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3. Behavior of the heliosphere over prolonged solar quiet periods by 44Ti measurements in meteorites

Author

Bonino, G., Castagnoli, G. Cini, Taricoo, C., and Bhandari, N.

Subjects
Solar magnetic field -- Research, Meteorites -- Composition -- Research, Science and technology, Composition, Research
Abstract

The heliospheric magnetic field (HMF) is controlled by solar activity, as established by measurements over the last few decades, but its characteristics when the sun was quiet for prolonged periods, such as during Gleissberg or Maunder minima, are not known. Titanium-44, produced in meteorites, provides a monitor of the galactic cosmic ray (GCR) flux and allows estimation of the modulation effect of the sun for the period 1883 to 1992. The titanium-44 activity is consistent with the expected value, but the increase, due to the last Gleissberg minimum, is four times greater than expected for a GCR modulation based solely on sunspot numbers. This result implies that the HMF was weaker than at present and as a result the GCR flux (for energy greater than 1 gigaelectron volt) was higher between 2.2 to 3.6 protons per square centimeter per second per 4π steradians at 1 to 3 astronomical units in solar cycles 12 to 15., Production of cosmogenic radioisotopes in meteorites depends on the GCR flux, which is controlled by the HMF which, in turn, depends on solar activity. GCR flux is inversely correlated with [...]

Published
1995

4. Isotopic record in a marine shallow-water core: Imprint of solar centennial cycles in the past 2 millennia

Author

G. Cini Castagnoli, Carla Taricco, and Silvia Maria Alessio

Subjects
Atmospheric Science, biology, Oscillation, Solar cycles, Aerospace Engineering, Solar–terrestrial relationships, Isotopic record, Climatic variations, Astronomy and Astrophysics, Atmospheric sciences, biology.organism_classification, Foraminifera, Waves and shallow water, Geophysics, Oceanography, Centennial, Space and Planetary Science, Period (geology), Dendrochronology, General Earth and Planetary Sciences, Singular spectrum analysis, Geology, Globigerinoides
Abstract

The δ 13 C profile of Globigerinoides ruber , measured in the GT90/3 shallow-water Ionian sea core and dated with high precision, is presented and analyzed using the Singular Spectrum Analysis and the Wavelet Transform. This time series covers the period 200–1979 AD, with a resolution of 3.87 years. The δ 13 C of foraminifera depends on the photosynthetic activity of the symbiontic algae living on the shells, strictly related to the illumination of the sea-surface. Both spectral methods, besides an 11-years oscillation in phase with the Schwabe cycle of the solar activity, show the presence of a centennial cycle that is in phase with the amplitude modulation of the sunspot number series in the last 300 years. Moreover, another climatic record, the tree ring δ 13 C of a Japanese cedar covering the time interval 125–1952 AD, shows a similar centennial oscillation and therefore suggests that this climatic variation is global and in phase with the solar activity.

Published
2005
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5. The limit to the UHE extraterrestrial neutrino flux from the observations of horizontal air showers at EAS-TOP

Author

A. Gazizov, Piero Vallania, P. L. Ghia, Veniamin Berezinsky, F. Arneodo, Marco Aglietta, P. Galeotti, O. Saavedra, L. Riccati, S. Vernetto, G. Cini, A. Chiavassa, Antonella Castellina, Pietro Antonioli, G. Mannocchi, G. Navarra, M. Iacovacci, Bruno Alessandro, B. D'Ettorre Piazzoli, C. Morello, W. Fulgione, G. C. Trinchero, L. Bergamasco, Carlotta Castagnoli, G. Di Sciascio, C. Melagrana, M., Aglietta, B., Alessandro, P., Antonioli, F., Arneodo, V. S., Berezinsky, L., Bergamasco, C., Castagnoli, A., Castellina, A., Chiavassa, G., Cini, D'ETTORRE PIAZZOLI, Benedetto, G., Disciascio, W., Fulgione, P., Galeotti, A. Z., Gazizov, P. L., Ghia, Iacovacci, Michele, G., Mannocchi, C., Melagrana, C., Morello, G., Navarra, L., Ricati, O., Saavedra, G. C., Trinchero, P., Vallania, and S., Vernetto

Subjects
Physics, Nuclear and High Energy Physics, Muon, Other Fields of Physics, Flux, Cosmic ray, Astrophysics, Radiation, Extraterrestrial life, Astrophysical neutrino, Muon flux, EASTOP, Neutrino, EAS Array, Horizontal Air Showrer, Zenith
Abstract

Extensive Air Showers at large zenith angles θ > 70° (Horizontal Air Showers, HAS) are observed at the EAS-TOP array at Campo Imperatore (Gran Sasso Laboratories). The rate of these events exceeds the one due to primary cosmic rays (at this angles) and therefore these showers have to be generated by penetrating particles. Assuming that they are produced by atmospheric muons we derived the muon flux as Fμ(> 30 TeV) = 1.1 × 10−11cm−2s−1sr−1, in good agreement with the underground measurements. The upper limits for diffuse neutrino radiation from these measurements is Iν(> 105GeV) dI ν e (E 0 )/dE ν e −18 cm −2 s −1 sr −1 GeV −1 , for the resonant ( E 0 = m W 2 2m e = 6.4 × 10 6 GeV ) neutrinos.

