The origin of the young stellar population in the solar neighborhood — A link to the formation of the Local Bubble?

@article{Berghoefer2002TheOO,
  title={The origin of the young stellar population in the solar neighborhood — A link to the formation of the Local Bubble?},
  author={T. W. Berghoefer and Dieter Breitschwerdt},
  journal={Astronomy and Astrophysics},
  year={2002},
  volume={390},
  pages={299-306}
}
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 years. Using Hipparcos stellar distances and the results of kinematical analyses by Asiain et al. (1999a) on the Pleiades moving groups, we are able to show that subgroup B1, consisting of early type B stars up to 10 M, but lacking more massive objects, has passed through the local interstellar… 

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References

SHOWING 1-10 OF 31 REFERENCES
The Geminga supernova as a possible cause of the local interstellar bubble
THE Solar System resides at the edge of a cavity of hot (106 K), low-density (5×10−3 cm−3), X-ray emitting gas embedded in the interstellar medium1–4. This void, sometimes called the Local Bubble, is
Supershells and propagating star formation
Stellar winds and repeated supernovae from an OB association will create a cavity of coronal gas in the interstellar medium, with radius greater than 100 pc, surrounded by a dense, expanding shell of
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
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
Local interstellar medium
This paper reviews and analyses various observational data about the local interstellar medium (LISM)-a volume with a radius of about 200 pc near the Sun. There are collected radio, IR, optical, UV,
Local stellar kinematics from Hipparcos data
TLDR
From the parallaxes and proper motions of a kinematically unbiased subsample of the Hipparcos Catalogue, it is re-determined as a function of colour the kinematics of main-sequence stars that spiral arms are responsible for the non-axisymmetry and that R0/Rd ≃ 3 to 3, where Rd is the scalelength of the disc.
The Initial Mass Function and Massive Star Evolution in the OB Associations of the Northern Milky Way
We investigate the massive star content of Milky Way clusters and OB associations in order to answer three questions: (1) How coeval is star formation? (2) How constant is the initial mass function
LISM structure — Fragmented superbubble shell?
Small scale structure in local interstellar matter (LISM) is considered. Overall morphology of the local cloud complex is inferred from Ca II absorption lines and observations of H I in white dwarf
Superbubbles in disk galaxies
Correlated supernovae from an OB association create a superbubble: a large, thin, shell of cold gas surrounding a hot pressurized interior. Because supernova blast waves usually become subsonic
The local interstellar medium
Observations and theoretical models of the local interstellar medium (LISM), defined as the region within a column density contour of 10 to the 19th H atoms/sq cm, are reviewed. The existence and
...
...