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

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

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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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8

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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9

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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11

Niemela, Virpi S. "Two New Massive Binary Stars in the Magellanic Clouds." Symposium - International Astronomical Union 207 (2002): 202–4. http://dx.doi.org/10.1017/s0074180900223759.

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The discovery and preliminary spectroscopic orbits of two early O type binaries in very young open clusters in the Magellanic Clouds is reported. The binaries are NGC 346–1 in the Small Magellanic Cloud, and HDE 270145 in NGC 2122 in the Large Magellanic Cloud.

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Shore, Steven N. "GHRS Observations of Massive Stars in the Large Magellanic Cloud." Highlights of Astronomy 9 (1992): 475–76. http://dx.doi.org/10.1017/s1539299600009588.

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Hot stars are the natural targets for ultraviolet space observations. The bulk of their energy emerges shortward of the atmospheric cutoff and nearly all of the important atomic transitions required for their analysis are located in the region shortward of λ3000Å. However, since they are intrinsically rare, reddening and distance conspire to make the job of studying these important members of the stellar population of a galaxy a very difficulty task. The Goddard High Resolution Spectrograph (GHRS) adds the new dimension of photon counting to high sensitivity and resolution. This means that the

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13

Feitzinger, J. V. "Star Formation in the Large Magellanic Cloud." Symposium - International Astronomical Union 115 (1987): 521–33. http://dx.doi.org/10.1017/s0074180900096315.

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Methods used in pattern recognition and cluster analysis are applied to investigate the spatial distribution of the star forming regions. The fractal dimension of these structures is deduced. The new 21 cm, radio continuum (1.4 GHz) and IRAS surveys reveal scale structures of 700 pc to 1500 pc being identical with the optically identified star forming sites. The morphological structures delineated by young stars reflect physical parameters which determine the star formation in this galaxy. The formation of spiral arm filaments is understandable by stochastic selfpropagating star formation proc

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Popowski, Piotr. "The Distance to the Large Magellanic Cloud." International Astronomical Union Colloquium 176 (2000): 203–7. http://dx.doi.org/10.1017/s0252921100057547.

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AbstractI demonstrate that the two unexpected results in the local Universe: anomalous intrinsic (V – I)0 colors of RR Lyrae stars and clump giants in the Galactic center, and very short distances to Magellanic Clouds inferred from clump giants, can be at least partially resolved with a modified coefficient of selective extinction AV/E(V – I). With this modification, I find a new clump-giant distance modulus to the Large Magellanic Cloud, μLMC = 18.27 ± 0.07, which is 0.09 larger than the Udalski (1998b) result. When distance estimates from the red clump, RR Lyrae stars and the eclipsing binar

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Bohannan, Bruce. "A Large Sample of Emission-Line Stars in the Large Magellanic Cloud: Their Location in the Hertzsprung-Russell Diagram." Symposium - International Astronomical Union 116 (1986): 227–28. http://dx.doi.org/10.1017/s0074180900148922.

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The paths that massive stars follow in their evolution can potentially be determined by studying a homogeneous collection of luminous stars. In this investigation, mass-losing stars in a galaxy are studied through a sample of 59 H alpha emission-line stars in the Large Magellanic Cloud (LMC). The most luminous, most massive stars in the LMC, like their counterparts in the Galaxy, are losing mass at a rate that significantly alters their spectroscopic appearance and that affects their evolution.

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Feast, M. W., and P. A. Whitelock. "CH stars in the Large Magellanic Cloud and in our Galaxy." Monthly Notices of the Royal Astronomical Society 259, no. 1 (1992): 6–16. http://dx.doi.org/10.1093/mnras/259.1.6.

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17

Minelli, Alice, and Alessio Mucciarelli. "Chemical and kinematic study of Large Magellanic Cloud RGB stars." Proceedings of the International Astronomical Union 14, S351 (2019): 126–30. http://dx.doi.org/10.1017/s1743921319007178.

