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The reaction rate for the destruction of fluorine in AGB stars

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Title: The reaction rate for the destruction of fluorine in AGB stars
Authors: Ugalde, C.1, Azuma, R.2, Couture, A.1, Görres, J.1, Heil, M.3, Scheller, K.4, Stech, E.1, Tan, W.1, Wiescher, M.1
Source: Nuclear Physics A. Jul2005, Vol. 758 Issue 1-4, p577-580. 4p.
Subjects: Nuclear reactions, Chemical kinetics, Fluorine, Nuclear physics
Abstract: The 19 F(α, p)22 Ne reaction is considered to be the main source of fluorine depletion during the Asymptotic Giant Branch phase in stars. The reaction rate still retains large uncertainties due to the lack of experimental studies available. The yields for both the ground p0 and first excited state p1 exit channels of 22 Ne have been measured with the University of Notre Dame KN van de Graaff accelerator. Ten resonances were found in the energy range and their strengths have been determined. A comparison between the rate calculated from the experimental data and other standard rates is provided. [Copyright &y& Elsevier]
Copyright of Nuclear Physics A is the property of Elsevier B.V. and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
Database: Engineering Source
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Header DbId: egs
DbLabel: Engineering Source
An: 18038019
AccessLevel: 6
PubType: Academic Journal
PubTypeId: academicJournal
PreciseRelevancyScore: 0
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  Data: The reaction rate for the destruction of fluorine in AGB stars
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  Data: <searchLink fieldCode="AR" term="%22Ugalde%2C+C%2E%22">Ugalde, C.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Azuma%2C+R%2E%22">Azuma, R.</searchLink><relatesTo>2</relatesTo><br /><searchLink fieldCode="AR" term="%22Couture%2C+A%2E%22">Couture, A.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Görres%2C+J%2E%22">Görres, J.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Heil%2C+M%2E%22">Heil, M.</searchLink><relatesTo>3</relatesTo><br /><searchLink fieldCode="AR" term="%22Scheller%2C+K%2E%22">Scheller, K.</searchLink><relatesTo>4</relatesTo><br /><searchLink fieldCode="AR" term="%22Stech%2C+E%2E%22">Stech, E.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Tan%2C+W%2E%22">Tan, W.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Wiescher%2C+M%2E%22">Wiescher, M.</searchLink><relatesTo>1</relatesTo>
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  Data: <searchLink fieldCode="JN" term="%22Nuclear+Physics+A%22">Nuclear Physics A</searchLink>. Jul2005, Vol. 758 Issue 1-4, p577-580. 4p.
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  Data: <searchLink fieldCode="DE" term="%22Nuclear+reactions%22">Nuclear reactions</searchLink><br /><searchLink fieldCode="DE" term="%22Chemical+kinetics%22">Chemical kinetics</searchLink><br /><searchLink fieldCode="DE" term="%22Fluorine%22">Fluorine</searchLink><br /><searchLink fieldCode="DE" term="%22Nuclear+physics%22">Nuclear physics</searchLink>
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  Label: Abstract
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  Data: The 19 F(α, p)22 Ne reaction is considered to be the main source of fluorine depletion during the Asymptotic Giant Branch phase in stars. The reaction rate still retains large uncertainties due to the lack of experimental studies available. The yields for both the ground p0 and first excited state p1 exit channels of 22 Ne have been measured with the University of Notre Dame KN van de Graaff accelerator. Ten resonances were found in the energy range and their strengths have been determined. A comparison between the rate calculated from the experimental data and other standard rates is provided. [Copyright &y& Elsevier]
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  Data: <i>Copyright of Nuclear Physics A is the property of Elsevier B.V. and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
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