73 citations · 590 across the 23 of their papers we have counts for
6 papers · 1 filter
BRITE-Constellation high-precision time-dependent photometry of the early-O-type supergiant Puppis unveils the photospheric drivers of its small- and large-scale wind structures
Tahina Ramiaramanantsoa, Anthony F. J. Moffat, Robert Harmon +33
From months of dual-band optical photometric monitoring at the mmag level, BRITE-Constellation has revealed two simultaneous types of variability in the O4I(n)fp star …
A detailed X-ray investigation of zeta Puppis IV. Further characterization of the variability
Yael Naze, Tahina Ramiaramanantsoa, Ian R. Stevens +2
Previously, the X-ray emission of zeta Puppis was found to be variable with light curves harbouring "trends" with a typical timescale longer than the exposure length. The origin of…
The variability of the BRITE-est Wolf-Rayet binary, Velorum I. Photometric and spectroscopic evidence for colliding winds
Noel D. Richardson, Christopher M. P. Russell, Lucas St-Jean +26
We report on the first multi-color precision light curve of the bright Wolf-Rayet binary Velorum, obtained over six months with the nanosatellites in the BRITE- Constellation…
BRITE-Constellation: Data processing and photometry
Adam Popowicz, Andrzej Pigulski, Krzysztof Bernacki +15
The BRITE mission is a pioneering space project aimed at the long-term photometric monitoring of the brightest stars in the sky by means of a constellation of nano-satellites. Its…
Studying the photometric and spectroscopic variability of the magnetic hot supergiant Orionis Aa
B. Buysschaert, C. Neiner, N. D. Richardson +14
Massive stars play a significant role in the chemical and dynamical evolution of galaxies. However, much of their variability, particularly during their evolved supergiant stage, i…
The Most Massive Heartbeat: An In-depth Analysis of ι Orionis
Herbert Pablo, N. D. Richardson, J. Fuller +17
ι Ori is a well studied massive binary consisting of an O9 III + B1 III/IV star. Due to its high eccentricity (e = 0.764) and short orbital period (P orb = 29.13376 d), it has been…