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AbstractThe Large Magellanic Cloud (LMC) is the closest massive satellite of the Milky Way (MW), and its proximity allows us to study its stellar populations with great detail, both with resolved photometry and spectroscopy. In turn, this is crucial to unveil its star formation and chemical enrichment histories, and also to investigate the effects that gravitational interactions with other systems (as the Small Magellanic Cloud (SMC) and the MW) may induce on an irregular galaxy. The LMC is characterized by a still on-going star formation activity, as traced by the wide range of ages and metal

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Fujimoto, M., T. Sawa, and Y. Kumai. "The Magellanic Stream and the Magellanic Cloud System." Symposium - International Astronomical Union 186 (1999): 31–38. http://dx.doi.org/10.1017/s0074180900112161.

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A tidal model has been introduced to the triple system of the Galaxy, Large and Small Magellanic Clouds (the LMC and SMC hereafter) and successfully reproduced the Magellanic Stream (Murai and Fujimoto 1980; Lin and Lynden-Bell 1982; Gardiner et al. 1994; Gardiner and Noguchi 1995; Lin et al. 1995), a narrow band of diffuse atomic hydrogen gas emerging from the SMC region, passing by the South Galactic Pole along an overhead great circle spanning over 100° (Wannier and Wrixon 1972; Mathewson et al. 1974). The LMC and SMC have a hydrogen bridge and common envelope (Hindman 1964; McGee and Milto

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Ramamani, N., T. Meinya Singh, and Saleh Mohammed Alladin. "Tidal interactions between the Galaxy and the Magellanic Clouds." Symposium - International Astronomical Union 106 (1985): 477–78. http://dx.doi.org/10.1017/s0074180900242964.

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The merging time and the disruption time in a binary galaxy system are analytically obtained under the Adiabatic Approximation (AA). Applications are made to the Galaxy-LMC (Large Magellanic Cloud) pair.

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Niemela, Virpi S. "Massive Binaries in the Magellanic Clouds." Highlights of Astronomy 13 (2005): 463. http://dx.doi.org/10.1017/s1539299600016270.

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We present results of our ongoing observing program on search and studies of massive stars (O and WR type) in binary systems in our neighbor galaxies, the Magellanic Clouds. Radial velocity orbits are presented for two new binaries, one in the Small Magellanic Cloud and another in the Large Magellanic Cloud, and improved orbits for previously known systems. We compare orbital parameters of selected binaries containing O and WR type components. We also discuss the present status of knowledge for massive binary stars in the Magellanic Clouds and the problems encountered in their orbital studies

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Shenar, T., D. P. Sablowski, R. Hainich, et al. "The Wolf–Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud." Astronomy & Astrophysics 627 (July 2019): A151. http://dx.doi.org/10.1051/0004-6361/201935684.

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Context. Massive Wolf–Rayet (WR) stars dominate the radiative and mechanical energy budget of galaxies and probe a critical phase in the evolution of massive stars prior to core collapse. It is not known whether core He-burning WR stars (classical WR; cWR) form predominantly through wind stripping (w-WR) or binary stripping (b-WR). Whereas spectroscopy of WR binaries has so-far largely been avoided because of its complexity, our study focuses on the 44 WR binaries and binary candidates of the Large Magellanic Cloud (LMC; metallicity Z ≈ 0.5 Z⊙), which were identified on the basis of radial vel

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Schmidt, Thomas, Maria-Rosa L. Cioni, Florian Niederhofer, et al. "Proper motion of the Magellanic Bridge: Removal of foreground stars." Proceedings of the International Astronomical Union 14, S353 (2019): 128–29. http://dx.doi.org/10.1017/s1743921319008135.

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AbstractThe Large and Small Magellanic Cloud (LMC and SMC) are the most luminous dwarf galaxy satellites of the Milky Way. Thanks to their close proximity (50-60 kpc), they provide one of the best opportunities to study in detail the kinematics of resolved stellar populations in an interacting pair of galaxies. Large photometric surveys like the ongoing Gaia mission and the near-infrared VISTA survey of the Magellanic Cloud system (VMC) will have a significant impact on our insight into the Magellanic system. We have combined the individual strengths of VMC and Gaia DR2 data to improve our und

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Niemela, Virpi S., Roberto Gamen, Nidia I. Morrell, and Sixto Giménez Benítez. "Wolf-Rayet binaries: old friends and new acquaintances." Symposium - International Astronomical Union 193 (1999): 26–37. http://dx.doi.org/10.1017/s0074180900204890.