Published
1994
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6. Imaging of atmospheric EAS Cherenkov light at EAS-TOP

Author

B. D'Ettorre Piazzoli, L. Bergamasco, A. Campos Fauth, O. Saavedra, G. C. Trinchero, G. Cini, Marco Aglietta, S. Vernetto, Bruno Alessandro, A. Chiavassa, Piero Vallania, F. Arneodo, C. Castagnoli, C. Cattadori, G. Navarra, Antonella Castellina, P. Galeotti, L. Riccati, P. L. Ghia, G. Mannocchi, C. Morello, W. Fulgione, M., Aglietta, B., Alessandro, F., Arneodo, L., Bergamasco, A., Campos Fauth, C., Castagnoli, A., Castellina, C., Cattadori, A., Chiavassa, G., Cini, D'ETTORRE PIAZZOLI, Benedetto, W., Fulgione, P., Galeotti, P. L., Ghia, G., Mannocchi, C., Morello, G., Navarra, L., Riccati, O., Saavedra, G. C., Trinchero, P., Vallania, and S., Vernetto

Subjects
Atmospheric radiation, Physics, Photomultiplier, business.industry, Cherenkov detector, Field of view, Cosmic ray, Space radiation, law.invention, Optics, law, business, Analysis method, Cherenkov radiation
Abstract

Images of atmospheric EAS Cherenkov light have been recorded in connection with the EAS-TOP experiment. We describe the technique (based on a multianode photomultiplier Philips XP4702) and present some preliminary data analysis.

Published
1992
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7. Weekly gemcitabine plus Epirubicin as effective chemotherapy for advanced pancreatic cancer: a multicenter phase II study

Author

D Pantalone, Enrico Mini, M Scatizzi, Bruno Neri, M Turrini, G. Cini, A.S. Ribecco, Fioretto L, C Fulignati, Alessandro Quattrone, L. Doni, C. De Luca Cardillo, G Zocchi, and R Moretti

Subjects
Male, Oncology, Cancer Research, medicine.medical_specialty, medicine.drug_class, medicine.medical_treatment, gemcitabine (GEM), Phases of clinical research, Apoptosis, Adenocarcinoma, chemotherapy, Deoxycytidine, Antimetabolite, Drug Administration Schedule, Clinical, Internal medicine, Pancreatic cancer, Antineoplastic Combined Chemotherapy Protocols, medicine, Humans, Aged, Epirubicin, epirubicin (EPI), Chemotherapy, business.industry, clinical benefit, Combination chemotherapy, Middle Aged, Metastatic Pancreatic Adenocarcinoma, medicine.disease, Hematologic Diseases, Survival Analysis, Gemcitabine, Surgery, tumour response, Pancreatic Neoplasms, Treatment Outcome, Female, business, DNA Damage, medicine.drug
Abstract

The current role of chemotherapy in pancreatic carcinoma is limited, and progress in the treatment of this disease represents a significant challenge to medical oncology. The most promising drug under study is gemcitabine, a relatively new antimetabolite that represents an attractive candidate for combination chemotherapy because of its excellent side-effect profile and the absence of overlapping toxicities with other chemotherapeutic agents. Combined administration of gemcitabine and anthracyclines could result in the induction of DNA breaks that are not easily repaired by the cell's machinery, thus enhancing the apoptotic signals triggered by these lesions. Forty-four patients with locally advanced and/or metastatic pancreatic adenocarcinoma were enrolled in this multicenter study. Patients received Epirubicin 20 mg m−2 for 3 weeks followed by 1 week of rest (1 cycle) and gemcitabine 1000 mg m−2 after Epirubicin on the same day. All were assessable for toxicity and response, 11 patients responded to treatment with one complete response and 10 partial responses, for an overall response rate of 25%. Median survival was 10.9 months (range, 2–26 months). Therapy was well tolerated, with a low incidence of haematologic grade >2 toxicity. A total of 12 of 27 (44.4%) eligible patients attained a clinical benefit response. Our findings suggest that the gemcitabine-epirubicin schedule is active and well tolerated in patients with advanced pancreatic cancer. British Journal of Cancer (2002) 87, 497–501. doi:10.1038/sj.bjc.6600482 www.bjcancer.com © 2002 Cancer Research UK

Published
2002
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8. Solar and galactic cosmic-ray records of the Fermo (H) chondrite regolith breccia

Author

Narendra Bhandari, P. N. Shukla, G. Bonino, S. V. S. Murty, K. M. Suthar, R. R. Mahajan, Anil D. Shukla, Carla Taricco, and G. Cini Castagnoli

Subjects
Geophysics, Meteorite, Solar flare, Meteoroid, Space and Planetary Science, Chondrite, Breccia, Astronomy, Cosmic ray, Regolith, Parent body, Geology
Abstract

We demonstrate the presence of solar flare as well as neutron capture effects in the isotopic composition of rare gases in the Fermo regolith breccia acquired on its parent body based on the measurements of tracks, rare gases and radionuclides. The track density along a 3.2 cm long core decreases by a factor of about 6 and by more than a factor of 13 within the meteorite, indicating small (2-9 cm) and asymmetrical ablation. Rare gases show a large trapped component; the isotopic ratios, particularly 20 Ne/ 22 Ne ≅ 11 and 20 Ne/ 36 Ar = 10 are indicative of a solar component. The galactic cosmic-ray exposure age is determined to be 8.8 Ma. Activities of a dozen radionuclides ranging in half-life from 16 day 48 V to 0.73 Ma 26 Al are consistent with their expected production rates. Track, rare gas and radionuclide data show that the meteoroid was a small body (≤ 120 kg) and had a simple, one-stage exposure history to cosmic rays in the interplanetary space. However, 82 Kr and 128 Xe show an excess due to neutron irradiation on the parent body of the meteorite. The presence of solar gases and the neutron capture effects indicate several stages of irradiation on the parent asteroid. The chemical composition of Fermo confirms that it belongs to the H group of ordinary chondrites with lithic clasts having varying compositions. δ 15 N is found to be 8.3 ± 1.2%0, close to the typical values observed in H chondrites.

