Masses and luminosities of O- and B-type stars and red supergiants

  title={Masses and luminosities of O- and B-type stars and red supergiants},
  author={Markus Matthias Hohle and Ralph Neuhaeuser and Bernard F. Schutz},
  journal={Astronomische Nachrichten},
Massive stars are of interest as progenitors of supernovae, i.e. neutron stars and black holes, which can be sources of gravitational waves. Recent population synthesis models can predict neutron star and gravitational wave observations but deal with a fixed supernova rate or an assumed initial mass function for the population of massive stars. Here we investigate those massive stars, which are supernova progenitors, i.e. with O- and early B-type stars, and also all supergiants within 3 kpc. We… 
Spectroscopic and physical parameters of Galactic O-type stars. III. Mass discrepancy and rotational mixing
Context. Massive stars play a key role in the evolution of galaxies and our Universe. Aims. Our goal is to compare observed and predicted properties of single Galactic O stars to identify and
The masses, and the mass discrepancy of O-type stars
Context. The “mass discrepancy” in massive O stars represents a long-standing problem in stellar astrophysics with far-reachin g implications for the chemical and dynamical feedback in galaxies.
Galactic kinematics from a sample of young massive stars
Based on published sources, we have created a kinematic database on 220 massive (> 10 M⊙) young Galactic star systems located within ≤3 kpc of the Sun. Out of them, ≈100 objects are spectroscopic
The Detection and Characterization of Be+sdO Binaries from HST/STIS FUV Spectroscopy
The B emission-line stars are rapid rotators that were probably spun up by mass and angular momentum accretion through mass transfer in an interacting binary. Mass transfer will strip the donor star
Determination of a temporally and spatially resolved supernova rate from OB stars within 5 kpc
We spatially and temporally resolve the future Supernova (SN) rate in the Solar vicinity and the whole Galaxy by comparing observational parameters of massive stars with theoretical models for
Fundamental properties of nearby single early B-type stars
Fundamental parameters of a sample of 26 apparently slowly-rotating single early B-type stars in the solar neighbourhood are presented and compared to high-precision data from detached eclipsing
The dependence of stellar age distributions on giant molecular cloud environment
In this Letter, we analyse the distributions of stellar ages in giant molecular clouds (GMCs) in spiral arms, interarm spurs and at large galactic radii, where the spiral arms are relatively weak. We
Photometric detection of internal gravity waves in upper main-sequence stars
Context. Main sequence stars with a convective core are predicted to stochastically excite internal gravity waves (IGWs), which effectively transport angular momentum throughout the stellar interior
Formation of high-mass stars in an isolated environment in the Large Magellanic Cloud
The aim of this study is to characterize the distribution and basic properties of the natal gas associated with high-mass young stellar objects (YSOs) in isolated environments in the Large
Supernovae producing unbound binaries and triples
  • C. Kochanek
  • Physics
    Monthly Notices of the Royal Astronomical Society
  • 2021
The fraction of stars that are in binaries or triples at the time of stellar death and the fraction of these systems that survive the supernova explosion are crucial constraints for evolution


Absolute magnitudes of OB and Be stars based on Hipparcos parallaxes – III
The absolute visual magnitudes, M v , of A-M stars are based on calculated Hipparcos trigonometric parallaxes. The sample used consists of 30986 unreddened and reddened A-M stars in luminosity
Accurate masses and radii of normal stars
SummaryBinary stars are the main source of fundamental data on stellar masses and radii (M, R). Considerable progress has been made in recent years in the quality and quantity of such data, and
Toward Understanding Massive Star Formation
AbstractAlthough fundamental for astrophysics, the processes that produce massive stars are not well understood. Large distances, high extinction, and short timescales of critical evolutionary phases
Young Close-By Neutron Stars: The Gould Belt Vs. The Galactic Disc
We present new population synthesis calculations of close young neutron stars. In comparison with our previous investigation we use a different neutron star mass spectrum and different initial
Simulation of a population of isolated neutron stars evolving through the emission of gravitational waves
We study, via a Monte Carlo simulation, a population of isolated asymmetric neutron stars where the magnitude of the magnetic field is low enough so that the dynamical evolution is dominated by the
3D dynamical evolution of the interstellar gas in the Gould Belt
The dynamical evolution of the Gould Belt has been modelled in 3D and compared to the spatial and velocity distributions of all HI and H 2 clouds found within a few hundred parsecs from the Sun and
The absolute magnitudes and spectral types of the stars in the gamma Velorum system.
The ratio of the visual luminosities of the O and WC components of the binary system gamma (2) Vel has been derived by comparison of the emission-line strengths in the spectrum with those in the
An Introduction to Close Binary Stars
Preface 1. Close binary stars - a historical review 2. Two-body orbital motion 3. The determination of orbits 4. Perturbations, the Roche model, and mass exchange/loss 5. Photometry and polarimetry -
Validation of the new Hipparcos reduction
Context. A new reduction of the astrometric data as produced by the Hipparcos mission has been published, claiming accuracies for nearly all stars brighter than magnitude Hp = 8 to be better, by up
Trigonometric parallaxes and a kinematically adjusted distance sale for OB associations
By directly comparing the photometric distances of Blaha and Humphreys (1989) (BH) to OB associations and field stars with the corresponding Hipparcos trigonometric parallaxes, we show that the BH