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Observations of WR stars in binary systems are discussed, emphasizing constraints on our knowledge of the binary frequency of WR stars, and of WR stars as a distinctive class of objects. Radial velocity orbits of newly discovered binaries, e.g., WR 29, a short period WN7+OB binary in our Galaxy, and SMC/AB 7, a massive WN+O7 binary in the Small Magellanic Cloud, are presented. New spectroscopic observations of binary systems with previously known orbits are also reported, showing in the case of WR 21 evidence of change of the orbital elements as derived from different spectral lines. An ellipt

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Smith, Lindsey F. "Wolf-Rayet stars in the Magellanic Clouds." Symposium - International Astronomical Union 148 (1991): 267–72. http://dx.doi.org/10.1017/s0074180900200570.

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The most striking feature of the Wolf-Rayet stars in the Magellanic Clouds is their subtype distribution. The range of WC subtypes found in the Large and Small Cloud agrees with evolutionary model predictions at the corresponding metallicities. It follows that the WR subtype distribution in any external galaxy is a clear indicator of the metallicity in that galaxy.The fluxes in the emission lines of WC stars appear to be consistent within the LMC. This can be used (with some precautions) in the Milky Way and other galaxies to determine reddening, distance and the numbers of WR stars in compact

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Bekki, Kenji. "Triggered star formation in the Magellanic Clouds." Proceedings of the International Astronomical Union 2, S237 (2006): 373–77. http://dx.doi.org/10.1017/s1743921307001755.

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AbstractWe discuss how tidal interaction between the Large Magellanic Cloud (LMC), the Small Magellanic Cloud (SMC), and the Galaxy triggers galaxy-wide star formation in the Clouds for the last ~0.2 Gyr based on our chemodynamical simulations on the Clouds. Our simulations demonstrate that the tidal interaction induces the formation of asymmetric spiral arms with high gas densities and consequently triggers star formation within the arms in the LMC. Star formation rate in the present LMC is significantly enhanced just above the eastern edge of the LMC's stellar bar owing to the tidal interact

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Lozinskaya, Tatiana A. "Interstellar gas around WO stars in the Galaxy and the Magellanic Clouds." Symposium - International Astronomical Union 148 (1991): 438–39. http://dx.doi.org/10.1017/s0074180900201113.

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The four oxygen-sequence WR stars, Sand 1 in the Small Magellanic Cloud (SMC), Sand 2 in the Large Magellanic Cloud (LMC), and WR 102 and WR 142 in the Galaxy represent the latest stage of the evolution of massive stars (Sanduleak 1971, Barlow and Hummer 1982, Moffatet al.1985). We have shown WR 102 to be a stripped CO core of a supermassive star (Dopitaet al.1990), probably seen only several thousand years before a SN explosion. The four stars are characterized by extremely energetic stellar winds –Vw from 4500 to 7400 km/s (Barlow and Hummer 1982, Dopitaet al.1990, Torreset al.1986). Examina

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Niemela, V. S., M. A. Cerruti, N. I. Morrell, and H. G. Luna. "Observations of Two Binary Systems with 04f Type Components." Symposium - International Astronomical Union 151 (1992): 505–8. http://dx.doi.org/10.1017/s0074180900122831.

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We present linear polarization observations of two binary systems with early Of type components, namely Sk-67°105 in the Large Magellanic Cloud, and LSS 3074 in our Galaxy. Both binaries show phase-locked polarization variations, from which we determined orbital inclinations for the systems.

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Graham, J. A. "Old Globular Clusters in the Magellanic Clouds." Symposium - International Astronomical Union 126 (1988): 151–58. http://dx.doi.org/10.1017/s0074180900042455.

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The old globular clusters in the Magellanic Clouds are important links between our understanding of globular clusters in our own galaxy and similar unresolved objects in more distant galaxies. The Cloud clusters spread over a large range in age. Several contain RR Lyrae variable stars. High weight abundance data are needed for individual cluster members as well as deeper color-magnitude diagrams.

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Bartzakos, P., A. F. J. Moffat, and V. S. Niemela. "A spectroscopic search for colliding winds in a complete sample of WC/WO stars in the Magellanic Clouds." Symposium - International Astronomical Union 163 (1995): 406–10. http://dx.doi.org/10.1017/s0074180900202374.

