Probing the evolving massive star population in Orion with kinematic and radioactive tracers

@article{Voss2010ProbingTE,
  title={Probing the evolving massive star population in Orion with kinematic and radioactive tracers},
  author={Rasmus Voss and Roland Diehl and Jacco Vink and Dieter H. Hartmann},
  journal={Astronomy and Astrophysics},
  year={2010},
  volume={520},
  pages={1-10}
}
Context. Orion is the nearest star-forming region to host a significant number of young and massive stars. The energy injected by these OB stars is thought to have created the Eridanus superbubble. Because of its proximity, Orion is a prime target for a detailed investigation of the interaction between massive stars and their environment. Aims. We study the massive star population of Orion and its feedback in terms of energy and mass, in order to compare the current knowledge of massive stars… 

Figures and Tables from this paper

Energetic feedback and 26Al from massive stars and their supernovae in the Carina region
Aims. We study the populations of massive stars in the Carina region and their energetic feedback and ejection of 26 Al. Methods. We did a census of the stellar populations in young stellar clusters
Feedback by massive stars and the emergence of superbubbles II. X-ray properties
Context. In a previous paper we investigated the energy transfer of massive stars to the interstellar medium (ISM) as a function of time and the geometrical configuration of three massive stars via
Feedback by massive stars and the emergence of superbubbles - I. Energy efficiency and Vishniac instabilities
Context. Massive stars influence their environment via stellar winds , ionising radiation and supernova explosions. This is sign ified by observed interstellar bubbles. Such “feedback” is an
The radioactive nuclei and in the Cosmos and in the solar system
The cosmic evolution of the chemical elements from the Big Bang to the present time is driven by nuclear fusion reactions inside stars and stellar explosions. A cycle of matter recurrently
The GALAH survey: Chemical homogeneity of the Orion complex
Due to its proximity, the Orion star forming region is often used as a proxy to study processes related to star formation and to observe young stars in the environment they were born in. With the
Gas shells and magnetic fields in the Orion-Eridanus superbubble
Aims. The Orion-Eridanus superbubble has been blown by supernovae and supersonic winds of the massive stars in the Orion OB associations. It is the nearest site at which stellar feedback on the
Cosmic Rays in the Orion-Eridanus Superbubble
The Orion-Eridanus superbubble, formed from the winds and the explosions of Orion’s massive stars, could be a cosmic-ray acceleration site. Inside the superbubble, the large level of
Triggered Star Formation inside the Shell of a Wolf-Rayet Bubble as the Origin of the Solar System.
TLDR
It is estimated that 1%-16% of all Sun-like stars could have formed in such a setting of triggered star formation in the shell of a W-R bubble, and this model is a viable model that can explain the initial abundances of 26Al and 60Fe.
Steady-state nucleosynthesis throughout the Galaxy
Multiple star systems in the Orion nebula
This work presents an interferometric study of the massive-binary fraction in the Orion Trapezium cluster with the recently comissioned GRAVITY instrument. We observed a total of 16 stars of mainly
...
...

References

SHOWING 1-10 OF 62 REFERENCES
Using population synthesis of massive stars to study the interstellar medium near OB associations
Aims. We study the massive stars in OB associations and their surrounding interstellar medium environment, using a population synthesis code. Methods. We developed a new population synthesis code for
A census of the Carina Nebula — I. Cumulative energy input from massive stars
The Carina Nebula (NGC 3372) is our richest nearby laboratory in which to study feedback through ultraviolet radiation and stellar winds from very massive stars during the formation of an OB
The brightest stars of the σ Orionis cluster
Context. The very young σ Orionis cluster (∼3 Ma) is a cornerstone in understanding the formation of stars and substellar objects down to planetary masses. However, its stellar population is far from
The Spatial Distribution of the λ Orionis Pre-Main-Sequence Population
The λ Ori star-forming region presents a snapshot of a moderate-mass giant molecular cloud 1–2 Myr after cloud disruption by OB stars, with the OB stars, the low-mass stellar population, remnant
New estimates of the gamma-ray line emission of the Cygnus region from INTEGRAL/SPI observations
Context. The Cygnus region harbours a huge complex of massive stars at a distance of 1.0–2.0 kpc from us. About 170 O stars are distributed over several OB associations, among which the Cyg OB2
The distance to the Orion Nebula cluster
The distance to the Orion Nebula cluster (ONC) is estimated using the rotational properties of its low-mass pre-main-sequence (PMS) stars. Rotation periods, projected equatorial velocities and
A census of the Carina Nebula – II. Energy budget and global properties of the nebulosity
The first paper in this series took a direct census of energy input from the known OB stars in the Carina Nebula, and in this paper we study the global properties of the surrounding nebulosity. This
Radioactive 26Al from massive stars in the Galaxy
TLDR
High spectral resolution measurements of 26Al emission at 1808.65 keV demonstrate that the 26Al source regions corotate with the Galaxy, supporting its Galaxy-wide origin and determining a present-day equilibrium mass of 2.8 (± 0.8) solar masses of 27Al.
25 Orionis: A Kinematically Distinct 10 Myr Old Group in Orion OB1a*
We report here on the photometric and kinematic properties of a well-defined group of nearly 200 low-mass pre-main-sequence stars, concentrated within ~1? of the early-B star 25 Ori, in the Orion
Stellar evolution with rotation XI. Wolf-Rayet star populations at different metallicities
Grids of models of massive stars (M ≥ 20 M� ) with rotation are computed for metallicities Z ranging from that of the Small Magellanic Cloud (SMC) to that of the Galactic Centre. The hydrostatic
...
...