Ground-State Proton Decay of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi>Br</mml:mi><mml:mprescripts /><mml:none /><mml:mn>69</mml:mn></mml:mmultiscripts></mml:math>and Implications for the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi>Se</mml:mi><mml:mprescripts /><mml:none /><mml:mn>68</mml:mn></mml:mmultiscripts></mml:math>Astrophysical Rapid Proton-Capture Process Waiting Point

Rogers, A. M.; Famiano, M.; Lynch, W. G.; Wallace, Mark; Amorini, F.; Bazin, D.; Charity, R. J.; Delaunay, F.; Souza, R. T. de; Elson, J. M.; Gade, A.; Galaviz, D.; Goethem, van Marc-Jan; Hudan, S.; Lee, J.; Lobastov, S. P.; Lukyanov, S. M.; Matoš, M.; Mocko, M.; Schatz, H.; Shapira, D.; Sobotka, L. G.; Tsang, M. B.; Verde, G.

doi:10.1103/physrevlett.106.252503

Cited by 36 publications

(26 citation statements)

References 43 publications

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“…We note that the impact on predictions from XRB models coupled to large networks has been examined for recent measurements of particular species (most mentioned above), including: 45 Cr, 224 65 As, 225 68 Se, 226 69 Br, 227 87 Tc, 228 99 Cd, 229 105 Sb 230 and 106 Sb. 85 Recent experimental studies such as measurements of the masses of 64 Ge, 231, 232 65 As 225 (first mentioned in Wallace and Woosley 233 in connection with accreting neutron stars), 68 Se, 234, 235 69 Br, 227 and 72 Kr; 236 measurements of excited states in 66 Se; 237,238 and measurements to improve, e.g., the 23 Al(p, γ ) 24 Si 239 and 30 S(α, p) 33 Cl 240 rates have helped to address key uncertainties around waiting points in model calculations of type I XRBs. As with classical nova explosions, however, detailed results from sensitivity studies coupling a hydrodynamic model with the required network (up to at least ≈Te 26, 27 ) have not been reported, although partial and preliminary results have been presented 29,207 (as mentioned above).…”

Section: Nuclear Physics Quantities With Demonstrated Impact On Xrb Mmentioning

confidence: 99%

Classical novae and type I X-ray bursts: Challenges for the 21st century

2014

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Classical nova explosions and type I X-ray bursts are the most frequent types of thermonuclear stellar explosions in the Galaxy. Both phenomena arise from thermonuclear ignition in the envelopes of accreting compact objects in close binary star systems. Detailed observations of these events have stimulated numerous studies in theoretical astrophysics and experimental nuclear physics. We discuss observational features of these phenomena and theoretical efforts to better understand the energy production and nucleosynthesis in these explosions. We also examine and summarize studies directed at identifying nuclear physics quantities with uncertainties that significantly affect model predictions.

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Section: Nuclear Physics Quantities With Demonstrated Impact On Xrb Mmentioning

confidence: 99%

Classical novae and type I X-ray bursts: Challenges for the 21st century

2014

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“…For 67 Ge and 81 Br, where masses were previously deduced through indirect measurements, discrepancies with literature values were found. The feasibility of using this device for mass measurements of nuclides more neutron-deficient side, which have significant impact on the rp-process pathway, is discussed.have been determined experimentally, with uncertainties of 85 keV [8] and 40 keV [9], respectively. For the others, only theoretical predictions are given.…”

mentioning

confidence: 99%

“…have been determined experimentally, with uncertainties of 85 keV [8] and 40 keV [9], respectively. For the others, only theoretical predictions are given.…”

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confidence: 99%

Atomic masses of intermediate-mass neutron-deficient nuclei with relative uncertainty down to 35-ppb via multireflection time-of-flight mass spectrograph

