26Al imaging details from COMPTEL

Diehl, R.; Knödlseder, J.; Bennett, K.; Bloemen, H.; Dupraz, C.; Hermsen, W.; Lichti, G.; Morris, D.; Oberlack, U.; Ryan, J. M.; Schönfelder, V.; Steinle, H.; Strong, A. W.; Varendorff, M.; Winkler, Christoph

doi:10.1016/0273-1177(94)00050-b

Cited by 59 publications

(84 citation statements)

References 6 publications

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“…VIII of this review). Similarly, the discovery of 26 Mg abundance anomalies in meteorites Ireland and Compston, 1987;Gallino et al, 1994, Hoppe et al, 1994Russell et al, 1996), and the discovery of 26 Al in the ISM of our galaxy (Mahoney et al, 1984;Share et al, 1985;MacCallum et al, 1987;von Ballmoos et al, 1987, Diehl et al, 1995 have focused a great deal of attention on the MgAl cycle. The reactions in these two cycles have been subjected to careful experimental scrutiny.…”

Section: H Burning In the Nesi Region: Laboratory Studies A Intmentioning

confidence: 96%

Synthesis of the elements in stars: forty years of progress

et al. 1997

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Forty years ago Burbidge, Burbidge, Fowler, and Hoyle combined what we would now call fragmentary evidence from nuclear physics, stellar evolution and the abundances of elements and isotopes in the solar system as well as a few stars into a synthesis of remarkable ingenuity. Their review provided a foundation for forty years of research in all of the aspects of low energy nuclear experiments and theory, stellar modeling over a wide range of mass and composition, and abundance studies of many hundreds of stars, many of which have shown distinct evidence of the processes suggested by B 2 FH. In this review we summarize progress in each of these fields with emphasis on the most recent developments. [S0034-6861(97)

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Section: H Burning In the Nesi Region: Laboratory Studies A Intmentioning

confidence: 96%

Synthesis of the elements in stars: forty years of progress

et al. 1997

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“…2, Diehl et al 1995;Knödlseder et al 1998;Plüschke et al 2001). The significance of this result is low, however, and depends upon the specific formulation of the hypothesis.…”

Section: Earlier Data and Hintsmentioning

confidence: 99%

Radioactive²⁶Al from the Scorpius-Centaurus association

Diehl

Lang

Martin

et al. 2010

A&A

129

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Context. The Scorpius-Centaurus association is the most-nearby group of massive and young stars. As nuclear-fusion products are ejected by massive stars and supernovae into the surrounding interstellar medium, the search for characteristic γ-rays from radioactivity is one way to probe the history of activity of such nearby massive stars on a My time scale through their nucleosynthesis. 26 Al decays with a radioactivity lifetime τ ∼1 My, 1809 keV γ-rays from its decay can be measured with current γ-ray telescopes. Aims. We aim to identify nucleosynthesis ejecta from the youngest subgroup of Sco-Cen stars, and interpret their location and bulk motion from 26 Al observations with INTEGRAL's γ-ray spectrometer SPI. Methods. Following earlier 26 Al γ-ray mapping with NASA's Compton observatory, we test spatial emission skymaps of 26 Al for a component which could be attributed to ejecta from massive stars in the Scorpius-Centaurus group of stars. Such a model fit of spatial distributions for large-scale and local components is able to discriminate 26 Al emission associated with Scorpius-Centaurus, in spite of the strong underlying nucleosynthesis signal from the Galaxy at large. Results. We find an 26 Al γ-ray signal above 5σ significance, which we associate with the locations of stars of the Sco-Cen group. The observed flux of 6 × 10 −5 ph cm −2 s −1 corresponds to ∼1.1 × 10 −4 M of 26 Al. This traces the nucleosynthesis ejecta of several massive stars within the past several million years. Conclusions. We confirm through direct detection of radioactive 26 Al the recent ejection of massive-star nucleosynthesis products from the Sco-Cen association. Its youngest subgroup in Upper Scorpius appears to dominate 26 Al contributions from this association. Our 26 Al signal can be interpreted as a measure of the age and richness of this youngest subgroup. We also estimate a kinematic imprint of these nearby massive-star ejecta from the bulk motion of 26 Al and compare this to other indications of Scorpius-Centaurus massive-star activity.

