Gamow–Teller strength distributions and electron capture rates for 55Co and 56Ni

Nabi, Jameel‐Un; Rahman, Muneeb-Ur

doi:10.1016/j.physletb.2005.02.059

Cited by 37 publications

(26 citation statements)

References 28 publications

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“…Our rates are still around four times faster than shell model ones at higher densities and temperatures ([see also Ref. [30]). We calculated a 55 Co halflife of 1108 sec.…”

Section: Resultsmentioning

confidence: 60%

Electron and positron capture rates on 55Co in stellar matter

Nabi¹,

Rahman²

2007

Braz. J. Phys.

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55 Co is not only present in abundance in presupernova phase but is also advocated to play a decisive role in the core collapse of massive stars. The spectroscopy of electron capture and emitted neutrinos yields useful information on the physical conditions and stellar core composition. B(GT) values to low-lying states are calculated microscopically using the pn-QRPA theory. Our rates are enhanced compared to the reported shell model rates. The enhancement is attributed partly to the liberty of selecting a huge model space, allowing consideration of many more excited states in our rate calculations. Unlike previous calculations the so-called Brinks hypothesis is not assumed leading to a more realistic estimate of the rates. The electron and positron capture rates are calculated over a wide temperature (0.01 × 10 9 − 30 × 10 9 K) and density (10 − 10 11 gcm −3 ) grid.

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“…Our rates are still around four times faster than shell model ones at higher densities and temperatures ([see also Ref. [30]). We calculated a 55 Co halflife of 1108 sec.…”

Section: Resultsmentioning

confidence: 60%

Electron and positron capture rates on 55Co in stellar matter

Nabi¹,

Rahman²

2007

Braz. J. Phys.

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“…It can be seen from Table 1 that at low densities and temperatures the antineutrino energy loss rates due to 49,51,52,53 Ti dominate by order of magnitudes and hence more important for the collapse simulators. As T 9 [K] ∼ 30, the neutrino energy loss rates try to catch up with the antineutrino energy loss rates. At high stellar densities the story reverses with neutrino energy loss rates assuming the role of the dominant partner.…”

Section: Calculations and Resultsmentioning

confidence: 99%

Neutrino and Antineutrino Energy Loss Rates in Massive Stars Due to Isotopes of Titanium

Nabi

2010

Int. J. Mod. Phys. E

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Weak interaction rates on titanium isotopes are important during the late phases of evolution of massive stars. A search was made for key titanium isotopes from available literature and a microscopic calculation of weak rates of these nuclei were performed using the proton-neutron quasiparticle random phase approximation (pn-QRPA) theory. Earlier the author presented the stellar electron capture rates on titanium isotopes. In this paper I present the neutrino and antineutrino energy loss rates due to capture and decay rates on isotopes of titanium in stellar environment. Accurate estimate of neutrino energy loss rates are needed for the study of the late stages of the stellar evolution, in particular for cooling of neutron stars and white dwarfs. The results are also compared against previous calculations. At high stellar temperatures the calculated neutrino and antineutrino energy loss rates are bigger by more than two orders of magnitude as compared to the large scale shell model results and favor stellar cores with lower entropies. This study can prove useful for core-collapse simulators.

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“…These weak interaction rate calculations included decay rates, capture rates, neutrino energy loss rates, gamma heating rates, probabilities of β-delayed particle emissions and energy rate of these particle emissions (Nabi et al , 2004. These calculations were later refined using more efficient algorithms, incorporating latest data from mass compilations and experimental values, and by fine-tuning of model parameters (Nabi et al 2005)- ). The present work is devoted to a microscopic calculation of Gamow-Teller strength distribution and detailed analysis of the neutrino and antineutrino energy loss rates due to weak-interaction reactions on isotopes of chromium in stellar environment.…”

Section: Iron (mentioning

confidence: 99%

Gamow-Teller strength distributions and neutrino energy loss rates due to chromium isotopes in stellar matter

Nabi

Shehzadi

Fayaz

2016

Astrophys Space Sci

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Gamow-Teller transitions in isotopes of chromium play a consequential role in the presupernova evolution of massive stars. β-decay and electron capture rates on chromium isotopes significantly affect the time rate of change of lepton fraction (Ẏ e ). Finetuning of this parameter is one of the key for simulating a successful supernova explosion. The (anti)neutrinos produced as a result of electron capture and β-decay are transparent to stellar matter during presupernova phases. They carry away energy and this result in cooling the stellar core. In this paper we present the calculations of Gamow-Teller strength distributions and (anti)neutrino energy loss rates due to weak interactions on chromium isotopes of astrophysical importance. We compare our results with measured data and previous calculations wherever available.

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Gamow–Teller strength distributions and electron capture rates for 55Co and 56Ni

Cited by 37 publications

References 28 publications

Electron and positron capture rates on 55Co in stellar matter

Electron and positron capture rates on 55Co in stellar matter

Neutrino and Antineutrino Energy Loss Rates in Massive Stars Due to Isotopes of Titanium

Gamow-Teller strength distributions and neutrino energy loss rates due to chromium isotopes in stellar matter

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