Why 'ksi'(1690) and 'ksi'(2120) are so narrow (2018)
- Authors:
- USP affiliated authors: TORRES, ALBERTO MARTINEZ - IF ; NAVARRA, FERNANDO SILVEIRA - IF ; NIELSEN, MARINA - IF
- Unidade: IF
- DOI: 10.1103/PhysRevD.97.034005
- Subjects: CROMODINÂMICA QUÂNTICA; QUARK; FÍSICA TEÓRICA
- Language: Inglês
- Imprenta:
- Publisher place: College, PK.
- Date published: 2018
- Source:
- Título: Physical Review D
- Volume/Número/Paginação/Ano: v. 97, n. 3, p. 034005, fev. 2018
- Este periódico é de assinatura
- Este artigo é de acesso aberto
- URL de acesso aberto
- Cor do Acesso Aberto: green
-
ABNT
KHEMCHANDANI, K. P. et al. Why 'ksi'(1690) and 'ksi'(2120) are so narrow. Physical Review D, v. fe 2018, n. 3, p. 034005, 2018Tradução . . Disponível em: https://doi.org/10.1103/PhysRevD.97.034005. Acesso em: 03 out. 2024. -
APA
Khemchandani, K. P., Hosaka, A., Nagahiro, H., Torres, A. M., Navarra, F. S., & Nielsen, M. (2018). Why 'ksi'(1690) and 'ksi'(2120) are so narrow. Physical Review D, fe 2018( 3), 034005. doi:10.1103/PhysRevD.97.034005 -
NLM
Khemchandani KP, Hosaka A, Nagahiro H, Torres AM, Navarra FS, Nielsen M. Why 'ksi'(1690) and 'ksi'(2120) are so narrow [Internet]. Physical Review D. 2018 ; fe 2018( 3): 034005.[citado 2024 out. 03 ] Available from: https://doi.org/10.1103/PhysRevD.97.034005 -
Vancouver
Khemchandani KP, Hosaka A, Nagahiro H, Torres AM, Navarra FS, Nielsen M. Why 'ksi'(1690) and 'ksi'(2120) are so narrow [Internet]. Physical Review D. 2018 ; fe 2018( 3): 034005.[citado 2024 out. 03 ] Available from: https://doi.org/10.1103/PhysRevD.97.034005 - Understanding close-lying exotic charmonia states within QCD sum rules
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- Understanding close-lying exotic charmonia states within QCD sum rules
- Update on J / 'psi' regeneration in a hadron gas
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- Production and absorption of exotic bottomonium-like states in high energy heavy ion collisions
- X, Y and Z States
- Understanding close-lying exotic charmonia states within QCD sum rules
- On the absorption and production cross sections of 'K' and 'K' POT.*'
Informações sobre o DOI: 10.1103/PhysRevD.97.034005 (Fonte: oaDOI API)
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