Galactic cosmic ray neon isotopic abundances measured by the cosmic ray isotope spectrometer (cris) on ace

Binns, W. R.; Wiedenbeck, M. E.; Christian, E. R.; Cummings, A. C.; George, Jimin; Hink, P. L.; Israel, M. H.; Klarmann, J.; Leske, R. A.; Lijowski, M.; Mewaldt, R. A.; Stone, E. C.; Rosenvinge, T. T. von; Yanasak, N. E.

doi:10.1016/s0273-1177(01)00119-3

Cited by 6 publications

(41 citation statements)

References 23 publications

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“…The abundance ratio of 22 Ne/ 20 Ne in the galactic cosmic rays (GCR) is well known to be high compared to the solar wind (SW) [1]. For neon, the solar wind (SW) is believed to best represent the composition of the pre-solar nebula [2].…”

Section: Introductionmentioning

confidence: 99%

“…Cosmic rays originating in a region of the Galaxy with metallicity that is higher than the Solar System could produce an overabundance of 22 Ne/ 20 Ne. However, this should also lead to an overabundance of the neutron-rich isotopes of Mg and Si, which has not been observed [8].…”

Section: Introductionmentioning

confidence: 99%

“…However, this should also lead to an overabundance of the neutron-rich isotopes of Mg and Si, which has not been observed [8]. Galactic chemical evolution might also play a role in the 22 Ne/ 20 Ne overabundance, since cosmic rays may represent a more recent sample of matter than solar system abundances [11].…”

Section: Introductionmentioning

confidence: 99%

“…Olive and Schramm [12] suggested that an alternative to the conclusion that the GCR 22 Ne/ 20 Ne ratio is anomalously high is that the Solar System could instead be anomalously low. Supernovae in the near vicinity of the pre-solar nebula could have injected large amounts of 20 Ne and other aparticle nuclei shortly before the solar system formed, thus making the solar system anomalous rather than the GCRs.…”

Section: Introductionmentioning

confidence: 99%

“…Soutoul and Legrain [14,15] have developed a diffusion model in which GCRs come preferentially from the inner Galaxy. The assumptions in this model are that 1) there is a gradient in the cosmic-ray density as a function of galacto-centric radius and that the density increases as one moves nearer the galactic center, 2) there is a larger gradient in the density of WR stars than for O stars as the galactocentric radius decreases [16], and 3) that these WR stars enrich the Galaxy locally in 22 Ne [17,18]. Mewaldt [19] reviews in greater detail the above models that predate his paper.…”

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confidence: 99%

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GCR neon isotopic abundances: Comparison with wolf-rayet star models and meteoritic abundances

Binns¹,

Wiedenbeck²,

Christian³

et al. 2001

AIP Conference Proceedings

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 99%

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GCR neon isotopic abundances: Comparison with wolf-rayet star models and meteoritic abundances

Binns¹,

Wiedenbeck²,

Christian³

et al. 2001

AIP Conference Proceedings

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Cosmic rays from microquasars: A narrow component to the CR spectrum?

Heinz

Sunyaev

2002

A&A

149

142

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Abstract. We propose that relativistic Galactic jets like those observed in GRS 1915+105 and GRO J1655-40 may produce a small but measurable contribution to the cosmic ray (CR) spectrum. If these jets contain cold protons and heavy ions (as in the case of SS433), it is plausible that this component will consist of a narrow spectral feature, with a mean particle energy corresponding roughly to the bulk kinetic particle energy in the beam, Γ jet m p c 2 . Based on the current estimates of Γ jet , this feature will fall into the range of 3-10 GeV. The presence of several sources with different Γ jet will lead to the superposition of several such peaks. In addition to the narrow peaks, diffusive particle acceleration should also produce a powerlaw, whose low energy cutoff at or above Γ 2 jet m p c 2 would be visible as an additional spectral feature. The large metallicities measured in several binary companions of jet sources suggest that this CR component could have an anomalous composition compared to the bulk Galactic CR spectrum. We provide estimates of the effects of adiabatic losses which are the greatest challenge to models of narrow band CR production in microquasar jets. While the total energy contained in the microquasar CR component is highly uncertain, the local CR spectrum in the vicinity of any microquasar should be severely affected. The upcoming AMS 02 experiment will be able probe the low energy CR spectrum for such components and for composition anomalies. The spectrally peculiar gamma-ray emission produced by interaction of the ISM with CRs surrounding microquasars might be detectable by GLAST. If the presence of a microquasar CR proton component can be ruled out observationally, this argument could be turned around in favor of electron-positron jets. We show that existing OSSE/GRO and future INTEGRAL data on the Galactic 511 keV line flux put interesting constraints on the particle content of microquasar jets. The process of CR production in relativistic flows inside the Galaxy is fundamentally different from the standard picture of CR production in nonrelativistic shocks in supernova remnants, because the particles injected by a relativistic flow are already relativistic, without any need for diffusive acceleration.

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New Wolf–Rayet wind yields and nucleosynthesis of Helium stars

Higgins,

Vink,

Hirschi

et al. 2024

Monthly Notices of the Royal Astronomical Society

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Strong metallicity-dependent winds dominate the evolution of core He-burning, classical Wolf-Rayet (cWR) stars, which eject both H and He-fusion products such as 14N, 12C, 16O, 19F, 22Ne and 23Na during their evolution. The chemical enrichment from cWRs can be significant. cWR stars are also key sources for neutron production relevant for the weak s-process. We calculate stellar models of cWRs at solar metallicity for a range of initial Helium star masses (12-50 $\rm M_{\odot }$), adopting recent hydrodynamical wind rates. Stellar wind yields are provided for the entire post-main sequence evolution until core O-exhaustion. While literature has previously considered cWRs as a viable source of the radioisotope 26Al, we confirm that negligible 26Al is ejected by cWRs since it has decayed to 26Mg or proton-captured to 27Al. However, in Paper I, we showed that very massive stars eject substantial quantities of 26Al, among other elements including N, Ne, and Na, already from the zero-age-main-sequence. Here, we examine the production of 19F and find that even with lower mass-loss rates than previous studies, our cWR models still eject substantial amounts of 19F. We provide central neutron densities (Nn) of a 30 $\rm M_{\odot }$ cWR compared with a 32 $\rm M_{\odot }$ post-VMS WR and confirm that during core He-burning, cWRs produce a significant number of neutrons for the weak s-process via the 22Ne(α,n)25Mg reaction. Finally, we compare our cWR models with observed [Ne/He], [C/He] and [O/He] ratios of Galactic WC and WO stars.

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Galactic cosmic ray neon isotopic abundances measured by the cosmic ray isotope spectrometer (cris) on ace

Cited by 6 publications

References 23 publications

GCR neon isotopic abundances: Comparison with wolf-rayet star models and meteoritic abundances

GCR neon isotopic abundances: Comparison with wolf-rayet star models and meteoritic abundances

Cosmic rays from microquasars: A narrow component to the CR spectrum?

New Wolf–Rayet wind yields and nucleosynthesis of Helium stars

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