@article{ReyesIturbideVelazquezRosado2015,
  author    = {Reyes-Iturbide, J. and Vel{\´a}zquez, Pablo F. and Rosado, M.},
  title     = {3D numerical model for NGC 6888 Nebula},
  series = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  journal   = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-88485},
  pages     = {363},
  year      = {2015},
  abstract  = {We present 3D numerical simulations of the NGC6888 nebula considering the proper motion and the evolution of the star, from the red supergiant (RSG) to the Wolf-Rayet (WR) phase. Our simulations reproduce the limb-brightened morphology observed in [OIII] and X-ray emission maps. The synthetic maps computed by the numerical simulations show filamentary and clumpy structures produced by instabilities triggered in the interaction between the WR wind and the RSG shell.},
  language  = {en}
}
@article{RamirezAlegriaCheneBorissovaetal.2015,
  author    = {Ram{\´i}rez Alegr{\´i}a, S. and Chen{\´e}, A.-N. and Borissova, J. and Kurtev, R. and Navarro, C. and Kuhn, M. and Carballo-Bello, J. A.},
  title     = {A not so massive cluster hosting a very massive star},
  series = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  journal   = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-88477},
  pages     = {362},
  year      = {2015},
  abstract  = {We present the first physical characterization of the young open cluster VVVCL041. We spectroscopically observed the cluster main-sequence stellar population and a very-massive star candidate: WR62-2. CMFGEN modelling to our near-infrared spectra indicates that WR62-2 is a very luminous (10^6.4±0.2 L⊙)and massive (∼ 80M⊙) star.},
  language  = {en}
}
@article{MaryevaPolcaroRossietal.2015,
  author    = {Maryeva, O. and Polcaro, V. F. and Rossi, C. and Viotti, R.},
  title     = {Modeling of spectral variability of Romano's star},
  series = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  journal   = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-88462},
  pages     = {361},
  year      = {2015},
  abstract  = {We present results of investigation of spectral variability of one of the most interesting massive stars, Romano's star (M33/V532 or GR290), located in the M33 galaxy. Brightness of the star changes together with its spectral class, which varies from WN11 to WN8. Using CMFGEN code we estimated parameters of stellar atmosphere and found that during last ten years bolometric luminosity of the star changed synchronously with stellar magnitude. Our calculations argue in favor of the hypothesis of a post-LBV status of GR290.},
  language  = {en}
}
@article{KochiashviliBeradzeKochiashvilietal.2015,
  author    = {Kochiashvili, N. and Beradze, S. and Kochiashvili, I. and Natsvlishvili, R. and Vardosanidze, M.},
  title     = {New Photometric Observations of P Cygni},
  series = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  journal   = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-88452},
  pages     = {360},
  year      = {2015},
  abstract  = {We present the results of the new photometric observations of the famous hypergiant PCygni. New observations were obtained in 2014 using the 48 cm Cassegrain telescope of the Abastumani Astrophysical Observatory, Georgia. We reveal some interesting behaviors of the B,V,R,I light curves, and also report new results on the periodicity of PCygni's variation. The latter result is based on the analysis of the photometric data (U,B,V filters) collected at the Abastumani Observatory between 1937 and 1983.},
  language  = {en}
}
@article{KanarekSharaFahertyetal.2015,
  author    = {Kanarek, G. and Shara, M. and Faherty, J. and Zurek, D. and Moffat, Anthony F. J.},
  title     = {New Galactic Wolf-Rayet Stars},
  series = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  journal   = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-88448},
  pages     = {359},
  year      = {2015},
  abstract  = {Over the course of 6 months in 2013, we observed nearly 400 Wolf-Rayet candidates in the Galactic plane. Preliminary results from this dataset are presented.},
  language  = {en}
}
@article{IgnaceToalaOskinova2015,
  author    = {Ignace, R. and Toal{\´a}, Jes{\´u}s Alberto and Oskinova, Lidia M.},
  title     = {Inversion of Intensity Profiles for Bubble Emissivity},
  series = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  journal   = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-88432},
  pages     = {358},
  year      = {2015},
