Penning trap mass measurements of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi mathvariant="normal">Cd</mml:mi><mml:mprescripts /><mml:none /><mml:mrow><mml:mn>99</mml:mn><mml:mo>−</mml:mo><mml:mn>109</mml:mn></mml:mrow></mml:mmultiscripts></mml:math>with the ISOLTRAP mass spectrometer, and implications for the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>r</mml:mi><mml:mi>p</mml:mi></mml:mrow></mml:math>pr

Breitenfeldt, M.; Audi, G.; Beck, D.; Blaum, Klaus; George, Sebastian; Herfurth, F.; Herlert, A.; Kellerbauer, A.; Kluge, H.‐J.; Kowalska, M.; Lunney, D.; Naimi, S.; Neidherr, D.; Schatz, H.; Schwarz, S.; Schweikhard, L.

doi:10.1103/physrevc.80.035805

Cited by 32 publications

(17 citation statements)

References 78 publications

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“…The results reported here show that the relevant b βp are small and do not significantly affect rp-process nucleosynthesis in the A = 92-98 region. Along with recent mass measurements [54][55][56], the results presented here are an important step towards more reliable rp-process calculations in this mass region. With the β-decay properties largely pinned down, the remaining uncertainties arise from the unknown nuclear masses near the proton drip line and the untested proton capture rates in this entire region.…”

Section: Discussionmentioning

confidence: 61%

β-delayed proton emission in the100Sn region

Lorusso¹,

Becerril²,

Amthor³

et al. 2012

Phys. Rev. C

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β-delayed proton emission from nuclides in the neighborhood of 100 Sn was studied at the National Superconducting Cyclotron Laboratory. The nuclei were produced by fragmentation of a 120 MeV/nucleon 112 Sn primary beam on a Be target. Beam purification was provided by the A1900 Fragment Separator and the Radio Frequency Fragment Separator. The fragments of interest were identified and their decay was studied with the NSCL Beta Counting System (BCS) in conjunction with the Segmented Germanium Array (SeGA +1.9 −1.7 %, 1.3(5)%, 1.9(1)%, 7.5(5)% and 2.5(3)%, respectively. The b βp = 22(1)% for 101 Sn was deduced with higher precision than previously reported. The impact of the newly measured b βp values on the composition of the type-I X-ray burst ashes was studied.

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Section: Discussionmentioning

confidence: 61%

β-delayed proton emission in the100Sn region

Lorusso¹,

Becerril²,

Amthor³

et al. 2012

Phys. Rev. C

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“…Other recent relevant mass measurements have provided precise values for masses A > 80, including proton-rich isotopes of elements between Rb and I [154,[203][204][205][206][207][208] 8 . Some of these studies have been motivated in part by exploring the still-unclear maximum endpoint of nucleosynthesis in XRBs [154] or explaining the solar abundances of the light p-nuclei 92,94 Mo and 96,98 Ru through contributions from XRBs (see Section 3.3.2).…”

Section: Recent Experimental Efforts To Improve Model Predictionsmentioning

confidence: 99%

Nucleosynthesis in type I X-ray bursts

Parikh

José

Sala

et al. 2013

Progress in Particle and Nuclear Physics

111

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Type I X-ray bursts are thermonuclear explosions that occur in the envelopes of accreting neutron stars. Detailed observations of these phenomena have prompted numerous studies in theoretical astrophysics and experimental nuclear physics since their discovery over 35 years ago. In this review, we begin by discussing key observational features of these phenomena that may be sensitive to the particular patterns of nucleosynthesis from the associated thermonuclear burning. We then summarize efforts to model type I X-ray bursts, with emphasis on determining the nuclear physics processes involved throughout these bursts. We discuss and evaluate limitations in the models, particularly with regard to key uncertainties in the nuclear physics input. Finally, we examine recent, relevant experimental measurements and outline future prospects to improve our understanding of these unique environments from observational, theoretical and experimental perspectives. (A. Parikh).1 See http://www.sron.nl/∼jeanz/bursterlist.html for a list of known Galactic bursting sources. 2 Most X-ray sources are named using letters from the satellites that discovered them (e.g., 4U stands for the fourth catalogue of the satellite Uhuru, the first X-ray observatory) and numbers corresponding to their coordinates in right ascension (1820 stands for 18h20min) and declination (-30 deg) in the sky. These sources may also be named after the constellation where they are located and the order of discovery: 4U 1820-30 is also known as Sgr X-4, the fourth X-ray source discovered in the constellation Sagittarius. To complicate matters further, even within one of these naming conventions a single source may have two names. For example, the source 4U 1820-30 has been referred to in the literature as 3U 1820-30 as well.3 1 Crab = 2.4×10 −8 erg s −1 cm −2 in the 2-10 keV band.2 to 2003 [9]), and the Rossi X-ray Timing Explorer (RXTE, operating from 1995(RXTE, operating from to 2012). RXTE, with its large collecting area and capability for high temporal resolution X-ray analysis, has observed more than 1000 bursts from about 50 sources [11]. Soon after the discovery of X-ray bursting sources, it was proposed that the explosions could be powered by thermonuclear runaways on the surface of accreting neutron stars [12,13] (see Section 3.1). The discovery of the Rapid Burster in 1976 [14], with burst recurrence times as short as 10 s, complicated matters. The quick succession of flashes observed from this source seemed incompatible with the proposed mechanism, and moreover, did not match the general pattern shown by the other bursting sources. A classification of type I and type II bursts was therefore established [15], the former associated with thermonuclear flashes and the latter linked to accretion instabilities. The Rapid Burster is one of only two known sources showing type II bursts, together with the Bursting Pulsar (GRO 1744-28); furthermore, the Rapid Burster is the only source giving both type I and type II X-ray bursts [16]. Type I bursts display a sp...

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“…While much progress has been made in recent years with precision mass measurements of proton-rich nuclides using Penning traps, see, e.g., [10][11][12][13][14] and references therein, the masses of crucial nuclides for model calculations beyond A % 78 have not been measured yet. Thus, one has to rely on the extrapolations of the Atomic Mass Evaluation 2003 (AME03) [15] and on mass models.…”

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confidence: 99%

Mass Measurements of Very Neutron-Deficient Mo and Tc Isotopes and Their Impact onrpProcess Nucleosynthesis

Haettner¹,

Ackermann²,

Audi³

et al. 2011

Phys. Rev. Lett.

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The masses of ten proton-rich nuclides, including the N=Z+1 nuclides ⁸⁵Mo and ⁸⁷Tc, were measured with the Penning trap mass spectrometer SHIPTRAP. Compared to the Atomic Mass Evaluation 2003 a systematic shift of the mass surface by up to 1.6 MeV is observed causing significant abundance changes of the ashes of astrophysical x-ray bursts. Surprisingly low α separation energies for neutron-deficient Mo and Tc are found, making the formation of a ZrNb cycle in the rp process possible. Such a cycle would impose an upper temperature limit for the synthesis of elements beyond Nb in the rp process.

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Penning trap mass measurements ofCd99−109with the ISOLTRAP mass spectrometer, and implications for therppr

Cited by 32 publications

References 78 publications

β-delayed proton emission in the100Sn region

β-delayed proton emission in the100Sn region

Nucleosynthesis in type I X-ray bursts

Mass Measurements of Very Neutron-Deficient Mo and Tc Isotopes and Their Impact onrpProcess Nucleosynthesis

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