Nucleosynthesis

Diehl, R.

doi:10.1007/978-3-662-04593-0_10

Cited by 3 publications

(3 citation statements)

References 62 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The metallicity gradient in the Galaxy is substantial enough for excess 26 Al emission to be seen from the inner Galaxy in COMPTEL data (Palacios et al 2005); 60 Fe should be more evenly distributed. When the possibility is factored in that some 60 Fe is made in SNIa (Iwamoto et al 1999), and some 26 Al in AGB stars and novae (Diehl 2001), which have a quite different history and distribution, it appears that we must expect the unexpected when the data become sufficient for a 60 Fe map to be made.…”

Section: Discussionmentioning

confidence: 99%

“…Further, they have similar half-lives (7.4 × 10 5 yr and 1.5 × 10 6 yr respectively) which are much longer than the characteristic interval between CCSN (∼100 yr). Therefore they will accumulate in the interstellar medium until a steady state is reached, and indeed this steady-state abundance of 26 Al has been detected via a flux ∼4 × 10 −4 γ cm −2 s −1 in the 1809 keV line from its β-decay (Mahoney et al 1982;Diehl 2001).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Detection of γ-ray lines from interstellar $\mathsf{^{60}}$Fe by the high resolution spectrometer SPI

Harris¹,

Knödlseder²,

Jean³

et al. 2005

A&A

View full text Add to dashboard Cite

Abstract. It is believed that core-collapse supernovae (CCSN), occurring at a rate ∼once per century, have seeded the interstellar medium with long-lived radioisotopes such as 60 Fe (half-life 1.5 Myr), which can be detected by the γ-rays emitted when they β-decay. Here we report the detection of the 60 Fe decay lines at 1173 keV and 1333 keV with fluxes 3.7 ± 1.1 × 10 −5 γ cm −2 s −1 per line, in spectra taken by the SPI spectrometer on board INTEGRAL during its first year. The same analysis applied to the 1809 keV line of 26 Al yielded a line flux ratio 60 Fe/ 26 Al = 0.11 ± 0.03. This supports the hypothesis that there is an extra source of 26 Al in addition to CCSN.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Detection of γ-ray lines from interstellar $\mathsf{^{60}}$Fe by the high resolution spectrometer SPI

Harris¹,

Knödlseder²,

Jean³

et al. 2005

A&A

View full text Add to dashboard Cite

show abstract

“…The observation of 26 Al via the 1.809 keV γray line also explains the excess of 26 Mg found in pre-solar dust grains on meteorites [2,3]. The spatial distribution of 26 Al γ-ray intensity mapped by the COMPTEL [4] and INTEGRAL [5] space missions estimate an equilibrium mass of ≈ 2 -3 solar masses of 26 Al currently present in the Milky Way, with 26 Al been accumulated in regions of star formation and co-rotating with the plane of the Galaxy.…”

Section: Introductionmentioning

confidence: 65%

Low-lying resonances in Si26 relevant for the determination of the astrophysical Al25(p,γ

et al. 2022

View full text Add to dashboard Cite

The 25 Al(p,γ) 26 Si reaction plays a key role in accurately modeling and understanding the nucleosynthesis of the long-lived radioisotope 26 Al observed throughout the Galaxy by γ-ray telescopes via the detection of its 1.809 MeV γ-ray line. The 25 Al(p,γ) 26 Si reaction is responsible for redirecting the flux of nuclear material away from the ground state of the long-lived radioisotope 26 Al ( 26 Al g ) in favor of its short-lived isomer ( 26 Al m ) which bypasses the emission of the 1.809 MeV γ-ray, but is observed in, for example, an excess of the isotopic abundance of 26 Mg in meteorites. Uncertainties in the 25 Al(p,γ) 26 Si reaction rate are dominated by the nuclear properties of low-lying proton-unbound states in 26 Si. A high-sensitivity spectroscopic study of 26 Si was performed at the John D. Fox Accelerator Laboratory at Florida State University, using a neutron/γ-ray coincidence measurement with the 24 Mg( 3 He,nγ) 26 Si reaction. The present measurement solves previous discrepancies in the existence and location of the relevant resonances in 26 Si. Furthermore, the high sensitivity of the study allowed for a direct estimate of the 3 + 3 γ-partial width. The present experimental information combined with previous works provide an updated rate of the 25 Al(p,γ) 26 Si reaction at nova temperatures.

show abstract

Journey Through Nanometals: From the Synthesis Lab to Utilization

Sharon,

Höfer

2024

Reference Module in Materials Science and Materials Engineering

View full text Add to dashboard Cite

Nucleosynthesis

Cited by 3 publications

References 62 publications

Detection of γ-ray lines from interstellar $\mathsf{^{60}}$Fe by the high resolution spectrometer SPI

Detection of γ-ray lines from interstellar $\mathsf{^{60}}$Fe by the high resolution spectrometer SPI

Low-lying resonances in Si26 relevant for the determination of the astrophysical Al25(p,γ

Journey Through Nanometals: From the Synthesis Lab to Utilization

Contact Info

Product

Resources

About