  abstract  = {Under the assumption of spherical symmetry, the run of intensity with impact parameter for a spatially resolved and optically thin bubble can be inverted for an "effective emissivity" as a function of radius. The effective emissivity takes into account instrumental sensitivity and even interstellar absorption. This work was supported by a grant from NASA (G03-14008X).},
  language  = {en}
}
@article{GormazMatamalaHerveCheneetal.2015,
  author    = {Gormaz-Matamala, A. C. and Herv{\´e}, A. and Chen{\´e}, A.-N. and Cur{\´e}, M. and Mennickent, R. E.},
  title     = {Results Of The Spectroscopic Analysis Of WR6 Using CMFGEN},
  series = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  journal   = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-88422},
  pages     = {357},
  year      = {2015},
  abstract  = {Using ESPaDOnS optical spectra of WR6, we search variations on the stellar wind parameters during the different phases of the spectral variations. We use the radiative transfer code CMFGEN (Hillier \& Miller 1998) to determine the wind parameters. Our work gives mean parameters for WR6, Teff = 55 kK, M = 2.7 × 10^-5 M⊙/yr and v∞ =1700 km/s. Furthermore the line profiles variations at different phases are the consequence of a variation of mass loss rate and temperature un the winds. Effective temperature reaches 59 kK at the highest intensity, whereas the mass-loss rate decreases to 2.5 × 10^-5 M⊙/yr in that case. On the other hand, effective temperature decreases to 52.5 kK and the mass-loss rate increases to 3 × 10^-5 M/⊙yr when the line profile reach its minimum intensity. Results confirm the variable nature of the stellar wind, presented in this case on two of its fundamental parameters: temperature and mass-loss; which could be used to constrain the nature of the instability at the basis of the wind.},
  language  = {en}
}
@article{CalderonBalloneCuadraetal.2015,
  author    = {Calder{\´o}n, D. and Ballone, A. and Cuadra, J. and Schartmann, M. and Burkert, Andreas and Gillessen, S.},
  title     = {Formation of the infalling Galactic Centre cloud G2 by collision of stellar winds},
  series = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  journal   = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-88412},
  pages     = {356},
  year      = {2015},
  abstract  = {The gas cloud G2 is currently being tidally disrupted by the Galactic Centre super-massive black hole, Sgr A*. The region around the black hole is populated by ∼ 30 Wolf-Rayet stars, which produce strong outflows. Here we explore the possibility that gas clumps like G2 originate from the collision of stellar winds via the non-linear thin shell instability.},
  language  = {en}
}
@article{BibbySharaZureketal.2015,
  author    = {Bibby, J. and Shara, M. and Zurek, D. and Crowther, P. A. and Moffat, Anthony F. J. and Drissen, L. and Wilde, M.},
  title     = {The Distribution of Massive Stars in M101},
  series = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  journal   = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-88402},
  pages     = {355},
  year      = {2015},
  abstract  = {75 WR stars and 164 RSGs are identified in a single WFC3 pointing of our M101 survey. We find that within it's large star-forming complex NGC 5462 WR stars are preferentially located in the core whilst RSGs are found in the halo, suggesting two bursts of star-formation. A review of our WR candidates reveals that only ∼30\% are detected in the archival broad-band ACS imaging whilst only ∼50\% are associated with HII regions.},
  language  = {en}
}
@article{Bestenlehner2015,
  author    = {Bestenlehner, J. M.},
  title     = {Stellar parameters from photometric data for fainter and more distant Wolf-Rayet stars},
  series = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  journal   = {Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.-5. June 2015},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-88390},
  pages     = {354},
  year      = {2015},
  abstract  = {Spectroscopy is the preferred way to study the physical and wind properties of Wolf-Rayet (WR) stars, but with decreasing brightness and increasing distance of the object spectroscopy become very expensive. However, photometry still delivers a high signal to noise ratio. Current and past astronomical surveys and space missions provide large data sets, that can be harvested to discover new WR stars and study them over a wide metallicity range with the help of state of the art stellar atmosphere and evolutionary models.},
  language  = {en}
}