Superbubbles and energetic particles in the Galaxy

Parizot, E.; Marcowith, A.; Swaluw, E. van der; Bykov, A. M.; Tatischeff, V.

doi:10.1051/0004-6361:20041269

Cited by 194 publications

(194 citation statements)

References 68 publications

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“…In addition to shocks from WR winds and SNe shocks, the winds and mass loss of OB stars in phases other than WR are very significant and may produce substantial shocks, though not as significant as either WR or SNe shocks (Parizot, 2004;Bykov, 2001). Furthermore, although the average time between SN events in an OB association is long compared to the 59 Ni half-life, there will be a fraction of SN events that occur on shorter time scales, thus resulting in acceleration of recently synthesized 59 Ni before it can decay.…”

Section: Discussionmentioning

confidence: 99%

OB Associations, Wolf–Rayet Stars, and the Origin of Galactic Cosmic Rays

Binns

Wiedenbeck

Arnould³

et al. 2007

The Composition of Matter

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Abstract. We have measured the isotopic abundances of neon and a number of other species in the galactic cosmic rays (GCRs) using the Cosmic Ray Isotope Spectrometer (CRIS) aboard the ACE spacecraft. Our data are compared to recent results from two-component (Wolf-Rayet material plus solar-like mixtures) Wolf-Rayet (WR) models. The three largest deviations of galactic cosmic ray isotope ratios from solar-system ratios predicted by these models, 12 C/ 16 O, 22 Ne/ 20 Ne, and 58 Fe/ 56 Fe, are very close to those observed. All of the isotopic ratios that we have measured are consistent with a GCR source consisting of ~20% of WR material mixed with ~80% material with solar-system composition. Since WR stars are evolutionary products of OB stars, and most OB stars exist in OB associations that form superbubbles, the good agreement of our data with WR models suggests that OB associations within superbubbles are the likely source of at least a substantial fraction of GCRs. In previous work it has been shown that the primary 59 Ni (which decays only by electron-capture) in GCRs has decayed, indicating a time interval between nucleosynthesis and acceleration of >10 5 yr. It has been suggested that in the OB association environment, ejecta from supernovae might be accelerated by the high velocity WR winds on a time scale that is short compared to the half-life of 59 Ni. Thus the 59 Ni might not have time to decay and this would cast doubt upon the OB association origin of cosmic rays. In this paper we suggest a scenario that should allow much of the 59 Ni to decay in the OB association environment and conclude that the hypothesis of the OB association origin of cosmic rays appears to be viable.

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Section: Discussionmentioning

confidence: 99%

OB Associations, Wolf–Rayet Stars, and the Origin of Galactic Cosmic Rays

Binns

Wiedenbeck

Arnould³

et al. 2007

The Composition of Matter

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“…In the absence of convincing alternatives, the "superbubble paradigm" became the physical explanation for both the origin of GCR (e.g. Parizot et al 2004) and -by default -for primary Be (despite some criticism, e.g. in Prantzos 2006a).…”

Section: Introductionmentioning

confidence: 99%

Production and evolution of Li, Be, and B isotopes in the Galaxy

Prantzos

2012

A&A

164

158

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Context. We reassess the problem of the production and evolution of the light elements Li, Be and B and of their isotopes in the Milky Way in the light of new observational and theoretical developments. Aims. The main novelty is the introduction of a new scheme for the origin of Galactic cosmic rays (GCR), which for the first time enables a self-consistent calculation of their composition during galactic evolution. Methods. The scheme accounts for key features of the present-day GCR source composition, it is based on the wind yields of the Geneva models of rotating, mass-losing stars and it is fully coupled to a detailed galactic chemical evolution code. Results. We find that the adopted GCR source composition accounts naturally for the observations of primary Be and helps understanding why Be follows Fe more closely than O. We find that GCR produce ∼70% of the solar 11 B/ 10 B isotopic ratio; the remaining 30% of 11 B presumably result from ν-nucleosynthesis in massive star explosions. We find that GCR and primordial nucleosynthesis can produce at most ∼30% of solar Li. At least half of the solar Li has to originate in low-mass stellar sources (red giants, asymptotic giant branch stars, or novae), but the required average yields of those sources are found to be much higher than obtained in current models of stellar nucleosynthesis. We also present radial profiles of LiBeB elemental and isotopic abundances in the Milky Way disc. We argue that the shape of those profiles -and the late evolution of LiBeB in general -reveals important features of the production of those light elements through primary and secondary processes.

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“…What is the origin of the nonthermal emission observed in some superbubbles (Smith & Wang 2004)? Are superbubbles a relevant source for the acceleration of galactic cosmic rays (Parizot et al 2004)?…”

Section: Superbubblesmentioning

confidence: 99%