The search for the origin of the Local Bubble redivivus

  title={The search for the origin of the Local Bubble redivivus},
  author={Burkhard Fuchs and Dieter Breitschwerdt and Miguel A. de Avillez and Christian Dettbarn and Chris Flynn},
  journal={Monthly Notices of the Royal Astronomical Society},
ABSTRACT We present anew unbiasedsearchand analysisofall B starsin the solarneighbourhood(within a volume of 400 pc diameter) using the Arivel data base to track down theremains of the OB associations, which hosted the supernovae responsible for the LocalBubble in the interstellar gas. We find after careful dereddening and by comparisonwith theoretical isochrones, that besides the Upper Scorpius the Upper CentaurusLupus and Lower Centaurus Crux subgroups are the youngest stellar associations… 

Figures from this paper

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
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
The Sun is located inside an extremely low density region called the Local Bubble (LB). Although they have been studied through a large variety of techniques, the contours of its neutral boundary,
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
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
Open clusters IC 4665 and Cr 359 and a probable birthplace of the pulsar PSR B1929+10
Based on the epicyclic approximation, we have simulated the motion of the young open star clusters IC 4665 and Collinder 359. The separation between the cluster centers is shown to have been minimal
Star formation near the Sun is driven by expansion of the Local Bubble
Three-dimensional analysis of the solar neighbourhood shows that nearly all star-forming regions near the Sun lie on the surface of the Local Bubble, which was inflated by supernovae about 14 million years ago, providing robust observational support for the theory of supernova-driven star formation.
The locations of recent supernovae near the Sun from modelling 60Fe transport
Calculations of the most probable trajectories and masses of the supernova progenitors, and hence their explosion times and sites, are reported and the model reproduces the measured relative abundances very well.
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
A census of the nearby Pisces-Eridanus stellar stream
Aims. Within a sphere of 400 pc radius around the Sun, we aim to search for members of the Pisces-Eridanus (Psc-Eri) stellar stream in the Gaia Data Release 2 data set. We compare basic astrophysical


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
The History and Future of the Local and Loop I Bubbles
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
Characteristics of nearby interstellar matter
There is a warm tenuous partially ionized cloud (T∼104 K,n(HI)∼0.1 cm−3,n(Hii∼ 0.22–0.44 cm−3) surrounding the solar system which regulates the environment of the solar system, determines the
The Origin of the Local Bubble
The Sun is located in a low-density region of the interstellar medium partially filled with hot gas that is the likely result of several nearby supernova explosions within the last 10 Myr. Here we
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
Formation scenarios for the young stellar associations between galactic longitudes l = 280-360 deg
We investigate the spatial distribution, the space velocities and age distribution of the pre-main sequence (PMS) stars belonging to Ophiuchus, Lupus and Chamaeleon star-forming regions (SFRs), and
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
OB Stars in the Solar Neighborhood. II. Kinematics
Using the spatial classification method and the structural parameters estimated for the Gould Belt (GB) and the local Galactic disk (LGD) from a previous paper, we have evaluated spatial membership
The local surface density of disc matter mapped by Hipparcos
We determine the surface density of matter in the disc of the Galaxy at the solar position using K giant stars. The local space density and luminosity function of the giants is determined using
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