these variations during planetary transits provide a wealth of information about the starspots properties such as size, position, temperature (i.e. intensity), and magnetic field. If observation of multiple transits is available, the spots lifetime can be estimated. Moreover it may also be possible to determine the stellar rotation and whether differential rotation is present. Here, the study is pe

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