34 citations · 169 across the 19 of their papers we have counts for
19 papers
The Stellar Winds Atlas II: Black Hole Formation at Solar Metallicity
Amedeo Romagnolo, Floor S. Broekgaarden, Alex C. Gormaz-Matamala +7
Stellar winds are a primary source of uncertainty in predicting the masses of black holes (BHs) from massive stars. At solar metallicity, theoretical models lead to widely divergen…
X-Shooting ULLYSES: Massive stars at low metallicity XV. On the metallicity dependence of B-supergiant mass-loss rates
O. Verhamme, J. O. Sundqvist, A. de Koter +21
Context. For stellar evolution models we rely on mass-loss rate prescriptions that show features that lack empirical confirmation, such as the bi-stability jump. This jump is an in…
New self-consistent theoretical descriptions for mass-loss rates of O-type stars
F. Figueroa-Tapia, J. A. Panei, M. Curé +5
Massive O-type stars lose a significant fraction of their mass through radiation-driven winds, a process that critically shapes their evolution and feedback into the interstellar m…
The Stellar Winds Atlas I: Current uncertainties in mass-loss rates
Amedeo Romagnolo, Floor S. Broekgaarden, Konstantinos Antoniadis +1
Stellar winds are a major source of uncertainty in understanding the life and deaths of massive stars. Across studies in the field, prescriptions for stellar winds differ substanti…
Revisiting the Evolutionary Status of Massive Stars at the central parsec of the Milky Way
A. C. Gormaz-Matamala, J. Cuadra, B. Kubátová +2
Massive stars and their winds have a large influence in their environment, e.g, determining the accretion rate on to the Galactic Centre (GC) super-massive black hole Sgr A*. The w…
X-Shooting ULLYSES: Massive stars at low metallicity. IV. Spectral analysis methods and exemplary results for O stars
A. A. C. Sander, J. -C. Bouret, M. Bernini-Peron +26
CONTEXT: The spectral analysis of hot, massive stars is a fundamental astrophysical method to obtain their intrinsic properties and their feedback. Quantitative spectroscopy for ho…
X-Shooting ULLYSES: Massive stars at low metallicity VII. Stellar and wind properties of B supergiants in the Small Magellanic Cloud
M. Bernini-Peron, A. A. C. Sander, V. Ramachandran +22
Context. B supergiants (BSGs) represent an important connection between the main sequence and more extreme evolutionary stages of massive stars. Additionally, lying toward the cool…
Evolution of stars with 60 and 200 Msun: predictions for WNh stars in the Milky Way
Alex Camilo Gormaz-Matamala, Amedeo Romagnolo, Krzysztof Belczynski
We study in detail the evolution of two massive stars at solar metallicity (), by calculating their final masses, radial expansion, and chemical enrichment. We run evoluti…
Evolution of rotating massive stars adopting a newer, self-consistent wind prescription at SMC metallicity
Alex Camilo Gormaz-Matamala, Jorge Cuadra, Sylvia Ekström +3
We use Geneva-evolution-code to run evolutionary tracks for stellar masses ranging from to at SMC metallicity (). We upgrade the recipe for stellar win…
On the maximum black hole mass at solar metallicity
Amedeo Romagnolo, Alex C. Gormaz-Matamala, Krzysztof Belczynski
In high metallicity environments the mass that black holes (BHs) can reach just after core-collapse widely depends on how much mass their progenitor stars lose via winds. On one ha…
Evolution of rotating massive stars with new hydrodynamic wind models
Alex Camilo Gormaz-Matamala, Jorge Cuadra, Georges Meynet +1
Mass loss due to line-driven winds is central to our understanding of the evolution of massive stars. We extend the evolution models introduced in Paper I, where the mass loss reci…
Evolution of massive stars with new hydrodynamic wind models
A. C. Gormaz-Matamala, M. Curé, G. Meynet +3
Here we present evolutionary models for a set of massive stars, introducing a new prescription for the mass-loss rate obtained from hydrodynamical calculations in which the wind ve…
New self-consistent wind parameters fitting optical spectra of O-type stars observed with HERMES spectrograph
Alex C. Gormaz-Matamala, Michel Curé, Alex Lobel +5
We perform spectral fitting for a set of O-type stars based on self-consistent wind solutions, which provide mass-loss rate and velocity profiles directly derived from the initial…
New hydrodynamic solutions for line-driven winds of hot massive stars using Lambert -function
Alex C. Gormaz-Matamala, Michel Curé, D. John Hillier +3
Hot massive stars present strong stellar winds that are driven by absorption, scattering and re\-emission of photons by the ions of the atmosphere (\textit{line-driven winds}). A b…
Analytical Solutions for Radiation-Driven Winds in Massive Stars II: The -slow Regime
I. Araya, A. Christen, M. Curé +7
Accurate mass-loss rates and terminal velocities from massive stars winds are essential to obtain synthetic spectra from radiative transfer calculations and to determine the evolut…
Evolution of Line-Force Multiplier Parameters in Radiation Driven Winds of Massive Stars
Alex Camilo Gormaz-Matamala
We present two self-consistent procedures that couple the hydrodynamics with calculations of the line-force in the frame of radiation wind theory. These procedures give us the line…
Self-consistent solutions for line-driven winds of hot massive stars. The m-CAK procedure
Alex C. Gormaz-Matamala, Michel Curé, Lydia S. Cidale +1
Massive stars present strong stellar that which are described by the radiation driven wind theory. Accurate mass-loss rates are necessary to properly describe the stellar evolution…
Deriving Metallicities from Calcium Triplet Spectroscopy in combination with Near Infrared Photometry
F. Mauro, C. Moni Bidin, D. Geisler +7
Context. [...] One of the most efficient methods is the measurement of the equivalent width (EW) of the Calcium II Triplet (CaT), corrected for the luminosity and temperature effec…
Investigating potential planetary nebula/cluster pairs
Christian Moni Bidin, Daniel Majaess, Charles Bonatto +10
Fundamental parameters characterizing the end-state of intermediate-mass stars may be constrained by discovering planetary nebulae (PNe) in open clusters (OCs). Cluster membership…