Coulomb Dissociation of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">B</mml:mi></mml:mrow><mml:mprescripts /><mml:mrow /><mml:mrow><mml:mn>8</mml:mn></mml:mrow><mml:mrow /><mml:mrow /></mml:mmultiscripts></mml:mrow></mml:math>and the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">Be</mml:mi></mml:mrow><mml:mprescripts /

Motobayashi, T.; Iwasa, N.; Ando, Yoshiaki; Kurokawa, M.; Murakami, Hiroyuki; Ruan, Juanfang; Shimoura, S.; Shirato, Shoji; Inabe, N.; Ishihara, M.; Kubo, T.; Watanabe, Yasushi; Gai, M.; Hahn, K. H.; Zhao, Z.; Nakamura, Takashi; Teranishi, Takashi; Futami, Yasuyuki; Furutaka, Kazuyoshi; Delbar, Thierry

doi:10.1103/physrevlett.73.2680

Cited by 258 publications

(349 citation statements)

References 27 publications

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“…(2) The rst case (x and s 17 increase), in addition to a large value of S 33 , requires also a value of S 17 almost three times larger than the one used in the SSM: S SSM 17 = 2 2 : 4 eV barn. Should we accept the recently proposed smaller value [5], the situation would be hopeless. (3) In the second case (x and t c increase), in addition to very large value of S 33 , an increase of the central temperature by 8% is also needed.…”

Section: B Analytical Approachmentioning

confidence: 99%

“…This agreement i s a c hieved due to a combination of the following factors: the use of the data [5] which indicate that the astrophysical factor S 17 could be smaller than the standard value S 17 = 2 2 : 4 eV barn; a few percent decrease of the solar central temperature caused either by collective plasma e ects [6] or by slightly lower heavy element abundances [7]; a small increase of the astrophysical factor S 33 due to a hypothetical low-energy resonance in the reaction 3 He + 3 He, and a small decrease of the S 34 within the experimental uncertainties of the 3 He + 4 He cross section. The most important factor in reducing the boron ux, and consequently in bringing NSSM in agreement with Kamiokande, is the rst one, i.e.…”

Section: A Introductionmentioning

confidence: 99%

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LAST HOPE for an astrophysical solution to the solar neutrino problem

1996

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We discuss what appears the last hope for an astrophysical solution to the solar neutrino problem: a correlated variation of the astrophysical factors for the helium burning cross sections (S 33 and S 34 ) and either S 17 or the central temperature T c . In this context, we recognize the important role played by the CNO neutrinos. In fact, we can obtain a fair t to the experimental data only if three conditions are met simultaneously: the astrophysical factor S 33 is about 200 times what is presently estimated, the astrophysical factor S 17 is about 3 times larger and the 13 N and 15 O neutrino uxes are negligible compared to the ones predicted by standard solar models. These conditions are not supported by the present data and their correlated combination is improbable.

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Section: B Analytical Approachmentioning

confidence: 99%

Section: A Introductionmentioning

confidence: 99%

LAST HOPE for an astrophysical solution to the solar neutrino problem

1996

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“…These cross sections have also been considered to be a sum of the nuclear and Coulomb components. During recent years, the break-up of exotic halo nuclei has been investigated both theoretically and experimentally by several groups [1][2][3][4][5][6]. One of the main motivations of these studies is the possibility of determining, in selected cases, the astrophysical S-factor.…”

Section: Introductionmentioning

confidence: 99%

Target-mass dependence of the break-up of halo nuclei

et al. 2001

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Nuclear dissociation cross sections for halo nuclei have been assumed by various authors to have a A 1/3 dependence on the target mass. These cross sections have also been considered to be a sum of the nuclear and Coulomb components. During recent years, the break-up of exotic halo nuclei has been investigated both theoretically and experimentally by several groups [1][2][3][4][5][6]. One of the main motivations of these studies is the possibility of determining, in selected cases, the astrophysical S-factor. In fact, if the predominant contributions to the dissociation mechanism were due to first-order electromagnetic transitions into the continuum, the observed cross section could be related to those of the inverse photo-capture reaction process.To apply this procedure, however, it is necessary to justify the absence of a significant nuclear contribution to the relevant excitation amplitudes. To this end it has been argued that the Coulomb and nuclear break-up processes are associated with rather distinct regions of the impact parameter range. In such case Coulombnuclear interference needs not be considered and the total break-up cross section would simply be the sum

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“…There are five radiative and one proton channel open and an important contribution to the total width is the proton channel. Nonetheless, one step might use the recently developed Coulomb Dissociation Technique (CDT) of Motobayashi et al (1991Motobayashi et al ( , 1994 to remeasure the radiative part of F x . A radioactive Column 2 contains the values from Caughlan and Fowler (1988) [CF88] and columns 3 through 5 contain the log of the rates for the listed values of the width of the first resonance, , as discussed in the text.…”

Section: Discussionmentioning

confidence: 99%

Thermonuclear Reaction Rates for the $^2^4$Mg(p,\gamma)$^2^5$Al Reaction

Zaidins¹,

Langer²

1997

PASP

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ABSTRACT. There is substantial evidence that most of the material in the envelopes of some globular-cluster giants is mixed so deeply into the interior that the abundances of many of the light elements, including magnesium and aluminum, are reshuffled by proton capture before the material is returned to the envelope above. In order to understand these abundance changes we must know all of the appropriate proton-capture rates. We have recalculated the thermonuclear reaction rates, N A (av) T , for the 24 Mg(p,y) 25 Al reaction using the canonical 57 temperatures from Caughlan and Fowler (At. Data Nucl. Data Tables, 40, 283, 1988) in the range from T9 =0.004 to T9 = 10.0, where T9 is the temperature in units of 10 9 K. We have done these calculations using a range of values for the unmeasured total width, T l , of the lowest resonance, (l/2) + , in the p+ 24 Mg system. This resonance is located at 2486 keV excitation in 25 A1 and there is a large uncertainty in the value of . The rates currently used are based upon a value of T 1 =75 meV, whereas the most recently accepted experimental value is an upper limit for of 32 eV. For values of T9 <0.07 the rates are quite sensitive to this uncertain width. We discuss the consequences of this uncertainty and the need for experimental data to determine Tj. We have also found that for T9 >5.0, the recalculated rates are somewhat higher than those in Caughlan and Fowler (1988). We present our rates in tabular form.

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Coulomb Dissociation ofB8and theBe

Cited by 258 publications

References 27 publications

LAST HOPE for an astrophysical solution to the solar neutrino problem

LAST HOPE for an astrophysical solution to the solar neutrino problem

Target-mass dependence of the break-up of halo nuclei

Thermonuclear Reaction Rates for the $^2^4$Mg(p,\gamma)$^2^5$Al Reaction

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