The evolution of massive stars and their spectra - I. A non-rotating 60 M⊙ star from the zero-age main sequence to the pre-supernova stage

  title={The evolution of massive stars and their spectra - I. A non-rotating 60 M⊙ star from the zero-age main sequence to the pre-supernova stage},
  author={Jose H Groh and Georges Meynet and Sylvia Ekstrom and Cyril Georgy},
  journal={Astronomy and Astrophysics},
For the first time, the interior and spectroscopic evolution of a massive star is analyzed from the zero-age main sequence (ZAMS) to the pre-supernova (SN) stage. For this purpose, we combined stellar evolution models using the Geneva code and atmospheric models using CMFGEN. With our approach, we were able to produce observables, such as a synthetic high-resolution spectrum and photometry, aiding the comparison between evolution models and observed data. Here we analyze the evolution of a non… 

Spectroscopic evolution of massive stars near the main sequence at low metallicity

Context. The evolution of massive stars is not fully understood. Several physical processes affect their life and death, with major consequences on the progenitors of core-collapse supernovae,

Spectroscopic evolution of massive stars on the main sequence

Context. The evolution of massive stars depends on several parameters, and the relation between different morphological types is not fully constrained. Aims. We aim to provide an observational view

Impact of mass-loss on the evolution and pre-supernova properties of red supergiants

The post main-sequence evolution of massive stars is very sensitive to many parameters of the stellar models. Key parameters are the mixing processes, the metallicity, the mass-loss rate and the

Modeling the early evolution of massive OB stars with an experimental wind routine - The first bi-stability jump and the angular momentum loss problem

Context. Stellar evolution models of massive stars are very sensitive to the adopted mass-loss scheme. The magnitude and evolution of mass-loss rates significantly affect the main sequence evolution,

The Evolution and Properties of Rotating Massive Star Populations

We investigate the integrated properties of massive ( ) rotating single-star stellar populations for a variety of initial rotation rates ( , 0.2, 0.4, 0.5, and 0.6). We couple the new MESA Isochrone

Helium and nitrogen enrichment in massive main-sequence stars: mechanisms and implications for the origin of WNL stars

The evolutionary paths taken by massive stars with M ≳ 60 M⊙ remain substantially uncertain. They begin their lives as main-sequence (MS) O stars. Depending on their masses, rotation rates, and

Early-time spectra of supernovae and their precursor winds: the luminous blue variable/yellow hypergiant progenitor of SN 2013cu

We present the first quantitative spectroscopic modeling of an early-time supernova that interacts with its progenitor wind. Using the radiative transfer code CMFGEN, we investigate the

Predicting the nature of supernova progenitors

  • J. Groh
  • Physics
    Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences
  • 2017
Recent efforts to predict the nature of stars before death by performing coupled stellar evolution and atmosphere modelling of single stars in the pre-SN stage are reviewed, and the detectability of SN Ibc progenitors is assessed.

Impact of binary interaction on the evolution of blue supergiants

A large fraction of massive stars evolve in interacting binary systems, which dramatically modifies the outcome of stellar evolution. We investigated the properties of blue supergiants in binary

The Galactic WC and WO stars

Wolf-Rayet stars of the carbon sequence (WC stars) are an important cornerstone in the late evolution of massive stars before their core collapse. As core-helium burning, hydrogen-free objects with



Fundamental properties of core-collapse Supernova and GRB progenitors: predicting the look of massive stars before death

We investigate the fundamental properties of core-collapse Supernova (SN) progenitors from single stars at solar meta llicity. For this purpose, we combine Geneva stellar evolutionary models with


We present the first set of a new generation of models of massive stars with a solar composition extending between 13 and 120 M☉, computed with and without the effects of rotation. We included two

Massive stars at low metallicity - Evolution and surface abundances of O dwarfs in the SMC

We study the evolution, rotation, and surface abundances of O-type dwarfs in the Small Magellanic Cloud. We analyzed the UV and optical spectra of twenty-three objects and derived photospheric and

Grids of stellar models with rotation - II. WR populations and supernovae/GRB progenitors at Z = 0.014

Context. In recent years, many very interesting observations have appeared concerning the positions of Wolf-Rayet (WR) stars in the Hertzsprung-Russell diagram (HRD), the number ratios of WR stars,

Presupernova Evolution of Rotating Massive Stars. I. Numerical Method and Evolution of the Internal Stellar Structure

The evolution of rotating stars with zero-age main-sequence (ZAMS) masses in the range 8-25 M☉ is followed through all stages of stable evolution. The initial angular momentum is chosen such that the

Grids of stellar models with rotation - I. Models from 0.8 to 120 M⊙ at solar metallicity (Z = 0.014)

Aims. Many topical astrophysical research areas, such as the properties of planet host stars, the nature of the progenitors of different types of supernovae and gamma ray bursts, and the evolution of

The most massive stars in the Arches cluster

Aims. We study a sample composed of 28 of the brightest stars in the Arches cluster. Our aim is to constrain their stellar and wind properties and to establish their nature and evolutionary status.

A comparison of evolutionary tracks for single Galactic massive stars

Context. The evolution of massive stars is not fully understood. The relation between different types of evolved massive stars is not clear, and the role of factors such as binarity, rotation or

Mass loss from late-type WN stars and its Z-dependence: very massive stars approaching the Eddington limit

The mass loss from Wolf-Rayet (WR) stars is of fundamental importance for the final fate of massive stars and their chemical yields. Its Z-dependence is discussed in relation to the formation of

Constraints on the Evolution of Massive Stars through Spectral Analysis. I. The WC5 Star HD 165763

Using a significantly revised non-LTE radiative transfer code that allows for the effects of line blanketing by He, C, O, Si, and Fe, we have performed a detailed analysis of the Galactic Wolf-Rayet