Published
2001
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9. Study of jet production in p–N interactions at GeV in EAS multicore events

Author

O. Saavedra, Carlotta Castagnoli, A. Castellina, F. Arneodo, Pietro Antonioli, L. Bergamasco, A. Chiavassa, P. Vallania, M. Aglietta, G. Navarra, Bruno Alessandro, P.L. Ghia, M. E. Bertaina, G.C. Trinchero, G. Di Sciascio, W. Fulgione, G. Mannocchi, G. Cini Castagnoli, L. Riccati, C. Morello, B. D'Ettore Piazzoli, M. Iacovacci, S. Vernetto, C. Vigorito, and P. Galeotti

Subjects
Mass number, Physics, Nuclear and High Energy Physics, Particle physics, Jet (fluid), Range (particle radiation), law.invention, Calorimeter, Nuclear physics, Cross section (physics), medicine.anatomical_structure, law, medicine, Rapidity, Collider, Nucleus
Abstract

The cross section for large p t jet production for transverse momentum 10≤ p t ≤20 GeV/c and rapidity 1.6≤ η ≤2.6 in p – N ( p –`air') interactions is studied from the analysis of multicore Extensive Air Showers recorded in the EAS–TOP calorimeter. The projectiles are the leading particles interacting at atmospheric depths between 250 and 480 cm −2 , the CMS energy of interaction being s ≈500 GeV. The slope of the p t distribution agrees with the expected one from the p – p collider data at the same CMS energy. The measured jet production cross section in p – N interactions with respect to p – p interactions is (dσ/dp t ) pN jet =(dσ/dp t ) p p jet ·A α with α =1.56±0.07 for A =14.7 (average mass number of `air' nuclei). Such value is compatible within the experimental uncertainties with the one obtained in p –nucleus accelerator measurements at s ≃30 GeV in the same range of transverse momentum and rapidity. No indication of increase of α with energy, i.e. of the entity of the `Cronin effect', is found.

Published
1999
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10. The EAS size spectrum and the cosmic ray energy spectrum in the region 1015–1016 eV

Author

M. E. Bertaina, P. L. Ghia, Bruno Alessandro, B. D'Ettorre Piazzoli, O. Saavedra, Piero Vallania, F. Arneodo, C. Morello, L. Bergamasco, A. Chiavassa, Antonella Castellina, G. Navarra, M. Iacovacci, P. Galeotti, Gian Carlo Trinchero, Marco Aglietta, W. Fulgione, Pietro Antonioli, S. Vernetto, G. Cini Castagnoli, Carlo Vigorito, Carlotta Castagnoli, G. Mannocchi, G. Di Sciascio, M., Aglietta, B., Alessandro, P., Antonioli, E., Arneodo, L., Bergamasco, M., Bertaina, C., Castagnoli, A., Castellina, A., Chiavassa, G. C., Castagnoli, D'ETTORRE PIAZZOLI, Benedetto, G. D., Sciascio, W., Fulgione, P., Galeotti, P. L., Ghia, Iacovacci, Michele, G., Mannocchi, C., Morello, G., Navarra, O., Saavedra, G. C., Trinchero, P., Vallania, S., Vernetto, and C., Vigorito

Subjects
Physics, Astrophysics and Astronomy, Range (particle radiation), KNEE REGION, Attenuation, Extrapolation, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Power law, Charged particle, Bin, Zenith
Abstract

The cosmic ray energy spectrum in the range E-o = 10(15)-10(16) eV (including the region of the steepening, "knee") is studied by means of the EAS-TOP array (Campo Imperatore, Gran Sasso Laboratories, atmospheric depth 820 g cm(-2)). Measurements of the electromagnetic size (N-e = total number of charged particles at the observation level) are performed as a function of zenith angle with statistical accuracies of a few percent. The change of slope of the spectrum is observed in each bin of zenith angle at size values decreasing with increasing atmospheric depth. Its attenuation is compatible with the one of shower particles (Lambda(e) = 219 +/- 3 g cm(-2)). This observation provides a consistency check, supporting a normal behaviour of showers at the break, that make plausible astrophysical interpretations based on an effect on primaries occurring at a given primary energy. The break has a "sharp" shape (i.e., within experimental errors is compatible with two intersecting power laws) that represents a constraint with which any interpretation has to match. The change of slope of the power law index reproducing the size spectrum is Delta gamma = 0.40 +/- 0.09. The derived all particle energy spectrum is in good agreement with the extrapolation of the direct measurements at low energies and with other EAS data at and above the knee. Power laws fits to the energy spectrum below and above the knee give tin units of m(-2) s(-1) sr(-1) TeV-1) S(E-o) = (3.48 +/- 0.06) x 10(-10) (E-o/2300)(-2.76+/-0.03) for 900 TeV < E-o < 2300 TeV and S(E-o) = (3.77 +/- 0.08) x 10(-11) (E-o/5000)(-3.19+/-0.06) for 5000 TeV < E-o < 10(4) TeV. The systematic uncertainties connected to the interaction model and the primary composition are discussed. (C) 1999 Elsevier Science B.V.