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The Magellanic Clouds provide an ideal laboratory to study the properties of Wolf-Rayet stars. In particular, the 25 WC/WO stars that they contain are nearly all of the same sub-class (21 WC4, one WC5, one WC6 and one WO in the Large Magellanic Cloud; one WO in the Small Magellanic Cloud). This, along with their formation in the same isolated environment, suggests that the wind structure is similar in each star. Thus, a study of other characteristics, such as the effects of binary separation and period on binary wind collisions, can be undertaken with little concern for differing winds. Some 3

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Bekki, Kenji, and Masashi Chiba. "Origin of Structural and Kinematic Properties of the Small Magellanic Cloud." Publications of the Astronomical Society of Australia 26, no. 1 (2009): 37–57. http://dx.doi.org/10.1071/as08020.

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AbstractWe investigate structural, kinematic and chemical properties of stars and gas in the Small Magellanic Cloud (SMC) interacting with the Large Magellanic Cloud (LMC) and the Galaxy based on a series of self-consistent chemodynamical simulations. We adopt a new ‘dwarf spheroidal model’ in which the SMC initially has both old stars with a spherical spatial distribution and an extended Hi gas disk. We mainly investigate the evolution of the SMC for the last ∼3 Gyr, during which the Magellanic Stream (MS) and the Magellanic Bridge (MB) could have formed as a result of the LMC–SMC–Galaxy inte

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Gouliermis, Dimitrios A. "The sub-solar initial mass function in the Large Magellanic Cloud." Proceedings of the International Astronomical Union 4, S256 (2008): 250–55. http://dx.doi.org/10.1017/s1743921308028524.

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AbstractThe Magellanic Clouds offer a unique variety of star forming regions seen as bright nebulae of ionized gas, related to bright young stellar associations. Nowadays, observations with the high resolving efficiency of the Hubble Space Telescope allow the detection of the faintest infant stars, and a more complete picture of clustered star formation in our dwarf neighbors has emerged. I present results from our studies of the Magellanic Clouds, with emphasis in the young low-mass pre-main sequence populations. Our data include imaging with the Advanced Camera for Surveys of the association

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Clementini, G., L. Baldacci, A. Bragaglia, et al. "Distance scale, variable stars and stellar populations in Local Group galaxies." International Astronomical Union Colloquium 193 (2004): 60–64. http://dx.doi.org/10.1017/s0252921100010344.

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AbstractWe present an overview of our study of the short period variable stars in the Large Magellanic Cloud, and in the dwarf galaxies Fornax, Leo I, and NGC 6822. Light curves are presented for RR Lyrae stars, Anomalous Cepheids and, for the first time, for Dwarf Cepheids in the field and in the globular cluster #3 of the Fornax galaxy.

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Schmidt, Thomas, Maria-Rosa Cioni, Florian Niederhofer, Jonathan Diaz, and Gal Matijevic. "VMC proper motions of the Magellanic Bridge." Proceedings of the International Astronomical Union 14, S344 (2018): 130–33. http://dx.doi.org/10.1017/s1743921318006762.

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AbstractDwarf galaxies enable us to study early phases of galaxy evolution and are key to many open questions about the hierarchical structure of the Universe. The Large and Small Magellanic Cloud (LMC and SMC) are the most luminous dwarf galaxy satellites of the Milky Way (MW). They are most likely gravitationally bound to each other, and their last interaction occurred about 200 Myr ago. Also, they are in an early phase of minor merging with the MW and will impact the Galactic structure in the future because of their relatively large mass. However, there are still major uncertainties regardi

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Udalski, Andrzej. "Eclipsing Binaries in the Magellanic Clouds." Highlights of Astronomy 13 (2005): 451. http://dx.doi.org/10.1017/s153929960001618x.

