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See detailProspects for the study of dust making Wolf-Rayet binaries with the VLTI-Spectro-Imager (VSI)
De Becker, Michaël ULg; Filho, M.; Harries, T.

in Revista Mexicana de Astronomía y Astrofísica (2010, February), 38

In response to ESO's call for proposals for second generation instruments for the Very Large Telescope Interferometer (VLTI), a consortium has proposed to design and develop the VLTI-Spectro-Imager (VSI ... [more ▼]

In response to ESO's call for proposals for second generation instruments for the Very Large Telescope Interferometer (VLTI), a consortium has proposed to design and develop the VLTI-Spectro-Imager (VSI). In the context of the Phase A study, a science group has prepared a science case taking advantage of the expected performances of VSI. Among several science topics, the case of dust making Wolf-Rayet binaries producing the so-called pinwheel nebulae has been considered. Here, we review the main specifications of VSI, and we provide preliminary results expected to illustrate the imaging capabilities of VSI, and the interest for the study of pinwheel nebulae similar to those formed close to well-known systems such as WR98a and WR104. [less ▲]

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See detailLong baseline interferometry: a promising tool for multiplicity investigations of massive stars
De Becker, Michaël ULg

in Revista Mexicana de Astronomía y Astrofísica (2010, February), 38

Massive binaries are crucial laboratories that allow us to investigate processes occurring in quite extreme conditions, such as particle acceleration, high-energy emission, or even dust formation. All ... [more ▼]

Massive binaries are crucial laboratories that allow us to investigate processes occurring in quite extreme conditions, such as particle acceleration, high-energy emission, or even dust formation. All these processes are intimately dependent on binarity. Our understanding of the underlying physics strongly requires preliminary multiplicity studies likely to uncover still undetected binaries, and determine their orbital parameters. However, classical spectroscopic approaches sometimes fail to provide a solution to this issue. Long baseline interferometry turns out to be a promising complementary technique to address the question of the multiplicity of massive stars. A campaign has been initiated with the VLTI to take benefit of this technique. [less ▲]

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See detailThe mysterious Of?p class and the magnetic O-star theta(1) Ori C: Confronting observations
Nazé, Yaël ULg; Walborn, Nolan R.; Martins, Fabrice

in Revista Mexicana de Astronomía y Astrofísica (2008), 44(2), 331-340

In recent years, the stars of the Of?p category have revealed a wealth of peculiar phenomena: varying line profiles, photometric changes, and X-ray over-luminosity are only a few of their characteristics ... [more ▼]

In recent years, the stars of the Of?p category have revealed a wealth of peculiar phenomena: varying line profiles, photometric changes, and X-ray over-luminosity are only a few of their characteristics. Here we review their physical properties to facilitate comparisons among the Galactic members of this class. As one of them his been proposed to resemble the magnetic oblique rotator theta(1) Ori C, though with a longer period, this latter object is also included in our study to illuminate its similarities and differences with the Of?p category. [less ▲]

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See detailNew insights into the nature of the SMC WR/LBV binary HD 5980
Foellmi, C.; Koenigsberger, G.; Georgiev, L. et al

in Revista Mexicana de Astronomía y Astrofísica (2008), 44(1), 3-27

We present the results of optical wavelength observations of the unusual SMC eclipsing binary system HD 5980 obtained in 1999 and 2004-2005. Radial velocity curves for the erupting LBV/WR object (star A ... [more ▼]

We present the results of optical wavelength observations of the unusual SMC eclipsing binary system HD 5980 obtained in 1999 and 2004-2005. Radial velocity curves for the erupting LBV/WR object (star A) and its close WR-like companion (star B) are obtained by deblending the variable emission-line profiles of NIV and NV lines. The derived masses M-A = 58 - 79 M-circle dot and M-B = 51 - 67 M-circle dot, are more consistent with the the stars' location near the top of the HRD than previous estimates. The presence of a wind-wind interaction region is inferred from the orbital phase-dependent behavior of He I P Cygni absorption components. The emission-line intensities continued with the declining trend previously seen in UV spectra. The behavior of the photospheric absorption lines is consistent with the results of Schweickhardt (2000) who concludes that the third object in the combined spectrum, star C, is also a binary system with P-starC similar to 96.5 days, e=0.83. [less ▲]

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See detailQuasar Host Orientation and Polarization: Insights into the Type 1/Type 2 Dichotomy
Borguet, Benoît ULg; Hutsemekers, Damien ULg; Letawe, Géraldine ULg et al

in Revista Mexicana de Astronomía y Astrofísica (2008), 32

We investigate correlations between the optical linear polarization position angle and the orientation of the host galaxy/extended emission of Type 1 and Type 2 Radio-Loud (RL) and Radio-Quiet (RQ ... [more ▼]

We investigate correlations between the optical linear polarization position angle and the orientation of the host galaxy/extended emission of Type 1 and Type 2 Radio-Loud (RL) and Radio-Quiet (RQ) quasars. We have used high resolution Hubble Space Telescope (HST) data and deconvolution process to obtain a good determination of the host galaxy orientation. With these new measurements and a compilation of data from the literature, we find a significant correlation between the polarization position angle and the position angle of the major axis of the host galaxy/extended emission. The correlation appears different for Type 1 and Type 2 objects and depends on the redshift of the source. Interpretations in the framework of the unification model are discussed. [less ▲]

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See detailThe spectra of massive stars with GAIA
Bouret, J C; Lanz, T; Frémat, Y et al

in Revista Mexicana de Astronomía y Astrofísica (2008), 33

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