Published
1999
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11. The cosmic ray anisotropy at E0 > 100 TeV

Author

G.C. Trinchero, A. Castellina, C. Morello, B. D'Ettorre Piazzoli, O. Saavedra, G. Navarra, M. Iacovacci, L. Bergamasco, G. Cini Castagnoli, G. Di Sciascio, A. Chiavassa, G. Mannocchi, Carlo Vigorito, Pietro Antonioli, Carlotta Castagnoli, P. Galeotti, S. Vernetto, P.L. Ghia, W. Fulgione, M. Aglietta, M. E. Bertaina, Bruno Alessandro, F. Arneodo, and P. Vallania

Subjects
Physics, Atmospheric Science, Range (particle radiation), Phase (waves), Aerospace Engineering, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Interstellar medium, Geophysics, Amplitude, Space and Planetary Science, Sidereal time, General Earth and Planetary Sciences, Ultra-high-energy cosmic ray, Anisotropy
Abstract

The amplitude and phase of the first harmonic of the sidereal anisotropy of cosmic rays at E 0 = 2·10 14 eV have been measured by the EAS-TOP experiment (Campo Imperatore, 2005 m a.s.l., LNGS, Italy) and are respectively (at the equatorial plane): A sid = (3.73±0.57)·10 −4 ; φ sid = 1.82±0.49 h lst, with significance 6.5 s.d. The result is supported by different consistency checks. From the comparison with lower energy data, it follows that the amplitude and the phase of the cosmic ray anisotropy are constant over the energy range 10 12 – 2·10 14 eV. This implies at these energies a constant influence of the local interstellar medium on the propagation of cosmic rays.

Published
1999
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12. Galactic cosmic ray variations in the last two centuries recorded by cosmogenic 44Ti in meteorites

Author

P. Della Monica, G. Cini Castagnoli, Carla Taricco, Narendra Bhandari, and G. Bonino

Subjects
cosmic rays, meteorites, cosmogenic radionuclides, Physics, Atmospheric Science, Neutron monitor, Sunspot number, Aerospace Engineering, Astronomy, Flux, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Solar cycle, Geophysics, Meteorite, Space and Planetary Science, Magnitude (astronomy), General Earth and Planetary Sciences, Heliosphere
Abstract

We have previously shown that the very low activity of the cosmogenic 44Ti in meteorites records the galactic cosmic ray (GCR) flux over a century time-scale (Bonino et al., 1995). The heliospheric magnetic field (HMF) variations are the principal source of the GCR modulation in the heliosphere. We present here new measurements which extend our investigation over the last two centuries. The 44Ti activity at the time of fall has been obtained on the basis of the recently revised value of its half-life of 59.2 years. We basically confirm our earlier findings (Bonino et al., 1997). The 44Ti profile, with the time of fall of the meteorites, shows variations in phase in agreement with those expected. The magnitude of oscillations is ∼ 4 times higher than expected (∼ 6%) on the basis of the GCR flux over the past centuries deduced from sunspot number since 1700 and by the neutron monitor and balloon measurements in the last decades. The higher 44Ti production rate during prolonged solar quiet periods (Gleissberg minima) may imply that during these minima the HMF was weaker than during the recent minima of the 11-year solar cycle.

Published
1999
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13. The cosmic ray proton,helium and CNO fluxes in the 100 TeV energy region from TeV muons and EAS atmospheric Cherenkov light observations of MACRO and EAS-TOP