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We present results of a search for eclipsing binaries in the Magellanic Cloud fields covering central parts of these galaxies. The data were collected during the second phase of the Optical Gravitational Lensing Experiment survey (OGLE-II) in 1997-2000. In total, about 1500 and 3000 eclipsing stars were found in the Small and Large Magellanic Cloud, respectively (Udalski et al. 1998, Wyrzykowski et al. 2003). The photometric data of all objects are available to the astronomical community from the OGLE Internet archive (http://sirius.astrouw.edu.pl/~ogle/). OGLE-II data contain a full variety o

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Meixner, Margaret, Jean-Philippe Bernard, Robert D. Blum, et al. "Measuring the lifecycle of baryonic matter in the Large Magellanic Cloud with the Spitzer SAGE-LMC survey." Proceedings of the International Astronomical Union 4, S256 (2008): 3–8. http://dx.doi.org/10.1017/s1743921308028172.

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AbstractThe recycling of matter between the interstellar medium (ISM) and stars are key evolutionary drivers of a galaxy's baryonic matter. The Spitzer wavelengths provide a sensitive probe of circumstellar and interstellar dust and hence, allow us to study the physical processes of the ISM, the formation of new stars and the injection of mass by evolved stars and their relationships on the galaxy-wide scale of the LMC. Due to its proximity, favorable viewing angle, multi-wavelength information, and measured tidal interactions with the Small Magellanic Cloud (SMC), the LMC is uniquely suited f

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Lennon, Daniel J. "Massive star evolution in the Small Magellanic Cloud." Symposium - International Astronomical Union 212 (2003): 308–15. http://dx.doi.org/10.1017/s0074180900212370.

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We discuss abundances for eight early B-type giant/supergiant stars in the SMC cluster NGC 330. All are nitrogen rich with an abundance approximately 1.3 dex higher than an SMC main-sequence field. Given the number of B-type stars with low rotational projected velocities in NGC 330 (all our targets have v sin i < 50 kms–1), we suggest that it is unlikely that the stars in our sample are seen almost pole-on, but rather that they are intrinsically slow rotators. Comparing these results with the predictions of stellar evolution models including the effects of rotationally induced mixing, we co

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Zivkov, Viktor, Joana M. Oliveira, Monika G. Petr-Gotzens, et al. "The VMC survey – XXXVI. Young stellar variability in the Large Magellanic Cloud." Monthly Notices of the Royal Astronomical Society 494, no. 1 (2020): 458–86. http://dx.doi.org/10.1093/mnras/staa626.

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ABSTRACT Studies of young stellar objects (YSOs) in the Galaxy have found that a significant fraction exhibits photometric variability. However, no systematic investigation has been conducted on the variability of extragalactic YSOs. Here we present the first variability study of massive YSOs in an $\sim 1.5\, \mathrm{deg^2}$ region of the Large Magellanic Cloud (LMC). The aim is to investigate whether the different environmental conditions in the metal-poor LMC ($\sim 0.4\!-\!0.5\, \mathrm{Z_{\odot }}$) have an impact on the variability characteristics. Multi-epoch near-infrared (NIR) photome

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Niemela, Virpi S. "Spectroscopic Binaries in the LMC." Symposium - International Astronomical Union 116 (1986): 85–86. http://dx.doi.org/10.1017/s007418090014865x.

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Preliminary results are presented of an observing programme aimed to obtain estimates of the stellar masses from studies of spectroscopic binary systems in the Large Magellanic Cloud. These are the first steps with the final purpose to determine an empirical mass-luminosity relation in a galaxy other than our own.

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Muraveva, T., G. Clementini, C. Maceroni, and M. I. Moretti. "The structure of the Large Magellanic Cloud from hot binary stars and Classical Cepheids." EAS Publications Series 64 (2013): 409–10. http://dx.doi.org/10.1051/eas/1364069.

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Schmidt, Thomas, Maria-Rosa L. Cioni, Florian Niederhofer, et al. "The VMC survey." Astronomy & Astrophysics 641 (September 2020): A134. http://dx.doi.org/10.1051/0004-6361/202037478.

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Context. The Magellanic Clouds are a nearby pair of interacting dwarf galaxies and satellites of the Milky Way. Studying their kinematic properties is essential to understanding their origin and dynamical evolution. They have prominent tidal features and the kinematics of these features can give hints about the formation of tidal dwarfs, galaxy merging and the stripping of gas. In addition they are an example of dwarf galaxies that are in the process of merging with a massive galaxy. Aims. The goal of this study is to investigate the kinematics of the Magellanic Bridge, a tidal feature connect

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Zinn, R., X. Chen, A. C. Layden, and D. I. Casetti-Dinescu. "Local RR Lyrae stars: native and alien." Monthly Notices of the Royal Astronomical Society 492, no. 2 (2019): 2161–76. http://dx.doi.org/10.1093/mnras/stz3580.

