Gamma width of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">O</mml:mi></mml:mrow><mml:mrow /><mml:mrow><mml:mi mathvariant="normal">*</mml:mi></mml:mrow><mml:mrow /><mml:mrow /><mml:mprescripts /><mml:mrow /><mml:mrow><mml:mn>14</mml:mn></mml:mrow><mml:mrow /><mml:mrow /></mml:mmultiscripts></mml:mrow></mml:math>(5.17 MeV) and the stellar<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><

Ms, Smith; Pv, Magnus; Hahn, K. I.; Rm, Curley; Pd, Parker; Tf, Wang; Ke, Rehm; Pb, Fernandez; Sj, Sanders; Garcı́a, A.; Eg, Adelberger

doi:10.1103/physrevc.47.2740

Cited by 20 publications

(10 citation statements)

References 20 publications

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“…Comparing the 14 N( 3 He,t) 14 O spectrum with the mirror 14 N(d, 2 He) 14 C spectrum from Ref. [13], we can propose J π = 1 + for the 11.239 MeV level and confirm the J π = 2 + value for the 9.751 MeV level.…”

Section: -3supporting

confidence: 72%

“…Special attention has been paid in the past to the width and excitation energy of the 5.173 MeV, J π = 1 − state because it plays an important role in the CNO cycle and the change of the CNO cycle toward the hot-CNO cycle during the evolution of massive stars [2]. Because of its astrophysical importance, the width of this level has been thoroughly investigated and its value is known with a very good accuracy [1].…”

mentioning

confidence: 99%

“…The present spectrum was compared with the one shown in Ref. [13] for the mirror experiment 14 N(d, 2 He) 14 C. If a good isospin symmetry is assumed in the A = 14 system, this peak probably corresponds to the analog state of the J π = 1 + level at 11.306 MeV in 14 C, and therefore, a spin and parity of J π = 1 + is tentatively proposed for this 11.239-MeV state. The same argument confirms the tentative assignment of J π = 2 + for the 9.751-MeV state given in Ref.…”

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confidence: 99%

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Level widths ofO14states studied in the high-resolutionN14
Negreţ
¹
,
Adachi
²
,
Berg
³

et al. 2005
Phys. Rev. C
18
1
0
0
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A 14 C( 3 He,t) 14 O experiment was performed using a 3 He beam with E = 140 MeV/nucleon. The achieved resolution of 33 keV (full width at half maximum) for the small scattering angle spectrum allowed the determination of the widths of several levels up to an excitation energy of 11.5 MeV. The width of the E x = 5.17 MeV, J π = 1 − level was in good agreement with the known value, while for other states considerably improved or new results were obtained.

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Section: -3supporting

confidence: 72%

mentioning

confidence: 99%

mentioning

confidence: 99%

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Level widths ofO14states studied in the high-resolutionN14
Negreţ
¹
,
Adachi
²
,
Berg
³

et al. 2005
Phys. Rev. C
18
1
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0
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“…1 (Montgomery 2004) shows a CV family tree, and this work involves the DN and NL branches. All classes shown in this tree are discussed in, for example, Smith (2006), Warner (2003) and Hellier (2001).…”

Section: Introductionmentioning

confidence: 99%

Atlas of tilted accretion discs and source to negative superhumps

Montgomery

2009

Monthly Notices of the Royal Astronomical Society

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Using smoothed particle hydrodynamics, we numerically simulate steady‐state accretion discs for cataclysmic variable dwarf novae systems that have a secondary‐to‐primary mass ratio 0.35 ≤q≤ 0.55. After these accretion discs have come to quasi‐equilibrium, we rotate each disc out of the orbital plane by δ= (1, 2, 3, 4, 5 or 20)° to induce negative superhumps. For accretion discs tilted 5°, we generate light curves and associated Fourier transforms for an atlas on negative superhumps and retrograde precession. Our simulation results suggest that accretion discs need to be tilted more than 3° for negative superhumps to be statistically significant. We also show that if the disc is tilted enough such that the gas stream strikes a disc face, then a dense cooling ring is generated near the radius of impact. In addition to the atlas, we study these artificially tilted accretion discs to find the source to negative superhumps. Our results suggest that the source is additional light from innermost disc annuli, and this additional light waxes and wanes with the amount of gas stream overflow received as the secondary orbits. The nodes, where the gas stream transitions from flowing over to under the disc rim (and vice versa), precess in the retrograde direction.

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“…A considerable effort has been expended in recent years to determine the parameters for the resonance. These include the direct measurements using the radioactive 13 N beam [3,4], particle transfer reactions [5,6,7,8], and…”

Section: Introductionmentioning

confidence: 99%

N13(d,n)
Li
¹
,
Yan
²
,
Liu
³

et al. 2006
Phys. Rev. C

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Abstract13 N(p, γ) 14 O is one of the key reactions in the hot CNO cycle which occurs at stellar temperatures around T 9 ≥ 0.1. Up to now, some uncertainties still exist for the direct capture component in this reaction, thus an independent measurement is of importance. In present work, the angular distribution of the 13 N(d, n) 14 O reaction at E c.m. = 8.9 MeV has been measured in inverse kinematics, for the first time. Based on the distorted wave Born approximation (DWBA) analysis, the nuclear asymptotic normalization coefficient (ANC), C 14 O 1,1/2 , for the ground state of 14 O → 13 N + p is derived to be 5.42 ± 0.48 fm −1/2 . The 13 N(p, γ) 14 O reaction is analyzed with the R-matrix approach, its astrophysical S-factors and reaction rates at energies of astrophysical relevance are then determined with the ANC. The implications of the present reaction rates on the evolution of novae are then discussed with the reaction network calculations.

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Gamma width ofO*14(5.17 MeV) and the stellar<

Cited by 20 publications

References 20 publications

Level widths ofO14states studied in the high-resolutionN14
Negreţ
¹
,
Adachi
²
,
Berg
³

et al. 2005
Phys. Rev. C
18
1
0
0
View full text Add to dashboard Cite

Level widths ofO14states studied in the high-resolutionN14
Negreţ
¹
,
Adachi
²
,
Berg
³

et al. 2005
Phys. Rev. C
18
1
0
0
View full text Add to dashboard Cite

Atlas of tilted accretion discs and source to negative superhumps

N13(d,n)
Li
¹
,
Yan
²
,
Liu
³

et al. 2006
Phys. Rev. C

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Gamma width ofO*14(5.17 MeV) and the stellar<

Cited by 20 publications

References 20 publications

Level widths ofO14states studied in the high-resolutionN14Negreţ1, Adachi2, Berg3 et al. 2005Phys. Rev. C18100View full textAdd to dashboardCite

Level widths ofO14states studied in the high-resolutionN14Negreţ1, Adachi2, Berg3 et al. 2005Phys. Rev. C18100View full textAdd to dashboardCite

Atlas of tilted accretion discs and source to negative superhumps

N13(d,n)Li1, Yan2, Liu3 et al. 2006Phys. Rev. C

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Level widths ofO14states studied in the high-resolutionN14
Negreţ
¹
,
Adachi
²
,
Berg
³

et al. 2005
Phys. Rev. C
18
1
0
0
View full text Add to dashboard Cite

Level widths ofO14states studied in the high-resolutionN14
Negreţ
¹
,
Adachi
²
,
Berg
³

et al. 2005
Phys. Rev. C
18
1
0
0
View full text Add to dashboard Cite

N13(d,n)
Li
¹
,
Yan
²
,
Liu
³

et al. 2006
Phys. Rev. C