Author

G. Giannini, F. Maaroufi, Ioannis Katsavounidis, G. C. Barbarino, G. Mandrioli, N. Giglietto, G. Mancarella, J. Reynoldson, Eugenio Scapparone, M. De Vincenzi, L. Perrone, Teresa Montaruli, Gregory Tarle, L. R. Sulak, G. Battistoni, M. Cozzi, L. Patrizii, G. Cini, Hyun-Chul Kim, A. A. Grillo, V. Popa, Pietro Antonioli, F.J. Ronga, M. Ambrosio, Mario Sitta, C. Gustavino, F. Arneodo, H. Dekhissi, R. Nolty, S. Cecchini, Carlo Vigorito, A. Chiavassa, S. L. Mufson, M. Spinetti, C. Favuzzi, Donato Nicolo, M. Iacovacci, I. De Mitri, M. Vakili, R. Antolini, M. Giorgini, M. J. Longo, B. C. Choudhary, C. Satriano, G. de Cataldo, G. Navarra, C. R. Bower, R.M. Heinz, R. Caruso, E. Katsavounidis, F. Guarino, Kate Scholberg, Giuseppe Osteria, A. Marzari-Chiesa, D. Martello, E. Kearns, S. Petrera, P. Fusco, Marco Monteno, J. L. Stone, C. De Marzo, S. Valchierotti, O. Saavedra, J. Derkaoui, A. Stamerra, Vincenzo Patera, M. E. Bertaina, L. Bergamasco, C. Forti, P. Spinelli, Andrea Carlo Marini, Kael Hanson, Marco Aglietta, C. Orth, F. Loparco, R. Pazzi, Severino Angelo Maria Bussino, J. A. Musser, A. Sciubba, Np Longley, G. Giacomelli, M. Brigida, A. Baldini, P. Galeotti, C. E. Lane, O. Erriquez, Maurizio Spurio, O. Palamara, B. C. Barish, S. Vernetto, P. L. Ghia, D. Campana, C. W. Peck, G. Sirri, E. Lamanna, Tommaso Chiarusi, Alec Habig, M. Grassi, D. G. Michael, M. Carboni, A. Rainò, C. Morello, C. Bemporad, W. Fulgione, F. Cafagna, R. Steinberg, M. N. Mazziotta, Maximiliano Sioli, Yvonne Becherini, Fabrizio Cei, G. Mannocchi, A. Di Credico, S. Kyriazopoulou, P. Vallania, V. Togo, Bruno Alessandro, Roberto Bellotti, D. Levin, A. Surdo, R. C. Webb, P. Bernardini, B. D'Ettorre Piazzoli, Antonella Castellina, Annarita Margiotta, Carlotta Castagnoli, M. Calicchio, Halina Bilokon, V. Chiarella, P. Monacelli, S. Coutu, G. C. Trinchero, E. Iarocci, G. Di Sciascio, Paolo Lipari, C. W. Walter, Aglietta M., Alessandro B., Antonioli P., Arneodo F., Bergamasco L., Bertaina M., Castagnoli C., Castellina A., Chiavassa A., Cini G., D'Ettorre Piazzoli B., di Sciascio G., Fulgione W., Galeotti P., Ghia P. L., Iacovacci M., Mannocchi G., Morello C., Navarra G., Saavedra O., Stamerra A., Trinchero G. C., Valchierotti S., Vallania P., Vernetto S., Vigorito C., Ambrosio M., Antolini R., Baldini A., Barbarino G. C., Barish B. C., Battistoni G., Becherini Y., Bellotti R., Bemporad C., Bernardini P., Bilokon H., Bower C., Brigida M., Bussino S., Cafagna F., Calicchio M., Campana D., Carboni M., Caruso R., Cecchini S., Cei F., Chiarella V., Chiarusi T., Choudhary B. C., Coutu S., Cozzi M., de Cataldo G., Dekhissi H., de Marzo C., de Mitri I., Derkaoui J., de Vincenzi M., di Credico A., Erriquez O., Favuzzi C., Forti C., Fusco P., Giacomelli G., Giannini G., Giglietto N., Giorgini M., Grassi M., Grillo A., Guarino F., Gustavino C., Habig A., Hanson K., Heinz R., Iarocci E., Katsavounidis E., Katsavounidis I., Kearns E., Kim H., Kyriazopoulou S., Lamanna E., Lane C., Levin D. S., Lipari P., Longley N. P., Longo M. J., Loparco F., Maaroufi F., Mancarella G., Mandrioli G., Margiotta A., Marini A., Martello D., Marzari-Chiesa A., Mazziotta M. N., Michael D. G., Monacelli P., Montaruli T., Monteno M., Mufson S., Musser J., Nicolò D., Nolty R., Orth C., Osteria G., Palamara O., Patera V., Patrizii L., Pazzi R., Peck C. W., Perrone L., Petrera S., Popa V., Rainò A., Reynoldson J., Ronga F., Satriano C., Scapparone E., Scholberg K., Sciubba A., Sioli M., Sirri G., Sitta M., Spinelli P., Spinetti M., Spurio M., Steinberg R., Stone J. L., Sulak L. R., Surdo A., Tarlé G., Togo V., Vakili M., Walter C. W., Webb R., M., Aglietta, B., Alessandro, P., Antonioli, F., Arneodo, L., Bergamasco, M., Bertaina, C., Castagnoli, A., Castellina, A., Chiavassa, G., Cini, B., D'Ettorre Piazzoli, G., Di Sciascio, W., Fulgione, P., Galeotti, P. L., Ghia, M., Iacovacci, G., Mannocchi, C., Morello, G., Navarra, O., Saavedra, A., Stamerra, G. C., Trinchero, S., Valchierotti, P., Vallania, S., Vernetto, C., Vigorito, M., Ambrosio, R., Antolini, A., Baldini, G. C., Barbarino, B. C., Barish, G., Battistoni, Y., Becherini, R., Bellotti, C., Bemporad, Bernardini, Paolo, H., Bilokon, C., Bower, M., Brigida, S., Bussino, F., Cafagna, M., Calicchio, D., Campana, M., Carboni, R., Caruso, S., Cecchini, F., Cei, V., Chiarella, T., Chiarusi, B. C., Choudhary, S., Coutu, M., Cozzi, G., De Cataldo, H., Dekhissi, C., De Marzo, DE MITRI, Ivan, J., Derkaoui, M., De Vincenzi, A., Di Credico, O., Erriquez, C., Favuzzi, C., Forti, P., Fusco, G., Giacomelli, G., Giannini, N., Giglietto, M., Giorgini, M., Grassi, A., Grillo, F., Guarino, C., Gustavino, A., Habig, K., Hanson, R., Heinz, E., Iarocci, E., Katsavounidi, I., Katsavounidi, E., Kearn, H., Kim, S., Kyriazopoulou, E., Lamanna, C., Lane, D. S., Levin, P., Lipari, N. P., Longley, M. J., Longo, F., Loparco, F., Maaroufi, Mancarella, Giovanni, G., Mandrioli, A., Margiotta, A., Marini, Martello, Daniele, A., Marzari Chiesa, M. N., Mazziotta, D. G., Michael, P., Monacelli, T., Montaruli, M., Monteno, S., Mufson, J., Musser, D., Nicolo', R., Nolty, C., Orth, G., Osteria, O., Palamara, V., Patera, L., Patrizii, R., Pazzi, C. W., Peck, Perrone, Lorenzo, S., Petrera, V., Popa, A., Raino', J., Reynoldson, F., Ronga, C., Satriano, E., Scapparone, K., Scholberg, A., Sciubba, M., Sioli, G., Sirri, M., Sitta, P., Spinelli, M., Spinetti, M., Spurio, R., Steinberg, J. L., Stone, L. R., Sulak, A., Surdo, G., Tarle', V., Togo, M., Vakili, C. W., Walter, R., Webb, D'ETTORRE PIAZZOLI, Benedetto, Iacovacci, Michele, Aglietta, M, Alessandro, B, Antonioli, P, Arneodo, F, Bergamasco, L, Bertaina, M, Castagnoli, C, Castellina, A, Chiavassa, A, Cini, G, Piazzoli, Bd, Di Sciascio, G, Fulgione, W, Galeotti, P, Ghia, Pl, Iacovacci, M, Mannocchi, G, Morello, C, Navarra, G, Saavedra, O, Stamerra, A, Trinchero, Gc, Valchierotti, S, Vallania, P, Vernetto, S, Vigorito, C, Ambrosio, M, Antolini, R, Baldini, A, Barbarino, Gc, Barish, Bc, Battistoni, G, Becherini, Y, Bellotti, R, Bemporad, C, Bernardini, P, Bilokon, H, Bower, C, Brigida, M, Bussino, Severino Angelo Maria, Cafagna, F, Calicchio, M, Campana, D, Carboni, M, Caruso, R, Cecchini, S, Cei, F, Chiarella, V, Chiarusi, T, Choudhary, Bc, Coutu, S, Cozzi, M, De Cataldo, G, Dekhissi, H, De Marzo, C, De Mitri, I, Derkaoui, J, De Vincenzi, M, Di Credico, A, Erriquez, O, Favuzzi, C, Forti, C, Fusco, P, Giacomelli, G, Giannini, G, Giglietto, N, Giorgini, M, Grassi, M, Grillo, A, Guarino, F, Gustavino, C, Habig, A, Hanson, K, Heinz, R, Iarocci, E, Katsavounidis, E, Katsavounidis, I, Kearns, E, Kim, H, Kyriazopoulou, S, Lamanna, E, Lane, C, Levin, D, Lipari, P, Longley, Np, Longo, Mj, Loparco, F, Maaroufi, F, Mancarella, G, Mandrioli, G, Margiotta, A, Marini, A, Martello, D, Marzari Chiesa, A, Mazziotta, Mn, Michael, Dg, Monacelli, P, Montaruli, T, Monteno, M, Mufson, S, Musser, J, Nicolo, D, Nolty, R, Orth, C, Osteria, G, Palamara, O, Patera, V, Patrizii, L, Pazzi, R, Peck, Cw, Perrone, L, Petrera, S, Popa, V, Raino, A, Reynoldson, J, Ronga, F, Satriano, C, Scapparone, E, Scholberg, K, Sciubba, A, Sioli, M, Sirri, G, Sitta, M, Spinelli, P, Spinetti, M, Spurio, M, Steinberg, R, Stone, Jl, Sulak, Lr, Surdo, A, Tarle, G, Togo, V, Vakili, M, Walter, Cw, Webb, R., Guarino, Fausto, Barbarino, Giancarlo, Macro, and EAS TOP, Collaborations

