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Relevant bibliographies by topics / Large magellanic cloud; Galaxy; Binary stars

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Journal articles

Academic literature on the topic 'Large magellanic cloud; Galaxy; Binary stars'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

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Journal articles on the topic "Large magellanic cloud; Galaxy; Binary stars"

1

Gładkowski, Marcin, Marcin Hajduk, and Igor Soszyński. "Search for binary central stars of the Magellanic Clouds PNe." Proceedings of the International Astronomical Union 12, S323 (2016): 384–85. http://dx.doi.org/10.1017/s1743921317001892.

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AbstractThe Optical Gravitational Experiment (OGLE) was effectively used in discovering binary central stars of planetary nebulae (CSPNe). About 50 binary CSPNe have been hitherto identified in the Galaxy, almost half of them were detected in the OGLE database. We used the OGLE data to search for binary CSPNe in the Magellanic Clouds. We also searched for PNe mimics and removed them from the PNe sample. Here, we present results of the photometric analysis for Small Magellanic Cloud (SMC) and our progress on search of binary central stars in the Large Magellanic Cloud (LMC). So far, we have dis

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Mahy, L., L. A. Almeida, H. Sana, et al. "The Tarantula Massive Binary Monitoring." Astronomy & Astrophysics 634 (February 2020): A119. http://dx.doi.org/10.1051/0004-6361/201936152.

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Context. A high fraction of massive stars are found to be binaries but only a few of them are reported as photometrically variable. By studying the populations of double-lined spectroscopic binaries in the 30 Doradus region, we found a subset of them that have photometry from the OGLE project and that display variations in their light curves related to orbital motions. Aims. The goal of this study is to determine the dynamical masses and radii of the 26 binary components in order to investigate the mass-discrepancy problem and to provide an empirical mass-luminosity relation for the Large Mage

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Shenar, T., A. Gilkis, J. S. Vink, H. Sana, and A. A. C. Sander. "Why binary interaction does not necessarily dominate the formation of Wolf-Rayet stars at low metallicity." Astronomy & Astrophysics 634 (February 2020): A79. http://dx.doi.org/10.1051/0004-6361/201936948.

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Context. Classical Wolf-Rayet (WR) stars are massive, hydrogen-depleted, post main-sequence stars that exhibit emission-line dominated spectra. For a given metallicity Z, stars exceeding a certain initial mass MsingleWR(Z) can reach the WR phase through intrinsic mass-loss or eruptions (single-star channel). In principle, stars of lower masses can reach the WR phase via stripping through binary interactions (binary channel). Because winds become weaker at low Z, it is commonly assumed that the binary channel dominates the formation of WR stars in environments with low metallicity such as the S

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Hamann, Wolf-Rainer, Lidia Oskinova, Helge Todt, et al. "Massive stars in advanced evolutionary stages, and the progenitor of GW150914." Proceedings of the International Astronomical Union 12, S329 (2016): 223–27. http://dx.doi.org/10.1017/s1743921317002563.

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AbstractThe recent discovery of a gravitational wave from the merging of two black holes of about 30 solar masses each challenges our incomplete understanding of massive stars and their evolution. Critical ingredients comprise mass-loss, rotation, magnetic fields, internal mixing, and mass transfer in close binary systems. The imperfect knowledge of these factors implies large uncertainties for models of stellar populations and their feedback. In this contribution we summarize our empirical studies of Wolf-Rayet populations at different metallicities by means of modern non-LTE stellar atmosphe

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Irrgang, A., S. Kreuzer, and U. Heber. "Hypervelocity stars in the Gaia era." Astronomy & Astrophysics 620 (December 2018): A48. http://dx.doi.org/10.1051/0004-6361/201833874.

