Publications by authors named "F Baganoff"
Article Synopsis
- Sgr A* is a supermassive black hole at the center of the Milky Way that varies in its emissions of X-ray, near-infrared, and submillimeter radiation, making it a key subject for studying black hole accretion processes.
- Recent observations revealed two flares that challenge existing models of how these emissions are correlated over time, suggesting that the timing and mechanisms behind these emissions are more complex than previously thought.
- The findings highlight the need for ongoing, detailed multiwavelength studies to deepen our understanding of the fluctuations in emissions from Sgr A* and the processes at play.
Emission from Saggitarius A* is highly variable at both X-ray and infrared (IR) wavelengths. Observations over the last ~20 yr have revealed X-ray flares that rise above a quiescent thermal background about once per day, while faint X-ray flares from Sgr A* are undetectable below the constant thermal emission. In contrast, the IR emission of Sgr A* is observed to be continuously variable.
View Article and Find Full Text PDFThe tidal forces close to massive black holes can rip apart stars that come too close to them. As the resulting stellar debris spirals toward the black hole, the debris heats up and emits x-rays. We report observations of a stable 131-second x-ray quasi-periodic oscillation from the tidal disruption event ASASSN-14li.
View Article and Find Full Text PDFSagittarius A* (Sgr A*) is the variable radio, near-infrared (NIR), and X-ray source associated with accretion onto the Galactic center black hole. We present an analysis of the most comprehensive NIR variability data set of Sgr A* to date: eight 24 hr epochs of continuous monitoring of Sgr A* at 4.5 m with the IRAC instrument on the , 93 epochs of 2.
View Article and Find Full Text PDFArticle Synopsis
- The Galactic Centre features a unique group of young, massive stars near the supermassive black hole, Sagittarius A*, raising questions about stellar formation there.
- Previous research argued that soft X-ray emissions in the area are largely from accreting white dwarf systems, but limitations in detection technology have hindered the observation of hard X-ray emissions.
- New findings reveal a concentrated hard-X-ray emission in a small region, suggesting complex interactions involving more massive accreting white dwarfs, low-mass X-ray binaries, or new types of particle interactions, challenging our understanding of stellar evolution and cosmic phenomena in that region.