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“…Indeed, observations of the Galactic 1.8 MeV line by different instruments converge to a value of 4 × 10 −4 photons/cm 2 /s, which corresponds to a steady state value of 2 M of 26 Al (produced per Myr) in the interstellar medium (e.g. Diehl et al 1995;Prantzos & Diehl 1996;Diehl & Timmes 1998). The average 26 Al yield in the recent calculations of SNII is 2.5 × 10 −5 M (compared to 10 −4 M in WW95).…”

Section: Al and 60 Fe: Revised Yields And γ-Ray Line Fluxesmentioning

confidence: 99%

“…The detected flux (∼4 × 10 −4 cm −2 s −1 ) corresponds to ∼2 M of 26 Al currently present in the ISM (and produced per Myr, assuming a steady state situation). The COMPTEL instrument aboard CGRO mapped the 1.8 MeV emission in the Milky Way and found it to be irregular, with prominent "hot-spots" probably associated with the spiral arms (Diehl et al 1995). The spatial distribution of 26 Al suggests that massive stars are at its origin (Prantzos 1991(Prantzos , 1993Prantzos & Diehl 1996).…”

Section: Introductionmentioning

confidence: 99%

Radioactive $\mathsf{^{26}}$Al and $\mathsf{^{60}}$Fe in the Milky Way: Implications of the RHESSI detection of $\mathsf{^{60}}$Fe

Prantzos¹

2004

A&A

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Abstract. The recent detection of gamma-ray lines from radioactive 26 Al and 60 Fe in the Milky Way by the RHESSI satellite calls for a reassessment of the production sites of those nuclides. The observed gamma-ray line flux ratio is in agreement with calculations of nucleosynthesis in massive stars, exploding as SNII ; in the light of those results, this observation would suggest then that SNII are the major sources of 26 Al in the Milky Way, since no other conceivable source produces substantial amounts of 60 Fe. However, more recent theoretical studies find that SNII produce much higher 60 Fe/ 26 Al ratios than previously thought and, therefore, they cannot be the major 26 Al sources in the Galaxy (otherwise 60 Fe would be detected long ago, with a line flux similar to the one of 26 Al). Wolf-Rayet stars, ejecting 26 Al (but not 60 Fe) in their stellar winds, appear then as a most natural candidate. We point out, however, that this scenario faces also an important difficulty. Forthcoming results of ESA's INTEGRAL satellite, as well as consistent calculations of nucleosynthesis in massive stars (including stars of initial masses as high as 100 M and metallicities up to 3 Z ), are required to settle the issue.

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26Al imaging details from COMPTEL

Cited by 59 publications

References 6 publications

Synthesis of the elements in stars: forty years of progress

Synthesis of the elements in stars: forty years of progress

Radioactive²⁶Al from the Scorpius-Centaurus association

Radioactive $\mathsf{^{26}}$Al and $\mathsf{^{60}}$Fe in the Milky Way: Implications of the RHESSI detection of $\mathsf{^{60}}$Fe

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26Al imaging details from COMPTEL

Cited by 59 publications

References 6 publications

Synthesis of the elements in stars: forty years of progress

Synthesis of the elements in stars: forty years of progress

Radioactive26Al from the Scorpius-Centaurus association

Radioactive $\mathsf{^{26}}$Al and $\mathsf{^{60}}$Fe in the Milky Way: Implications of the RHESSI detection of $\mathsf{^{60}}$Fe

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Radioactive²⁶Al from the Scorpius-Centaurus association