46 citations · 103 across the 8 of their papers we have counts for
7 papers · 1 filter
Evidence for the emergence of stellar magnetic fields during rapid mass transfer
Gregg A. Wade, Tomer Shenar, Pablo Marchant +6
Binary interaction fundamentally alters the evolution of massive stars, yet the physical consequences of mass transfer remain poorly constrained. Here we present high-resolution sp…
A Detailed Spectroscopic Study of the WN6ha + O5 Colliding-wind Binary WR 25
Eric Gosset, Roberto Gamen, Laurent Mahy +3
Massive stars have a major impact on their environment in their host galaxy. Observational determinations of their physical parameters are required to better constrain evolutionary…
B fields in OB stars (BOB): Detection of a strong magnetic field in the O9.7 V star HD54879
N. Castro, L. Fossati, S. Hubrig +14
The number of magnetic stars detected among massive stars is small; nevertheless, the role played by the magnetic field in stellar evolution cannot be disregarded. Links between li…
The BinaMIcS project: understanding the origin of magnetic fields in massive stars through close binary systems
E. Alecian, C. Neiner, G. A. Wade +11
It is now well established that a fraction of the massive (M>8 Msun) star population hosts strong, organised magnetic fields, most likely of fossil origin. The details of the gener…
On the nature of the WO3 star DR1 in IC 1613
F. Tramper, G. Gräfener, O. E. Hartoog +8
We present the results of a quantitative spectroscopic analysis of the oxygen-sequence Wolf- Rayet star DR1 in the low-metallicity galaxy IC 1613. Our models suggest that the stron…
Rotational properties of the O-type star population in the Tarantula region
O. H. Ramírez-Agudelo, S. Simón-Díaz, H. Sana +15
The 30 Doradus (30\,Dor) region in the Large Magellanic Cloud (also known as the Tarantula Nebula) is the nearest massive starburst region, containing the richest sample of massive…
The nature of the line profile variability in the spectrum of the massive binary HD 152219
H. Sana
HD 152219 is a massive binary system with O9.5 III + B1-2 V/III components and a short orbital period of 4.2 d. Its primary component further displays clear line profile variabilit…