Detlef Rogalla
Ruhr University Bochum
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Featured researches published by Detlef Rogalla.
New Journal of Physics | 2011
S. Pezzagna; Detlef Rogalla; Dominik Wildanger; Jan Meijer; Alexander Zaitsev
A huge variety of optical colour centres can be found in diamond, emitting in its whole wide transparency range. Although several of these centres have been demonstrated as single-photon emitters, none of them meets all of the requirements of an ideal single-photon source. In this view, we discuss the properties of prominent optical centres, such as the nitrogen vacancy, the silicon vacancy or the so-called NE8 centre, as well as recently found centres ascribed to defects containing Ni, Si, Cr and Xe. Besides suitable intrinsic properties, it is necessary for practical applications that optical centres can be created artificially on demand. Of all known methods, only ion implantation allows for the most controlled creation of such defect centres. In this paper, we discuss how nanoscalability, that is, the nanometre placement and the deterministic creation of optical centres, can, could or cannot be achieved by the available ion implantation techniques. A fine analysis of individual optical centres is now possible, thanks to the recently developed subdiffraction optical microscopy methods.
European Physical Journal A | 2004
F. Raiola; P. Migliardi; G. Gyürky; M. Aliotta; A. Formicola; R. Bonetti; C. Broggini; L. Campajola; P. Corvisiero; H. Costantini; J. Cruz; A. D'Onofrio; Zs. Fülöp; G. Gervino; L. Gialanella; A. Guglielmetti; G. Imbriani; C. Gustavino; A.P. Jesus; M. Junker; R.W. Kavanagh; P.G. Prada Moroni; A. Ordine; J.V. Pinto; P. Prati; V. Roca; J.P. Ribeiro; Detlef Rogalla; C. Rolfs; M. Romano
Abstract:The recent observation of a large electron screening effect in the d(d, p)t reaction using a deuterated Ta target has been confirmed using somewhat different experimental approaches: Ue = 309±12 eV for the electron screening potential energy. The high Ue value arises from the environment of the deuterons in the Ta matrix, but a quantitative explanation is missing.
Physics Letters B | 2006
A. Lemut; D. Bemmerer; F. Confortola; R. Bonetti; C. Broggini; P. Corvisiero; H. Costantini; J. Cruz; A. Formicola; Zs. Fülöp; G. Gervino; A. Guglielmetti; C. Gustavino; G. Gyürky; G. Imbriani; A.P. Jesus; M. Junker; B. Limata; R. Menegazzo; P. Prati; V. Roca; Detlef Rogalla; C. Rolfs; M. Romano; C. Rossi Alvarez; F. Schümann; E. Somorjai; O. Straniero; F. Strieder; F. Terrasi
Abstract In stars with temperatures above 20 × 10 6 K , hydrogen burning is dominated by the CNO cycle. Its rate is determined by the slowest process, the 14N(p, γ)15O reaction. Deep underground in Italys Gran Sasso laboratory, at the LUNA 400 kV accelerator, the cross section of this reaction has been measured at energies much lower than ever achieved before. Using a windowless gas target and a 4π BGO summing detector, direct cross section data has been obtained down to 70 keV, reaching a value of 0.24 picobarn. The Gamow peak has been covered by experimental data for several scenarios of stable and explosive hydrogen burning. In addition, the strength of the 259 keV resonance has been remeasured. The thermonuclear reaction rate has been calculated for temperatures 90 – 300 × 10 6 K , for the first time with negligible impact from extrapolations.
European Physical Journal A | 2005
D. Bemmerer; F. Confortola; A. Lemut; R. Bonetti; C. Broggini; P. Corvisiero; H. Costantini; J. Cruz; A. Formicola; Zs. Fülöp; G. Gervino; A. Guglielmetti; C. Gustavino; Gy. Gyürky; G. Imbriani; A.P. Jesus; M. Junker; B. Limata; R. Menegazzo; P. Prati; V. Roca; Detlef Rogalla; C. Rolfs; M. Romano; C. Rossi Alvarez; F. Schümann; E. Somorjai; O. Straniero; F. Strieder; F. Terrasi
Abstract.The LUNA (Laboratory Underground for Nuclear Astrophysics) facility has been designed to study nuclear reactions of astrophysical interest. It is located deep underground in the Gran Sasso National Laboratory, Italy. Two electrostatic accelerators, with 50 and 400 kV maximum voltage, in combination with solid and gas target setups allowed to measure the total cross-sections of the radiative-capture reactions ^2H2H(p, γ)^3He3Heand ^14N14N(p, γ)^15O15Owithin their relevant Gamow peaks. We report on the gamma background in the Gran Sasso laboratory measured by germanium and bismuth germanate detectors, with and without an incident proton beam. A method to localize the sources of beam-induced background using the Doppler shift of emitted gamma rays is presented. The feasibility of radiative-capture studies at energies of astrophysical interest is discussed for several experimental scenarios.
Nuclear Physics | 2001
M. Aliotta; F. Raiola; György Gyürky; A. Formicola; R. Bonetti; C. Broggini; L. Campajola; P. Corvisiero; H. Costantini; A. D'Onofrio; Zs. Fülöp; G. Gervino; L. Gialanella; Alessandra Guglielmetti; C. Gustavino; G. Imbriani; M. Junker; P.G. Prada Moroni; A. Ordine; P. Prati; V. Roca; Detlef Rogalla; C. Rolfs; M. Romano; F. Schümann; E. Somorjai; O. Straniero; F. Strieder; F. Terrasi; H. P. Trautvetter
The cross section of the reactions 3He(d, p)4He and d(3He, p)4He has been measured at the center-of-mass energies E=5 to 60 keV and 10 to 40 keV, respectively. The experiments were performed to determine the magnitude of the electron screening effect leading to the respective electron-screening potential energy Ue=219±7 and 109±9 eV, which are both significantly higher than the respective values from atomic physics models, Ue=120 and 65 eV.
