Improved astrophysical rate for the 18O(p,α)15N reaction by underground measurements

Carlo Bruno; Marialuisa Aliotta; P  Descouvemont; A. Best; Thomas Davinson; D. Bemmerer; A. Boeltzig; C. Broggini; Antonio  Caciolli; F. Cavanna; Thomas Chillery; G. F. Ciani; Piero Corvisiero; R. Depalo; Di Leva Antonino; Z Elekes; F. Ferraro; Alba  Formicola; Zs Fülöp; Giampiero Gervino; Alessandra Guglielmetti; C  Gustavino; Gy Gyürky; Gianluca Imbriani; Matthias Junker; M. Lugaro; P. Marigo; Roberto  Menegazzo; V Mossa; F R  Pantaleo; D Piatti; P  Prati; K. Stöckel; O  Straniero; F  Strieder; T  Szucs; M. P. Takács; Davide Trezzi

doi:10.1016/j.physletb.2019.01.017

Improved astrophysical rate for the 18O(p,α)15N reaction by underground measurements

Carlo Bruno, Marialuisa Aliotta, P Descouvemont, A. Best, Thomas Davinson, D. Bemmerer, A. Boeltzig, C. Broggini, Antonio Caciolli, F. Cavanna, Thomas Chillery, G. F. Ciani, Piero Corvisiero, R. Depalo, Di Leva Antonino, Z Elekes, F. Ferraro, Alba Formicola, Zs Fülöp, Giampiero GervinoAlessandra Guglielmetti, C Gustavino, Gy Gyürky, Gianluca Imbriani, Matthias Junker, M. Lugaro, P. Marigo, Roberto Menegazzo, V Mossa, F R Pantaleo, D Piatti, P Prati, K. Stöckel, O Straniero, F Strieder, T Szucs, M. P. Takács, Davide Trezzi

School of Physics and Astronomy

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Abstract / Description of output

The 18O(p,)15N reaction aects the synthesis of 15N, 18O and 19F isotopes, whose abundances can be used to probe the
nucleosynthesis and mixing processes occurring deep inside asymptotic giant branch (AGB) stars. We performed a lowbackground
direct measurement of the 18O(p,)15N reaction cross-section at the Laboratory for Underground Nuclear
Astrophysics (LUNA) from center of mass energy Ec:m: = 340 keV down to Ec:m: = 55 keV, the lowest energy measured
to date corresponding to a cross-section of less than 1 picobarn/sr. The strength of a key resonance at center of mass
energy Er = 90 keV was found to be a factor of 10 higher than previously reported. A multi-channel R-matrix analysis
of our and other data available in the literature was performed. Over a wide temperature range, T = 0:01􀀀1:00 GK, our
new astrophysical rate is both more accurate and precise than recent evaluations. Stronger constraints can now be placed
on the physical processes controlling nucleosynthesis in AGB stars with interesting consequences on the abundance of
18O in these stars and in stardust grains, specically on the production sites of oxygen-rich Group II grains.

Original language	English
Pages (from-to)	237-242
Journal	Physics Letters B
Volume	790
Early online date	17 Jan 2019
DOIs	https://doi.org/10.1016/j.physletb.2019.01.017
Publication status	Published - 10 Mar 2019

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Bruno2018_v10 (002)Accepted author manuscript, 437 KB

Marialuisa Aliotta
- m.aliottaed.acuk
- School of Physics and Astronomy - Personal Chair in Experimental Nuclear Astrophysics
Person: Academic: Research Active
Carlo Bruno
- School of Physics and Astronomy - Reader
Person: Academic: Research Active (Research Assistant)

Cite this

Bruno, C., Aliotta, M., Descouvemont, P., Best, A., Davinson, T., Bemmerer, D., Boeltzig, A., Broggini, C., Caciolli, A., Cavanna, F., Chillery, T., Ciani, G. F., Corvisiero, P., Depalo, R., Antonino, D. L., Elekes, Z., Ferraro, F., Formicola, A., Fülöp, Z., ... Trezzi, D. (2019). Improved astrophysical rate for the 18O(p,α)15N reaction by underground measurements. Physics Letters B, 790, 237-242. https://doi.org/10.1016/j.physletb.2019.01.017

@article{ab68a5aa2df047bcb6abef8b396542fe,

title = "Improved astrophysical rate for the 18O(p,α)15N reaction by underground measurements",

abstract = "The 18O(p,)15N reaction aects the synthesis of 15N, 18O and 19F isotopes, whose abundances can be used to probe thenucleosynthesis and mixing processes occurring deep inside asymptotic giant branch (AGB) stars. We performed a lowbackgrounddirect measurement of the 18O(p,)15N reaction cross-section at the Laboratory for Underground NuclearAstrophysics (LUNA) from center of mass energy Ec:m: = 340 keV down to Ec:m: = 55 keV, the lowest energy measuredto date corresponding to a cross-section of less than 1 picobarn/sr. The strength of a key resonance at center of massenergy Er = 90 keV was found to be a factor of 10 higher than previously reported. A multi-channel R-matrix analysisof our and other data available in the literature was performed. Over a wide temperature range, T = 0:01􀀀1:00 GK, ournew astrophysical rate is both more accurate and precise than recent evaluations. Stronger constraints can now be placedon the physical processes controlling nucleosynthesis in AGB stars with interesting consequences on the abundance of18O in these stars and in stardust grains, specically on the production sites of oxygen-rich Group II grains.",

