References of "Nazé, Yaël"
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See detailThe strange case of the Of?p stars
Nazé, Yaël ULg; Walborn, N. R.; Martins, F. et al

Poster (2009)

Detailed reference viewed: 5 (2 ULg)
See detailHot stars survey with the GAIA space mission
Lobel, A.; Liu, C.; Frémat, Y. et al

Poster (2009)

Detailed reference viewed: 18 (8 ULg)
See detailEmission line stars in the Milky Way with the GAIA space mission
Martayan, C.; Frémat, Y.; Blomme, R. et al

Poster (2009)

Detailed reference viewed: 5 (0 ULg)
See detailMassive stars and emission-line stars with GAIA
Blomme, Ronny; Frémat, Y.; Lobel, Alex et al

Poster (2009)

Detailed reference viewed: 7 (0 ULg)
See detailReaching the schools
Nazé, Yaël ULg

Poster (2009)

Detailed reference viewed: 4 (0 ULg)
See detailOutreach goals of the Europa Jupiter System Mission
Blanc, M.; Coustenis; Nazé, Yaël ULg et al

Poster (2009)

Detailed reference viewed: 11 (0 ULg)
See detailL'Astronomie des anciens
Nazé, Yaël ULg

Article for general public (2009)

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See detailAstrobiologie cours-conférence du Collège Belgique (ARB)
Javaux, Emmanuelle ULg; Wilmotte, Annick ULg; Claeys, Philippe et al

Learning material (2009)

cours enregistrés sur le site de l'ARB (http://www.academieroyale.be/)

Detailed reference viewed: 37 (8 ULg)
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See detailThe Gaia satellite: a tool for Emission Line Stars and Hot Stars
Martayan, C.; Frémat, Y.; Blomme, R. et al

in SF2A-2008 (2008, November 01)

The Gaia satellite will be launched at the end of 2011. It will observe at least 1 billion stars, and among them several million emission line stars and hot stars. Gaia will provide parallaxes for each ... [more ▼]

The Gaia satellite will be launched at the end of 2011. It will observe at least 1 billion stars, and among them several million emission line stars and hot stars. Gaia will provide parallaxes for each star and spectra for stars till V magnitude equal to 17. After a general description of Gaia, we present the codes and methods, which are currently developed by our team. They will provide automatically the astrophysical parameters and spectral classification for the hot and emission line stars in the Milky Way and other close local group galaxies such as the Magellanic Clouds. [less ▲]

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See detailThe first orbital solution for the massive colliding-wind binary HD 93162 (=WR 25)
Gamen, R.; Gosset, Eric ULg; Morrell, N. I. et al

in Revista Mexicana de Astronomia y Astrofisica Conference Series (2008, August 01)

Since the discovery, with EINSTEIN, of strong X-ray emission associated with HD 93162, this object was recurrently predicted by some authors to be a colliding-wind binary system. However, radial-velocity ... [more ▼]

Since the discovery, with EINSTEIN, of strong X-ray emission associated with HD 93162, this object was recurrently predicted by some authors to be a colliding-wind binary system. However, radial-velocity variations that would prove the suspected binary nature have never been found so far. We spectroscopically monitored this object in order to investigate its possible variability and to provide an answer to the above-mentioned discordance. We derived radial velocities from spectroscopic data acquired mainly between 1994 and 2006, and searched for periodicities. For the first time, periodic radial-velocity variations are detected. Our analysis definitively shows that the Wolf-Rayet star WR 25 is actually an eccentric binary system with a probable period of about 208 days. [less ▲]

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See detailTowards an Understanding of the Of?p star HD 191612: Optical Spectroscopy
Howarth, I. D.; Walborn, N. R.; Lennon, D. J. et al

in Revista Mexicana de Astronomia y Astrofisica Conference Series (2008, August 01)

We have acquired extensive optical spectroscopy of the early-type magnetic star HD 191612 (O6.5f?pe-O8fp). The Balmer and HeI lines show strongly variable emission which is extremely reproducible on a ... [more ▼]

We have acquired extensive optical spectroscopy of the early-type magnetic star HD 191612 (O6.5f?pe-O8fp). The Balmer and HeI lines show strongly variable emission which is extremely reproducible on a well-determined 538-d period. Metal lines and HeII absorptions (including many selective emission lines, but excluding HeII lambda 4686 Å emission) are nearly constant in line strength, but are variable in velocity. The radial-velocity variations establish a double-lined binary orbit with P_{orb} = 1542d, e = 0.44; by elimination, rotational modulation of a magnetically constrained plasma is left as by far the most likely `clock' underlying the 538-d changes. The implied rotation period shows that slow rotators can easily be hidden in the O-star population, with gaussian-like `turbulence' dominating the line widths. [less ▲]

