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citations
Cited by 2,082 publications
(2,681 citation statements)
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References 300 publications
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“…As already investigated in our previous paper [15], the RSF conversion is strongly dependent on the deviation of Y e from 0.5, which is quite sensitive to the metallicities as well as the weak interaction rates adopted in the simulation of stellar evolution. The presupernova models by Woosley et al [17] (W02S and W02Z) shows the considerably different ρ(1 − 2Y e ) profile from that of the W95S model. For both models, there exists sudden drop of the ρ(1 − 2Y e ) profile at the RSF-H region, which pushes the RSF conversion rather nonadiabatic, and the expected neutrino signal was found to be different from that estimated with the W95S model.…”
Section: Resultsmentioning
confidence: 99%
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“…As already investigated in our previous paper [15], the RSF conversion is strongly dependent on the deviation of Y e from 0.5, which is quite sensitive to the metallicities as well as the weak interaction rates adopted in the simulation of stellar evolution. The presupernova models by Woosley et al [17] (W02S and W02Z) shows the considerably different ρ(1 − 2Y e ) profile from that of the W95S model. For both models, there exists sudden drop of the ρ(1 − 2Y e ) profile at the RSF-H region, which pushes the RSF conversion rather nonadiabatic, and the expected neutrino signal was found to be different from that estimated with the W95S model.…”
Section: Resultsmentioning
confidence: 99%
“…In the previous publication, we have investigated the dependence on presupernova models [15]; in the paper, we have also used recent 15M ⊙ presupernova models by Woosley et al [17] with both solar and zero metallicity (W02S and W02Z, where 'S' and 'Z' denotes solar and zero metallicity, respectively). This is because the RSF conversion [19].…”
Section: Presupernova Profilesmentioning
confidence: 99%
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“…WO stars have number abundance ratios (C+O)/He 0.62 (Kingsburgh et al 1995), initial masses M i > 40 M and WO-lifetimes of 27 000 yr to 62 000 yr, depending on initial mass and rotation on the main sequence (Meynet 2003, private communication). WO stars could very well be Gamma-Ray-Burst-associated supernova progenitors (e.g., Reeves et al 2002;Woosley et al 2002;Kaper 2003). Only three WO stars out of a total of 253 WR stars are known in the Galaxy: WR 30a (WO4+O5((f))) at d = 7.8 kpc, WR 102 (WO2) at d = 5.6 kpc, and WR 142 (WO2) at d = 1.0 kpc (van der Hucht 2001(van der Hucht , 2003, with terminal stellar wind velocities of, respectively, v ∞ = 4500, 4600, and 5500 km s −1 (Kingsburgh et al 1995), the largest wind velocities known among Population I WR stars.…”
Section: Introductionmentioning
confidence: 99%
“…A star with mass greater than 10M⊙ is believed to go through core collapse and explode to become a Type II supernova, producing either a neutron star or black hole in the core [7]. This process is important for injecting heavy elements and energy in the interstellar medium, and may play a significant role in the evolution of the host galaxy and even the dark matter halo.…”
Section: Introductionmentioning
confidence: 99%