Subjects
Proton, EAS-TOP, Astrophysics::High Energy Astrophysical Phenomena, Hadron, chemistry.chemical_element, Cosmic ray, MACRO, Nuclear physics, Raggi cosmici, cosmic rays, Cosmic rays, composition, high energies, extensive air showers, underground muons, Cherenkov radiation, Helium, Astroparticle physics, Physics, Muon, Cherenkov detectors, Astronomy and Astrophysics, Sciami estesi, chemistry, Muoni sotterranei, Physics::Accelerator Physics, High Energy Physics::Experiment, Nucleon, Composizione
Abstract

The primary cosmic ray (CR) proton, helium and CNO fluxes in the energy range 80-300 TeV are studied at the National Gran Sasso Laboratories by means of EAS-TOP (Campo Imperatore, 2005 m a.s.l.) and MACRO (deep underground, 3100 m w.e., the surface energy threshold for a muon reaching the detector being E-mu(th) approximate to 1.3 TeV). The measurement is based on: (a) the selection of primaries based on their energy/nucleon (i.e., with energy/nucleon sufficient to produce a muon with energy larger than 1.3 TeV) and the reconstruction of the shower geometry by means of the muons recorded by MACRO in the deep underground laboratories; (b) the detection of the associated atmospheric Cherenkov light (C.l.) signals by means of the C.l. detector of EAS-TOP. The C.l. density at core distance r > 100 m is directly related to the total primary energy E-0. Proton and helium ("p + He") and proton, helium and CNO ("p + He + CNO") primaries are thus selected at E-0 approximate to 80 TeV, and at E-0 similar or equal to 250 TeV, respectively. Their flux is measured: J(p+He)(80 TeV) = (1.8 +/- 0.4) x 10(-6) m(-1)-s(-1) sr(-1) TeV-1, and J(p+He+CNO)(250 TeV) = (1.1 +/- 0.3) x 10(-7) m(-2)-s(-1) sr(-1) TeV-1, their relative weights being J(p+He)(J(p+He+CNO)) over bar (250 TeV) = 0.78 +/- 0.17. By using the measurements of the proton spectrum obtained from the direct experiments and hadron flux data in the atmosphere, we obtain for the relative weights of the three components at 250 TeV: J(p) : J(He) : J(CNO) = (0.20 +/- 0.08) : (0.58 +/- 0.19) : (0.22 +/- 0.17). This corresponds to the dominance of helium over proton primaries at 100-1000 TeV, and a possible non-negligible contribution from CNO. The lateral distribution of Cherenkov light in Extensive Air Showers (EASs), which is related to the rate of energy deposit of the primary in the atmosphere, is measured for a selected proton and helium primary beam, and good agreement is found when compared with the one calculated with the CORSIKA/QGSJET simulation model. (C) 2004 Elsevier B.V. All rights reserved.

Published
2004

14. The cosmic ray proton, helium and CNO fluxes in the 100-TeV energy region from TeV muons and EAS atmospheric Cherenkov light observations of MACRO and EAS-TOP