Nuclear Physics | 2001
M. Aliotta; E. Somorjai; P. Corvisiero; M. Romano; G. Imbriani; Z. S. Fulop; A. D'Onofrio; A. Guglielmetti; H. P. Trautvetter; F. Raiola; O. Straniero; G. Gervino; S. Zavatarelli; G. Gyürky; A. Ordine; C. Broggini; A. Formicola; L. Campajola; C. Rolfs; P.G. Prada Moroni; F. Strieder; M. Junker; P. Prati; Detlef Rogalla; F. Terrasi; Frank O. Schumann; L. Gialanella; R. Bonetti; V. Roca; C. Gustavino
The cross section of the reactions 3He(d, p)4He and d(3He, p)4He has been measured at the center-of-mass energies E=5 to 60 keV and 10 to 40 keV, respectively. The experiments were performed to determine the magnitude of the electron screening effect leading to the respective electron-screening potential energy Ue=219±7 and 109±9 eV, which are both significantly higher than the respective values from atomic physics models, Ue=120 and 65 eV.
Radiocarbon | 2007
Isabella Passariello; Fabio Marzaioli; Carmine Lubritto; Mauro Rubino; A. D'Onofrio; Nicola De Cesare; Gianluca Borriello; Giovanni Casa; Antonio Palmieri; Detlef Rogalla; C. Sabbarese; F. Terrasi
A system with several lines for the preparation of graphite targets for radiocarbon analysis has been built at the new accelerator mass spectrometry (AMS) facility in Caserta, Italy. Special attention has been paid in the design to the reduc- tion of background contamination during sample preparation. Here, we describe the main characteristics of these preparation lines. Results of tests performed to measure 14C background levels and isotope fractionation in several blank samples with the Caserta AMS system are presented and discussed.
European Physical Journal A | 2005
D. Schürmann; A. Di Leva; L. Gialanella; Detlef Rogalla; F. Strieder; N. De Cesare; A. D'Onofrio; G. Imbriani; R. Kunz; Carmine Lubritto; A. Ordine; V. Roca; C. Rolfs; M. Romano; F. Schümann; F. Terrasi; H. P. Trautvetter
Abstract.The total cross-section of 12C(α,γ)16O was measured for the first time by a direct and ungated detection of the 16O recoils. This measurement in inverse kinematics using the recoil mass separator ERNA in combination with a windowless He gas target allowed to collect data with high precision in the energy range E = 1.9 to 4.9 MeV. The data represent new information for the determination of the astrophysical S(E) factor.The total cross-section of 12C(α,γ)16O was measured for the first time by a direct and ungated detection of the 16O recoils. This measurement in inverse kinematics using the recoil mass separator ERNA in combination with a windowless He gas target allowed to collect data with high precision in the energy range E = 1.9 to 4.9 MeV. The data represent new information for the determination of the astrophysical S(E) factor.
Nuclear Instruments & Methods in Physics Research Section A-accelerators Spectrometers Detectors and Associated Equipment | 2002
C. Casella; H. Costantini; A. Lemut; B. Limata; D. Bemmerer; R. Bonetti; C. Broggini; L. Campajola; P. Cocconi; P. Corvisiero; J. Cruz; A. D'Onofrio; A. Formicola; Zs. Fülöp; G. Gervino; L. Gialanella; Alessandra Guglielmetti; C. Gustavino; G. Gyürky; A. Loiano; G. Imbriani; A.P. Jesus; M. Junker; P. Musico; A. Ordine; F. Parodi; M. Parolin; J.V. Pinto; P. Prati; J.P. Ribeiro
For the study of astrophysically relevant capture reactions in the underground laboratory LUNA a newsetup of high sensitivity has been implemented. The setup includes a windowless gas target, a 4p BGO summing crystal, and beam calorimeters. The setup has been recently used to measure the d(p,g) 3 He cross-section for the first time within its solar Gamowpeak, i.e. dow n to 2.5 keV c.m. energy. The features of the optimized setup are described. r 2002 Elsevier Science B.V. All rights reserved.
arXiv: Nuclear Experiment | 2005
D. Schuermann; A. Di Leva; L. Gialanella; Detlef Rogalla; F. Strieder; N. De Cesare; A. D'Onofrio; G. Imbriani; R. Kunz; Carmine Lubritto; A. Ordine; V. Roca; C. Rolfs; M. Romano; F. Schuemann; F. Terrasi; H. P. Trautvetter
Abstract.The total cross-section of 12C(α,γ)16O was measured for the first time by a direct and ungated detection of the 16O recoils. This measurement in inverse kinematics using the recoil mass separator ERNA in combination with a windowless He gas target allowed to collect data with high precision in the energy range E = 1.9 to 4.9 MeV. The data represent new information for the determination of the astrophysical S(E) factor.The total cross-section of 12C(α,γ)16O was measured for the first time by a direct and ungated detection of the 16O recoils. This measurement in inverse kinematics using the recoil mass separator ERNA in combination with a windowless He gas target allowed to collect data with high precision in the energy range E = 1.9 to 4.9 MeV. The data represent new information for the determination of the astrophysical S(E) factor.