author = "Carlo Bruno and Marialuisa Aliotta and P Descouvemont and A. Best and Thomas Davinson and D. Bemmerer and A. Boeltzig and C. Broggini and Antonio Caciolli and F. Cavanna and Thomas Chillery and Ciani, {G. F.} and Piero Corvisiero and R. Depalo and Antonino, {Di Leva} and Z Elekes and F. Ferraro and Alba Formicola and Zs F{\"u}l{\"o}p and Giampiero Gervino and Alessandra Guglielmetti and C Gustavino and Gy Gy{\"u}rky and Gianluca Imbriani and Matthias Junker and M. Lugaro and P. Marigo and Roberto Menegazzo and V Mossa and Pantaleo, {F R} and D Piatti and P Prati and K. St{\"o}ckel and O Straniero and F Strieder and T Szucs and Tak{\'a}cs, {M. P.} and Davide Trezzi",

year = "2019",

month = mar,

day = "10",

doi = "10.1016/j.physletb.2019.01.017",

language = "English",

volume = "790",

pages = "237--242",

journal = "Physics Letters B",

issn = "0370-2693",

publisher = "Elsevier",

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Bruno, C , Aliotta, M, Descouvemont, P, Best, A, Davinson, T, Bemmerer, D, Boeltzig, A, Broggini, C, Caciolli, A, Cavanna, F, Chillery, T, Ciani, GF, Corvisiero, P, Depalo, R, Antonino, DL, Elekes, Z, Ferraro, F, Formicola, A, Fülöp, Z, Gervino, G, Guglielmetti, A, Gustavino, C, Gyürky, G, Imbriani, G, Junker, M, Lugaro, M, Marigo, P, Menegazzo, R, Mossa, V, Pantaleo, FR, Piatti, D, Prati, P, Stöckel, K, Straniero, O, Strieder, F, Szucs, T, Takács, MP & Trezzi, D 2019, 'Improved astrophysical rate for the 18O(p,α)15N reaction by underground measurements', Physics Letters B, vol. 790, pp. 237-242. https://doi.org/10.1016/j.physletb.2019.01.017

TY - JOUR

T1 - Improved astrophysical rate for the 18O(p,α)15N reaction by underground measurements

AU - Bruno, Carlo

AU - Aliotta, Marialuisa

AU - Descouvemont, P

AU - Best, A.

AU - Davinson, Thomas

AU - Bemmerer, D.

AU - Boeltzig, A.

AU - Broggini, C.

AU - Caciolli, Antonio

AU - Cavanna, F.

AU - Chillery, Thomas

AU - Ciani, G. F.

AU - Corvisiero, Piero

AU - Depalo, R.

AU - Antonino, Di Leva

AU - Elekes, Z

AU - Ferraro, F.

AU - Formicola, Alba

AU - Fülöp, Zs

AU - Gervino, Giampiero

AU - Guglielmetti, Alessandra

AU - Gustavino, C

AU - Gyürky, Gy

AU - Imbriani, Gianluca

AU - Junker, Matthias

AU - Lugaro, M.

AU - Marigo, P.

AU - Menegazzo, Roberto

AU - Mossa, V

AU - Pantaleo, F R

AU - Piatti, D

AU - Prati, P

AU - Stöckel, K.

AU - Straniero, O

AU - Strieder, F

AU - Szucs, T

AU - Takács, M. P.

AU - Trezzi, Davide

PY - 2019/3/10

Y1 - 2019/3/10

N2 - The 18O(p,)15N reaction aects the synthesis of 15N, 18O and 19F isotopes, whose abundances can be used to probe thenucleosynthesis and mixing processes occurring deep inside asymptotic giant branch (AGB) stars. We performed a lowbackgrounddirect measurement of the 18O(p,)15N reaction cross-section at the Laboratory for Underground NuclearAstrophysics (LUNA) from center of mass energy Ec:m: = 340 keV down to Ec:m: = 55 keV, the lowest energy measuredto date corresponding to a cross-section of less than 1 picobarn/sr. The strength of a key resonance at center of massenergy Er = 90 keV was found to be a factor of 10 higher than previously reported. A multi-channel R-matrix analysisof our and other data available in the literature was performed. Over a wide temperature range, T = 0:01􀀀1:00 GK, ournew astrophysical rate is both more accurate and precise than recent evaluations. Stronger constraints can now be placedon the physical processes controlling nucleosynthesis in AGB stars with interesting consequences on the abundance of18O in these stars and in stardust grains, specically on the production sites of oxygen-rich Group II grains.

AB - The 18O(p,)15N reaction aects the synthesis of 15N, 18O and 19F isotopes, whose abundances can be used to probe thenucleosynthesis and mixing processes occurring deep inside asymptotic giant branch (AGB) stars. We performed a lowbackgrounddirect measurement of the 18O(p,)15N reaction cross-section at the Laboratory for Underground NuclearAstrophysics (LUNA) from center of mass energy Ec:m: = 340 keV down to Ec:m: = 55 keV, the lowest energy measuredto date corresponding to a cross-section of less than 1 picobarn/sr. The strength of a key resonance at center of massenergy Er = 90 keV was found to be a factor of 10 higher than previously reported. A multi-channel R-matrix analysisof our and other data available in the literature was performed. Over a wide temperature range, T = 0:01􀀀1:00 GK, ournew astrophysical rate is both more accurate and precise than recent evaluations. Stronger constraints can now be placedon the physical processes controlling nucleosynthesis in AGB stars with interesting consequences on the abundance of18O in these stars and in stardust grains, specically on the production sites of oxygen-rich Group II grains.

U2 - 10.1016/j.physletb.2019.01.017

DO - 10.1016/j.physletb.2019.01.017

M3 - Article

SN - 0370-2693

VL - 790

SP - 237

EP - 242

JO - Physics Letters B

JF - Physics Letters B

ER -

Improved astrophysical rate for the 18O(p,α)15N reaction by underground measurements

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Marialuisa Aliotta

Carlo Bruno

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