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Context. Young massive stars in the halo are assumed to be runaway stars from the Galactic disk. Possible ejection scenarios are binary supernova ejections (BSE) or dynamical ejections from star clusters (DE). Hypervelocity stars (HVSs) are extreme runaway stars that are potentially unbound from the Galaxy. Powerful acceleration mechanisms such as the tidal disruption of a binary system by a supermassive black hole (SMBH) are required to produce them. Therefore, HVSs are believed to originate in the Galactic center (GC), the only place known to host an SMBH. Aims. The second Gaia data release

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Villaseñor, J. I., W. D. Taylor, C. J. Evans, et al. "The B-type binaries characterization programme I. Orbital solutions for the 30 Doradus population." Monthly Notices of the Royal Astronomical Society 507, no. 4 (2021): 5348–75. http://dx.doi.org/10.1093/mnras/stab2197.

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ABSTRACT We present results from the B-type binaries characterization (BBC) programme, a multi-epoch spectroscopic study of 88 early B-type binary candidates in the 30 Doradus region of the Large Magellanic Cloud (LMC). From radial-velocity analysis of 29 observational epochs, we confirm the binary status of 64 of our targets, comprising 50 SB1 and 14 SB2 B-type binaries. A further 20 systems (classified as SB1*) show clear signs of periodicity but with more tentative periods. Orbital solutions are presented for these 84 systems, providing the largest homogeneous sample to date of the binary p

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Juryšek, J., P. Zasche, M. Wolf, et al. "New inclination changing eclipsing binaries in the Magellanic Clouds." Astronomy & Astrophysics 609 (January 2018): A46. http://dx.doi.org/10.1051/0004-6361/201730655.

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Context. Multiple stellar systems are unique laboratories for astrophysics. Analysis of their orbital dynamics, if well characterized from their observations, may reveal invaluable information about the physical properties of the participating stars. Unfortunately, there are only a few known and well described multiple systems, this is even more so for systems located outside the Milky Way galaxy. A particularly interesting situation occurs when the inner binary in a compact triple system is eclipsing. This is because the stellar interaction, typically resulting in precession of orbital planes

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Vink, Jorick S. "Constraining the progenitor evolution of GW 150914." Proceedings of the International Astronomical Union 14, S346 (2018): 444–48. http://dx.doi.org/10.1017/s1743921318007731.

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AbstractOne of the largest surprises from the LIGO results regarding the first gravitational wave detection (GW 150914) was the fact the black holes (BHs) were “heavy”, of order 30 - 40 Mȯ. The most promising explanation for this obesity is that the BH-BH merger occurred at low metallicity (Z): when the iron (Fe) contents is lower this is expected to result in weaker mass loss during the Wolf-Rayet (WR) phase. We therefore critically evaluate the claims for the reasons of heavy BHs as a function of Z in the literature. Furthermore, weaker stellar winds might lead to more rapid stellar rotation

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Kołaczkowski, Z., A. Pigulski, I. Soszyński та ін. "β Cephei and SPB stars in the Large Magellanic Cloud". International Astronomical Union Colloquium 193 (2004): 225–29. http://dx.doi.org/10.1017/s0252921100010666.

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AbstractThis is a progress report of the study of pulsating main-sequence stars in the LMC. Using the OGLE-II photometry supplemented by the MACHO photometry, we find 64 β Cephei stars in the LMC. Their periods are generally much longer than observed in stars of this type in the Galaxy (the median value is 0.27 d compared with 0.17 d in the Galaxy). In 20 stars with short periods attributable to the β Cephei-type instability, we also find modes with periods longer than ~0.4d. They are likely low-order g modes, which means that in these stars both kinds of variability, β Cephei and SPB, are obs

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Hatzidimitriou, D., and R. K. Bhatia. "Do Binary Clusters Exist in the Large Magellanic Cloud?" Symposium - International Astronomical Union 126 (1988): 567–68. http://dx.doi.org/10.1017/s0074180900043102.

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The possible existence of binary clusters in our Galaxy (h and x Persei, Ocl 556) has been argued in the past, but it has never been a well established fact either in our Galaxy, or in external systems. An early speculation on the problem by Innanen et al (1972) has predicted a considerable degree of stability for binary clusters in low nuclear density galaxies, like the LMC.

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