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ABSTRACT Measurements of [Fe/H] and radial velocity are presented for 89 RR Lyrae (RRL) candidates within 6 kpc of the Sun. After the removal of two suspected non-RRLs, these stars were added to an existing data base, which yielded 464 RRLs with [Fe/H] on a homogeneous scale. Using data from the Gaia satellite (Data Release 2), we calculated the positions and space velocities for this sample. These data confirm the existence of a thin disc of RRL with [α/Fe] ∼ solar. The majority of the halo RRLs with large total energies have near-zero angular momenta about the Z-axis. Kinematically, these st

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Mastropietro, Chiara. "Modeling a high velocity LMC: The formation of the Magellanic Stream." Proceedings of the International Astronomical Union 4, S256 (2008): 117–21. http://dx.doi.org/10.1017/s1743921308028330.

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AbstractI use high resolution N-body/SPH simulations to model the new proper motion of the Large Magellanic Cloud (LMC) within the Milky Way (MW) halo and investigate the effects of gravitational and hydrodynamical forces on the formation of the Magellanic Stream (MS). Both the LMC and the MW are fully self consistent galaxy models embedded in extended cuspy ΛCDM dark matter halos. I find that ram-pressure from a low density ionized halo is sufficient to remove a large amount of gas from the LMC's disk forming a trailing Stream that extends more than 120 degrees from the Cloud. Tidal forces el

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El Youssoufi, Dalal, Maria-Rosa L. Cioni, Cameron P. M. Bell, et al. "The VMC survey – XXXIV. Morphology of stellar populations in the Magellanic Clouds." Monthly Notices of the Royal Astronomical Society 490, no. 1 (2019): 1076–93. http://dx.doi.org/10.1093/mnras/stz2400.

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ABSTRACT The Magellanic Clouds are nearby dwarf irregular galaxies whose morphologies show different properties when traced by different stellar populations, making them an important laboratory for studying galaxy morphologies. We study the morphology of the Magellanic Clouds using data from the Visible and Infrared Survey Telescope for Astronomy survey of the Magellanic Clouds system. We used about 10 and 2.5 million sources across an area of ∼105 and ∼42 deg2 towards the Large and Small Magellanic Cloud (LMC and SMC), respectively. We estimated median ages of stellar populations occupying di

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Miszalski, Brent, Ralph Napiwotzki, Maria-Rosa L. Cioni, et al. "Planetary nebulae in the VISTA Magellanic Cloud (VMC) Survey." Proceedings of the International Astronomical Union 7, S283 (2011): 444–45. http://dx.doi.org/10.1017/s1743921312011842.

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AbstractThe multi-epoch YJKs sub-arcsecond photometry of the VMC survey provides a long anticipated deep near-infrared (NIR) window into further understanding the stellar populations of the Magellanic Clouds. The first year of observations consisted of six tiles covering ~9% of the Large Magellanic Cloud (LMC) survey region and contains 102 objects previously classified as planetary nebulae (PNe). A large proportion of the sample were found to be contaminated by non-PNe. These initial results underline the importance of establishing a clean catalogue of LMC PNe before they are applied in areas

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Shara, Michael M., Steven M. Crawford, Dany Vanbeveren, Anthony F. J. Moffat, David Zurek, and Lisa Crause. "The spin rates of O stars in WR+O Magellanic Cloud binaries." Monthly Notices of the Royal Astronomical Society 492, no. 3 (2020): 4430–36. http://dx.doi.org/10.1093/mnras/staa038.