Author

M. AGLIETTA, B. ALESSANDRO, P. ANTONIOLI, F. ARNEODO, L. BERGAMASCO, M. BERTAINA, C. CASTAGNOLI, A. CASTELLINA, A. CHIAVASSA, G. CINI CASTAGNOLI, B. D'ETTORRE PIAZZOLI, G. DI SCIASCIO, W. FULGIONE, P. GALEOTTI, P. L. GHIA, M. IACOVACCI, G. MANNOCCHI, C. MORELLO, G. NAVARRA, O. SAAVEDRA, A. STAMERRA, G. C. TRINCHERO, S. VALCHIEROTTI, P. VALLANIA, S. VERNETTO, C. VIGORITO, M. AMBROSIO, R. ANTOLINI, A. BALDINI, G. C. BARBARINO, B. C. BARISH, G. BATTISTONI, Y. BECHERINI, R. BELLOTTI, C. BEMPORAD, P. BERNARDINI, H. BILOKON, C. BOWER, M. BRIGIDA, BUSSINO, Severino Angelo Maria, F. CAFAGNA, M. CALICCHIO, D. CAMPANA, M. CARBONI, R. CARUSO, S. CECCHINI, F. CEI, V. CHIARELLA, T. CHIARUSI, B. C. CHOUDHARY, S. COUTU, M. COZZI, G. DE CATALDO, H. DEKHISSI, C. DE MARZO, I. DE MITRI, J. DERKAOUI, A. DI CREDICO, O. ERRIQUEZ, C. FAVUZZI, C. FORTI, P. FUSCO, G. GIACOMELLI, G. GIANNINI, N. GIGLIETTO, M. GIORGINI, M. GRASSI, A. GRILLO, F. GUARINO, C. GUSTAVINO, ALEC HABIG, K. HANSON, R. HEINZ, E. IAROCCI, E. KATSAVOUNIDIS, I. KATSAVOUNIDIS, E. KEARNS, H. KIM, S. KYRIAZOPOULOU, E. LAMANNA, CHARLES E. LANE, D. S. LEVIN, P. LIPARI, N. P. LONGLEY, M. J. LONGO, F. LOPARCO, F. MAAROUFI, G. MANCARELLA, G. MANDRIOLI, A. MARGIOTTA, A. MARINI, D. MARTELLO, A. MARZARI CHIESA, M. N. MAZZIOTTA, D. G. MICHAEL, P. MONACELLI, T. MONTARULI, M. MONTENO, STUART L. MUFSON, J. MUSSER, D. NICOLO, R. NOLTY, C. ORTH, G. OSTERIA, O. PALAMARA, V. PATERA, L. PATRIZII, R. PAZZI, C. W. PECK, L. PERRONE, S. PETRERA, V. POPA, A. RAINO, J. REYNOLDSON, F. RONGA, C. SATRIANO, E. SCAPPARONE, K. SCHOLBERG, A. SCIUBBA, M. SIOLI, G. SIRRI, M. SITTA, P. SPINELLI, M. SPINETTI, M. SPURIO, R. STEINBERG, J. L. STONE, L. R. SULAK, A. SURDO, G. TARLE, V. TOGO, M. VAKILI, C. W. WALTER, R. WEBB, DE VINCENZI, Mario, M., Aglietta, B., Alessandro, P., Antonioli, F., Arneodo, L., Bergamasco, M., Bertaina, C., Castagnoli, A., Castellina, A., Chiavassa, G., CINI CASTAGNOLI, B., D'ETTORRE PIAZZOLI, G., DI SCIASCIO, W., Fulgione, P., Galeotti, P. L., Ghia, M., Iacovacci, G., Mannocchi, C., Morello, G., Navarra, O., Saavedra, A., Stamerra, G. C., Trinchero, S., Valchierotti, P., Vallania, S., Vernetto, C., Vigorito, M., Ambrosio, R., Antolini, A., Baldini, G. C., Barbarino, B. C., Barish, G., Battistoni, Y., Becherini, R., Bellotti, C., Bemporad, P., Bernardini, H., Bilokon, C., Bower, M., Brigida, Bussino, Severino Angelo Maria, F., Cafagna, M., Calicchio, D., Campana, M., Carboni, R., Caruso, S., Cecchini, F., Cei, V., Chiarella, T., Chiarusi, B. C., Choudhary, S., Coutu, M., Cozzi, G., DE CATALDO, H., Dekhissi, C., DE MARZO, I., DE MITRI, J., Derkaoui, DE VINCENZI, Mario, A., DI CREDICO, O., Erriquez, C., Favuzzi, C., Forti, P., Fusco, G., Giacomelli, G., Giannini, N., Giglietto, M., Giorgini, M., Grassi, A., Grillo, F., Guarino, C., Gustavino, Alec, Habig, K., Hanson, R., Heinz, E., Iarocci, E., Katsavounidi, I., Katsavounidi, E., Kearn, H., Kim, S., Kyriazopoulou, E., Lamanna, CHARLES E., Lane, D. S., Levin, P., Lipari, N. P., Longley, M. J., Longo, F., Loparco, F., Maaroufi, G., Mancarella, G., Mandrioli, A., Margiotta, A., Marini, D., Martello, A., MARZARI CHIESA, M. N., Mazziotta, D. G., Michael, P., Monacelli, T., Montaruli, M., Monteno, STUART L., Mufson, J., Musser, D., Nicolo, R., Nolty, C., Orth, G., Osteria, O., Palamara, V., Patera, L., Patrizii, R., Pazzi, C. W., Peck, L., Perrone, S., Petrera, V., Popa, A., Raino, J., Reynoldson, F., Ronga, C., Satriano, E., Scapparone, K., Scholberg, A., Sciubba, M., Sioli, G., Sirri, M., Sitta, P., Spinelli, M., Spinetti, M., Spurio, R., Steinberg, J. L., Stone, L. R., Sulak, A., Surdo, G., Tarle, V., Togo, M., Vakili, C. W., Walter, and R., Webb

Subjects
Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Experiment
Abstract