Kimura

Ito

Kaji

et al. 2018

International Journal of Mass Spectrometry

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High-precision mass measurements of 63 Cu, 64−66 Zn, 65 Ga, 65−67 Ge, 67 As, 78,81 Br, 80 Rb, and 79 Sr were performed utilizing a multireflection time-of-flight mass spectrograph combined with the gas-filled recoil ion separator GARIS-II. In the case of 65 Ga, a mass uncertainty of 2.1 keV, corresponding to a relative precision of δm/m = 3.5 × 10 −8 , was obtained and the mass value is in excellent agreement with the 2016 Atomic Mass Evaluation. For 67 Ge and 81 Br, where masses were previously deduced through indirect measurements, discrepancies with literature values were found. The feasibility of using this device for mass measurements of nuclides more neutron-deficient side, which have significant impact on the rp-process pathway, is discussed.have been determined experimentally, with uncertainties of 85 keV [8] and 40 keV [9], respectively. For the others, only theoretical predictions are given. A recent Q-value sensitivity study pointed out that the 65 As mass uncertainty has significant impact on the light curves and the ash compositions of X-ray bursts [10].High-precision experimental mass data of nuclides near the N = Z line are also necessary for verification of the Standard Model through the unitarity of the Cabibbo-Kobayashi-Masukawa (CKM) matrix. The "corrected" Ft-values of super allowed 0 + → 0 + β + -decay between T = 1 analog states are directly related to the dominant term in the top-row sum of the CKM matrix [11]. To calculate the Ft-values, the necessary nuclear parameters are partial lifetimes of the 0 + → 0 + transition and the corresponding Q EC -values. For nuclear masses, a relative precision of δm/m 5 × 10 −8 is required. The unitarity of the CKM matrix is confirmed to the level of 1.2 × 10 −4 with the uncertainties of present nuclear data [12]. A large fraction of the nuclear uncertainty stems from the mass uncertainty of 66 As (30 keV [5]) and the ambiguity in the 70 Br mass value [12,6].Half-lives of these as-yet insufficiently studied nuclides, excluding highly proton-unbound 69 Br and 73 Rb, span from tens to hundreds of milliseconds. These short half-lives make them difficult to effectively measure with Penning traps. In contrast, the multireflection time-of-flight mass spectrograph (MRTOF-MS) has advantages, discussed below.The MRTOF-MS has been developed for both mass measurement and isobar separation techniques in recent years. Typical mass resolving power of MRTOF-MS reaches R m > 10 5 with short measurement times of less than 10 ms. MRTOF-MS have been applied for mass measurement of heavy nuclei [13,14,15] and light neutron-rich nuclei [16,17,18] in several facilities. The achieved relative mass uncertainties have so far reached the order of δm/m ∼ 10 −7 , providing measurements relevant for nuclear-structure physics and some astrophysics. However, the measurement precision reported so far from on-line MRTOF-MS measurements is not sufficient for rp-process and unitarity of CKM matrix.The SHE-mass facility at RIKEN has been constructed to enable mass measurements of super-hea...

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“…These have helped to guide recent work (e.g., Refs. [42][43][44][45][46][47][48]), including the first measurements of the masses of 65 As and 69 Br [49,50]. Knowledge of these masses is critical to understanding the (p,γ)-(γ,p) reaction rate equilibria that develop at the 64 Ge and 68 Se waiting points along the rp process and the subsequent evolution of the abundance flow beyond these nuclei.…”

Section: Nucleosynthesismentioning

confidence: 99%

Nucleosynthesis in classical nova explosions and type I X-ray bursts

Parikh¹

2013

Proceedings of XII International Symposium on Nuclei in the Cosmos — PoS(NIC XII)

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Classical nova explosions and type I X-ray bursts are the most frequent types of thermonuclear stellar explosions in the Galaxy. Both phenomena arise from thermonuclear ignition in the envelopes of accreting compact objects in close binary star systems. Detailed observations of these events have stimulated numerous studies in theoretical astrophysics and experimental nuclear physics. We briefly discuss recent theoretical efforts to understand the nucleosynthesis in these explosions, as well as experimental efforts to measure nuclear reactions and masses whose uncertainties significantly affect model predictions.

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Ground-State Proton Decay ofBr69and Implications for theSe68Astrophysical Rapid Proton-Capture Process Waiting Point

Cited by 36 publications

References 43 publications

Classical novae and type I X-ray bursts: Challenges for the 21st century

Classical novae and type I X-ray bursts: Challenges for the 21st century

Atomic masses of intermediate-mass neutron-deficient nuclei with relative uncertainty down to 35-ppb via multireflection time-of-flight mass spectrograph

Nucleosynthesis in classical nova explosions and type I X-ray bursts

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