The History and Future of the Local and Loop I Bubbles

@article{Breitschwerdt2006TheHA,
  title={The History and Future of the Local and Loop I Bubbles},
  author={Dieter Breitschwerdt and Miguel A. de Avillez},
  journal={Astronomy and Astrophysics},
  year={2006},
  volume={452}
}
Context. The Local and Loop I superbubbles are the closest and best investigated supernova (SN) generated bubbles and serve as test laboratories for observations and theories of the interstellar medium. Aims. Since the morphology and dynamical evolution of bubbles depend on the ambient density and pressure distributions, a realistic modelling of the galactic environment is crucial for a detailed comparison with observations. Methods. We have performed 3D high resolution (down to 1.25 pc on a… 

Figures from this paper

What Physical Processes Drive the Interstellar Medium in the Local Bubble?
Recent 3D high-resolution simulations of the interstellar medium in a star forming galaxy like the Milky Way show that supernova explosions are the main driver of the structure and evolution of the
Non-equilibrium ionization modeling of the Local Bubble. I. Tracing Civ, Nv, and Ovi ions
Aims. We present the first high-resolution non-equilibrium ionization simulation of the joint evolution of the Local Bubble (LB) and Loop I superbubbles in the turbulent supernova-driven interstellar
Mapping the interface between the Local and Loop I bubbles using Strömgren photometry
Context. The Sun is located inside an extremely low density region of quite irregular shape called the Local Bubble or Local Cavity. The fraction of this cavity filled with extremely hot gas is known
Superbubble evolution in disk galaxies - I. Study of blow-out by analytical models
Context. Galactic winds are a common phenomenon in starburst galaxies in the local universe as well as at higher redshifts. Their sources are superbubbles driven by sequential supernova explosions in
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
A Way Out of the Bubble Trouble? - Upon Reconstructing the Origin of the Local Bubble and Loop I via Radioisotopic Signatures on Earth
Deep-sea archives all over the world show an enhanced concentration of the radionuclide $^{60}$Fe, isolated in layers dating from about 2.2 Myr ago. Since this comparatively long-lived isotope is not
Numerical studies on the link between radioisotopic signatures on Earth and the formation of the Local Bubble. I. 60Fe transport to the solar system by turbulent mixing of ejecta from nearby supernovae into a locally homogeneous interstellar medium
The discovery of radionuclides like 60Fe with half-lives of million years in deep-sea crusts and sediments offers the unique possibility to date and locate nearby supernovae. We want to
The trouble with the Local Bubble
The model of a Local Hot Bubble has been widely accepted as providing a framework that can explain the ubiquitous presence of the soft X-ray background diffuse emission. We summarize the current
Origin of the Local Bubble
AbstractWe present a new unbiased search for OB associations in the Solar neighbourhood which have hosted the progenitor stars of the core collapse supernovae responsible for the Local Bubble in the
26Al kinematics: superbubbles following the spiral arms? Constraints from the statistics of star clusters and HI supershells
Context. High-energy resolution spectroscopy of the 1.8 MeV radioactive decay line of 26Al with the SPI instrument onboard the INTEGRAL satellite has recently revealed that diffuse 26Al has higher
...
...

References

SHOWING 1-10 OF 42 REFERENCES
Multiple Supernova Remnant Models of the Local Bubble and the Soft X-Ray Background
This paper examines the possibility that a series of two or three supernovae in the diffuse interstellar medium might be capable of generating a long-lived hot diffuse bubble with characteristics
Testing Global ISM Models: A Detailed Comparison of O VI Column Densities with FUSE and Copernicus Data
We study the O VI distribution in space and time in a representative section of the Galactic disk using three-dimensional adaptive mesh refinement hydrodynamic and magnetohydrodynamic simulations of
The origin of the young stellar population in the solar neighborhood — A link to the formation of the Local Bubble?
We have analyzed the trajectories of moving stellar groups in the solar neighborhood in an attempt to estimate the number of supernova explosions in our local environment during the past 20 million
3D mapping of the dense interstellar gas around the Local Bubble
We present intermediate results from a long-term program of mapping the neutral absorption characteristics of the local interstellar medium, motivated by the availability of accurate and consistent
Global dynamical evolution of the ISM in star forming galaxies. I. High resolution 3D simulations: Effect of the magnetic field
In star forming disk galaxies, matter circulation between stars and the interstellar gas, and, in particular the energy input by random and clustered supernova explosions, determine the dynamical and
Volume filling factors of the ISM phases in star forming galaxies. I. The role of the disk-halo interaction
The role of matter circulation between the disk and halo in establishing the volume filling factors of the different ISM phases in the Galactic disk (|z |≤ 250 pc) is investigated, using a modified
Abundances of Deuterium, Nitrogen, and Oxygen in the Local Interstellar Medium: Overview of First Results from the FUSE Mission
Observations obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE) have been used to determine the column densities of D I, N I, and O I along seven sight lines that probe the local
Hot gas in the interstellar medium: A reanalysis of O VI absorption data
The Copernicus O(+5) column densities toward 72 stars provide a rare and valuable tracer of 10(exp 5.5) K gas in the interstellar medium. The original analysis of the data by Jenkins provided
The neutral atomic phases of the interstellar medium
We calculate the thermal equilibrium gas temperature of the diffuse interstellar medium. Our method incorporates a new photoelectric heating rate from small grains and polycyclic aromatic
Extended adiabatic blast waves and a model of the soft X-ray background. [interstellar matter
An analytical approximation is generated which follows the development of an adiabatic spherical blast wave in a homogeneous ambient medium of finite pressure. At early times when the external
...
...