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ABSTRACT Some massive, merging black holes (BHs) may be descendants of binary O stars. The evolution and mass transfer between these O stars determine the spins of their progeny BH. These will be measurable with future gravitational wave detectors, incentivizing the measurement of the spins of O stars in binaries. We previously measured the spins of O stars in Galactic Wolf–Rayet (WR)+O binaries. Here we measure the ve sin i of four Large Magellanic Cloud (LMC) and two Small Magellanic Cloud (SMC) O stars in WR+O binaries to determine whether lower metallicity might affect the spin rates. We f

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Condori, C. A. H., M. Borges Fernandes, M. Kraus, D. Panoglou, and C. A. Guerrero. "The study of unclassified B[e] stars and candidates in the Galaxy and Magellanic Clouds†." Monthly Notices of the Royal Astronomical Society 488, no. 1 (2019): 1090–110. http://dx.doi.org/10.1093/mnras/stz1540.

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ABSTRACT We investigated 12 unclassified B[e] stars or candidates, 8 from the Galaxy, 2 from the Large Magellanic Cloud (LMC), and 2 from the Small Magellanic Cloud (SMC). Based on the analysis of high-resolution spectroscopic (FEROS) and photometric data, we confirmed the presence of the B[e] phenomenon for all objects of our sample, except for one (IRAS 07455-3143). We derived their effective temperature, spectral type, luminosity class, interstellar extinction and, using the distances from Gaia DR2, we obtained their bolometric magnitude, luminosity, and radius. Modelling of the forbidden l

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Majewski, S. R., J. C. Ostheimer, W. E. Kunkel, K. V. Johnston, R. J. Patterson, and C. Palma. "A Search for Tidal Stellar Debris from the Magellanic Clouds: Survey Results from the First Two Years." Symposium - International Astronomical Union 190 (1999): 508–10. http://dx.doi.org/10.1017/s007418090011873x.

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An important discriminant between leading models for the origin of the Magellanic Stream is the presence of a stellar counterpart to the HI gas stream: ram pressure stripping of gas by a putative hot Galactic halo would act only on Magellanic gas while gravitational tidal stripping would act on both gas and stars. Several previous attempts to find tidal stellar debris have failed to find carbon stars, A stars, or other main sequence stars in the Magellanic Stream (Mathewson et al. 1979; Recillas-Cruz 1982; Brück & Hawkins 1983; Guhathakurta & Lin 1999). However, there has long been a s

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Ostrov, P. G., V. S. Niemela, and N. I. Morrell. "Discovery of a Stellar Association Surrounding the Massive Binary Sk–67°105 in the Large Magellanic Cloud." Symposium - International Astronomical Union 190 (1999): 235–36. http://dx.doi.org/10.1017/s0074180900117905.

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Sk–67°105, a luminous O4f type stars in the Large Magellanic Cloud, is the exiting star of the H II region N 50 (DEM 193). Niemela & Morrell (1986) found this hot star to be a massive short period double lined spectroscopic binary. Because luminous OB stars are usually found in young stellar groups, we have searched for such an aggregate in the vicinity of Sk–67°105.Here we report, as a result of our search, the discovery of a new OB association in the LMC. We also find that Sk–67°105 is the most luminous star of a small compact cluster inside this OB association.

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Pritchard, J. D., W. Tobin, M. Clark, and E. F. Guinan. "CCD photometry of variable stars in the Magellanic Clouds -- VI. The eclipsing binary HV 982 in the Large Magellanic Cloud." Monthly Notices of the Royal Astronomical Society 299, no. 4 (1998): 1087–96. http://dx.doi.org/10.1046/j.1365-8711.1998.01849.x.

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Antoniou, Vallia, Andreas Zezas, and Despina Hatzidimitriou. "A comprehensive study of the link between star-formation history and X-ray source populations in the SMC." Proceedings of the International Astronomical Union 4, S256 (2008): 355–60. http://dx.doi.org/10.1017/s1743921308028706.

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AbstractUsing Chandra, XMM-Newton and optical photometric catalogs we study the young X-ray binary (XRB) populations of the Small Magellanic Cloud (SMC). We find that the Be/X-ray binaries (Be-XRBs) are observed in regions with star-formation (SF) rate bursts ~30–70 Myr ago, which coincides with the age of maximum Be-star formation, while regions with strong but more recent SF (e.g., the Wing) are deficient in Be-XRBs. Using the 2dF spectrograph of the Anglo-Australian Telescope (AAT) we have obtained optical spectra of 20 High-Mass X-ray Binaries (HMXBs) in the SMC. All of these sources were

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