New light in nuclear physics: The extreme light infrastructure

Balabanski, D. L.; Popescu, Roxana Cristina; Stutman, D.; Tanaka, K. A.; Tešileanu, O.; Ur, C. A.; Ursescu, D.; Zamfir, N. V.

doi:10.1209/0295-5075/117/28001

Cited by 47 publications

(42 citation statements)

References 23 publications

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“…In the present work a brief summary is provided on the astrophysical motivation of γ-induced reaction studies with the activation method together with a brief account of state-of-the art γ-sources and the experimental setups relevant to activation. A special emphasis is given to the upcoming ELI-NP facility [129] opening new possibilities for the γ-induced reaction studies. Some examples will be provided as well.…”

Section: Gamma Induced Reactionsmentioning

confidence: 99%

The activation method for cross section measurements in nuclear astrophysics

et al. 2019

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The primary aim of experimental nuclear astrophysics is to determine the rates of nuclear reactions taking place in stars in various astrophysical conditions. These reaction rates are important ingredient for understanding the elemental abundance distribution in our solar system and the galaxy. The reaction rates are determined from the cross sections which need to be measured at energies as close to the astrophysically relevant ones as possible. In many cases the final nucleus of an astrophysically important reaction is radioactive which allows the cross section to be determined based on the off-line measurement of the number of produced isotopes. In general, this technique is referred to as the activation method, which often has substantial advantages over in-beam particle-or γ-detection measurements. In this paper the activation method is reviewed from the viewpoint of nuclear astrophysics. Important aspects of the activation method are given through several reaction studies for charged particle, neutron and γ-induced reactions. Various techniques for the measurement of the produced activity are detailed. As a special case of activation, the technique of Accelerator Mass Spectrometry in cross section measurements is also reviewed. PACS. 26.20.-f Hydrostatic stellar nucleosynthesis -26.30.-k Nucleosynthesis in novae, supernovae, and other explosive environments -24.10.-i Nuclear reaction models and methodsContents

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Section: Gamma Induced Reactionsmentioning

confidence: 99%

The activation method for cross section measurements in nuclear astrophysics

et al. 2019

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“…ELI-NP will benefit also from a very bright gamma beam system (GBS). The system was conceived as a dedicated device based on the inverse Compton backscattering of high-intensity laser pulses off e-mail: luca.guardo@eli-np.ro high brightness relativistic electron bunches and able to provide gamma beams with unprecedented features: continuous tuneable gamma-ray energy over a broad range (from 200 keV to 19.5MeV), high spectral density (about 10 4 photons/s/eV), small relative energy bandwidth (lower than 0.5%), high degree of linear polarization (higher than 95%), and high peak brilliance [2]. Such a facility will open new experimental perspectives for studies in the field of photonuclear physics.…”

Section: The Eli-np Facilitymentioning

confidence: 99%

Nuclear Astrophysics at ELI-NP: the ELISSA prototype tested at Laboratori Nazionali del Sud

et al. 2017

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Abstract. The Extreme Light Infrastructure-Nuclear Physics (ELI-NP) facility, under construction in Magurele near Bucharest in Romania, will provide high-intensity and high-resolution gamma ray beams that can be used to address hotly debated problems in nuclear astrophysics, such as the accurate measurements of the cross sections of the 24 Mg(γ,α) 20 Ne reaction, that is fundamental to determine the effective rate of 28 Si destruction right before the core collapse and the subsequent supernova explosion. For this purpose, a silicon strip detector array (named ELISSA, acronym for Extreme Light Infrastructure Silicon Strip Array) will be realized in a common effort by ELI-NP and Laboratori Nazionali del Sud (INFN-LNS), in order to measure excitation functions and angular distributions over a wide energy and angular range. A prototype of ELISSA was built and tested at INFN-LNS in Catania (Italy) with the support of ELI-NP. In this occasion, we have carried out experiments with alpha sources and with a 11 MeV 7 Li beam. Thanks to our approach, the first results of those tests show up a very good energy resolution (better than 1%) and very good position resolution, of the order of 1 mm. Moreover, a threshold of 150 keV can be easily achieved with no cooling.

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“…Thus, the ELI-NP laboratory opens a new dimension for nuclear physics studies with intense electromagnetic probes. The experimental program, which is under preparation at ELI-NP, targets all these experimental modes and a large variety of instruments are under construction for its realization [2, 5,6]. In this paper the emerging experimental program in the field of nuclear physics in astrophysics is described, with an emphasis of the considered day-one experiments.…”

Section: The Eli-np Facilitymentioning

confidence: 99%

Nuclear physics and astrophysics experiments at ELI-NP: The emerging future

Balabanski

2017

EPJ Web Conf.

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Abstract. The status of implementation of the ELI-NP high-power laser system and the high-brilliance gamma beam system is reported. The emerging experimental program at the facility in nuclear physics in astrophysics is discussed, with emphasis of the considered day-one experiments. The ELI-NP FacilityThe main research tools at Extreme Light Infrastructure Nuclear Physics (ELI-NP) facility are a high-power laser system (HPLS) and a high-brilliance gamma-beam system (GBS) [1]. They are superior to what is available at present in research laboratories worldwide. The mission of the facility, which will become operational in 2019 as an open access user facility, is cutting-edge research in the field of nuclear photonics. The HPLS has central wavelength of 815 nm, reaching 10 PW peak power in pulses of duration below 22 fs, with a contrast of 10 13 :1 at 100 ps and 10 9 :1 at 10 ps ahead of the pulse peak. It has two laser arms, operated by a common front-end. Each laser arm has three optical compressors, at 10 PW, 1 PW and 100 TW. The 10 PW outputs can provide pulses once per minute, the 1 PW outputs operate at 1 Hz and the 100 TW outputs -at 10 Hz. The two arms will be synchronized and experiments with any combination of pulses will be possible [2,3]. The HPLS system and the support target laboratory are placed in clean room areas.The ELI-NP GBS will provide beams in the range between 200 keV and 19.5 MeV with a bandwidth better than 0.5%, spectral density of about 10 4 photons/(eV·s) and linear polarization higher than 95%. The gamma beam will be produced by inverse Compton scattering of 515 nm green laser light, provided by 100 Hz Yb:YAG lasers, off electron beams accelerated to relativistic energies by a warm linac consisting of S-band photoinjector and C-band acceleration cavities [4]. The electrons will interact with the laser beams at two interaction points, at low and high electron beam energies, producing low (200 keV to 3.5 MeV) and high energy (3 MeV to 19.5 MeV) gamma beams. The gamma beams will be delivered along two beam lines, placed after each interaction point. The electron beam will be bunched with a frequency of 100 Hz, and each bunch will consist of a train of 32 microbunches. Laser re-circulators will be used at the interaction points to

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New light in nuclear physics: The extreme light infrastructure

Cited by 47 publications

References 23 publications

The activation method for cross section measurements in nuclear astrophysics

The activation method for cross section measurements in nuclear astrophysics

Nuclear Astrophysics at ELI-NP: the ELISSA prototype tested at Laboratori Nazionali del Sud

Nuclear physics and astrophysics experiments at ELI-NP: The emerging future

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