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See detailEuroPlaNet: Improving the Communication on Planetary Sciences
Nazé, Yaël ULg; Heward, A.

in EPO and a Changing World: Creating Linkages and Expanding Partnerships (2008, June 01)

EuroPlaNet is an EC-funded consortium. It coordinates the activities of European researchers working in planetary sciences but it is not only aimed at pure scientific activities. Its outreach action ... [more ▼]

EuroPlaNet is an EC-funded consortium. It coordinates the activities of European researchers working in planetary sciences but it is not only aimed at pure scientific activities. Its outreach action involves a networking of the members, in order to promote the planetary sciences in Europe, improve the public awareness of the major European achievements & projects, and stimulate the use of planetary sciences for the promotion of scientific education and culture at large. For more information: \url{http://www.europlanet-eu.org/} or \url{http://www.europlanet.cesr.fr/}. [less ▲]

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See detailMagnetic Massive Stars
Townsend, Rich; Cohen, David H; Dessart, Luc et al

in IAU Symposium (2008, June 01)

Magnetic fields are unexpected in massive stars, due to the absence of a sub-surface convective dynamo. However, advances in instrumentation over the past three decades have led to their detection in a ... [more ▼]

Magnetic fields are unexpected in massive stars, due to the absence of a sub-surface convective dynamo. However, advances in instrumentation over the past three decades have led to their detection in a small but growing subset of these stars. Moreover, complementary theoretical developments have highlighted their potentially significant influence over the structure, evolution and circumstellar environments of massive stars. Here, we summarize a special session convened prior to the main conference, focused on presenting recent developments in the study of massive-star magnetic fields. [less ▲]

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See detailThe XMM-Newton view of the rich cluster Cyg OB2
Rauw, Grégor ULg; De Becker, Michaël ULg; Nazé, Yaël ULg et al

Poster (2008, May)

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See detailA binary signature in the non-thermal radio-emitter Cyg OB2 #9
Nazé, Yaël ULg; De Becker, Michaël ULg; Rauw, Grégor ULg et al

in Astronomy and Astrophysics (2008), 483

Aims. Non-thermal radio emission associated with massive stars is believed to arise from a wind-wind collision in a binary system. However, the evidence of binarity is still lacking in some cases, notably ... [more ▼]

Aims. Non-thermal radio emission associated with massive stars is believed to arise from a wind-wind collision in a binary system. However, the evidence of binarity is still lacking in some cases, notably Cyg OB2 #9. Methods: For several years, we have been monitoring this heavily-reddened star from various observatories. This campaign allowed us to probe variations both on short and long timescales and constitutes the first in-depth study of the visible spectrum of this object. Results: Our observations provide the very first direct evidence of a companion in Cyg OB2 #9, confirming the theoretical wind-wind collision scenario. These data suggest a highly eccentric orbit with a period of a few years, compatible with the 2 yr-timescale measured in the radio range. In addition, the signature of the wind-wind collision is very likely reflected in the behaviour of some emission lines. [less ▲]

Detailed reference viewed: 29 (4 ULg)
See detailLa vie tourmentée des amas globulaires
Nazé, Yaël ULg

Article for general public (2008)

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Detailed reference viewed: 14 (1 ULg)
See detailPluralité des Mondes
Nazé, Yaël ULg

Article for general public (2008)

Not Available

Detailed reference viewed: 10 (1 ULg)
See detailA la Une du cosmos (rubrique mensuelle depuis 2008)
Nazé, Yaël ULg

in Athena (2008)

Detailed reference viewed: 8 (2 ULg)
See detailA la une du Cosmos (rubrique mensuelle)
Nazé, Yaël ULg

Article for general public (2008)

Detailed reference viewed: 9 (6 ULg)
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See detailMultiplicity of O-type stars in NGC 2244
Mahy, Laurent ULg; Nazé, Yaël ULg; Rauw, Grégor ULg et al

Poster (2008)

We present the main results from our long‐term spectroscopic campaign devoted to the O‐type stars in the young open cluster NGC 2244. Previous works by our team on the O‐stars multiplicity in other young ... [more ▼]

We present the main results from our long‐term spectroscopic campaign devoted to the O‐type stars in the young open cluster NGC 2244. Previous works by our team on the O‐stars multiplicity in other young open clusters (IC 1805 and NGC 6231) showed that the number of binary systems in such clusters was larger than 40%. Until now, only two stars (HD 47129 and HD 48099) in the surroundings of NGC 2244 have been confirmed as spectroscopic binaries (SB) although Garcia & Mermilliod (2001) estimated the O‐type binary fraction at 50%. In this context, we revisited the spectral classification, the projected rotational velocity and the multiplicity of O‐type stars in NGC 2244. [less ▲]

Detailed reference viewed: 11 (5 ULg)