The primary cosmic ray (CR) proton, helium and CNO fluxes in the energy range 80-300 TeV are studied at the National Gran Sasso Laboratories by means of EAS-TOP (Campo Imperatore, 2005 m a.s.l.) and MACRO (deep underground, 3100 m w.e., the surface energy threshold for a muon reaching the detector being Eμth~1.3 TeV). The measurement is based on: (a) the selection of primaries based on their energy/nucleon (i.e., with energy/nucleon sufficient to produce a muon with energy larger than 1.3 TeV) and the reconstruction of the shower geometry by means of the muons recorded by MACRO in the deep underground laboratories; (b) the detection of the associated atmospheric Cherenkov light (C.l.) signals by means of the C.l. detector of EAS-TOP. The C.l. density at core distance r>100 m is directly related to the total primary energy E0. Proton and helium (``p+He'') and proton, helium and CNO (``p+He+CNO'') primaries are thus selected at E0~=80 TeV, and at E0~=250 TeV, respectively. Their flux is measured: Jp+He(80TeV)=(1.8+/-0.4)×10-6 m-2s-1sr-1TeV-1, and Jp+He+CNO(250TeV)=(1.1+/-0.3)×10-7 m-2s-1sr-1TeV-1, their relative weights being: Jp+He/Jp+He+CNO(250TeV)=0.78+/-0.17. By using the measurements of the proton spectrum obtained from the direct experiments and hadron flux data in the atmosphere, we obtain for the relative weights of the three components at 250 TeV: Jp:JHe:JCNO=(0.20+/-0.08):(0.58+/-0.19):(0.22+/-0.17). This corresponds to the dominance of helium over proton primaries at 100-1000 TeV, and a possible non-negligible contribution from CNO. The lateral distribution of Cherenkov light in Extensive Air Showers (EASs), which is related to the rate of energy deposit of the primary in the atmosphere, is measured for a selected proton and helium primary beam, and good agreement is found when compared with the one calculated with the CORSIKA/QGSJET simulation model.

Published
2004

15. The Primary cosmic ray composition between 10**15 and 10**16 eV from extensive air showers electromagnetic and TeV muon data

Author

M. AGLIETTA, B. ALESSANDRO, P. ANTONIOLI, F. ARNEODO, L. BERGAMASCO, M. BERTAINA, C. CASTAGNOLI, A. CASTELLINA, A. CHIAVASSA, G. CINI, B. D'ETTORRE PIAZZOLI, G. DI SCIASCIO, W. FULGIONE, P. GALEOTTI, P. L. GHIA, M. IACOVACCI, G. MANNOCCHI, C. MORELLO, G. NAVARRA, O. SAAVEDRA, A. STAMERRA, G. C. TRINCHERO, S. VALCHIEROTTI, P. VALLANIA, S. VERNETTO, C. VIGORITO, M. AMBROSIO, R. ANTOLINI, A. BALDINI, G. C. BARBARINO, B. C. BARISH, GIUESEPP BATTISTONI, R. BELLOTTI, C. BEMPORAD, P. BERNARDINI, H. BILOKON, C. BLOISE, C. BOWER, M. BRIGIDA, F. CAFAGNA, D. CAMPANA, M. CARBONI, S. CECCHINI, F. CEI, B. C. CHOUDHARY, S. COUTU, G. DE CATALDO, H. DEKHISSI, C. DE MARZO, I. DE MITRI, A. DI CREDICO, C. FORTI, P. FUSCO, G. GIACOMELLI, G. GIANNINI, N. GIGLIETTO, M. GIORGINI, M. GRASSI, A. GRILLO, C. GUSTAVINO, ALEC HABIG, K. HANSON, R. HEINZ, E. IAROCCI, E. KATSAVOUNIDIS, I. KATSAVOUNIDIS, E. KEARNS, H. KIM, S. KYRIAZOPOULOU, E. LAMANNA, CHARLES E. LANE, D. S. LEVIN, P. LIPARI, M. J. LONGO, F. LOPARCO, F. MAAROUFI, G. MANCARELLA, G. MANDRIOLI, A. MARGIOTTA, A. MARINI, D. MARTELLO, A. MARZARI CHIESA, M. N. MAZZIOTTA, D. G. MICHAEL, P. MONACELLI, T. MONTARULI, M. MONTENO, STUART L. MUFSON, J. MUSSER, D. NICOLO, R. NOLTY, C. ORTH, G. OSTERIA, O. PALAMARA, V. PATERA, L. PATRIZII, R. PAZZI, C. W. PECK, L. PERRONE, S. PETRERA, V. POPA, A. RAINO, J. REYNOLDSON, F. RONGA, C. SATRIANO, E. SCAPPARONE, K. SCHOLBERG, A. SCIUBBA, M. SIOLI, M. SITTA, P. SPINELLI, M. SPINETTI, M. SPURIO, R. STEINBERG, J. L. STONE, L. R. SULAK, A. SURDO, G. TARLE, V. TOGO, M. VAKILI, C. W. WALTER, R. WEBB, DE VINCENZI, Mario, M., Aglietta, B., Alessandro, P., Antonioli, F., Arneodo, L., Bergamasco, M., Bertaina, C., Castagnoli, A., Castellina, A., Chiavassa, G., Cini, B., D'ETTORRE PIAZZOLI, G., DI SCIASCIO, W., Fulgione, P., Galeotti, P. L., Ghia, M., Iacovacci, G., Mannocchi, C., Morello, G., Navarra, O., Saavedra, A., Stamerra, G. C., Trinchero, S., Valchierotti, P., Vallania, S., Vernetto, C., Vigorito, M., Ambrosio, R., Antolini, A., Baldini, G. C., Barbarino, B. C., Barish, Giuesepp, Battistoni, R., Bellotti, C., Bemporad, P., Bernardini, H., Bilokon, C., Bloise, C., Bower, M., Brigida, F., Cafagna, D., Campana, M., Carboni, S., Cecchini, F., Cei, B. C., Choudhary, S., Coutu, G., DE CATALDO, H., Dekhissi, C., DE MARZO, I., DE MITRI, DE VINCENZI, Mario, A., DI CREDICO, C., Forti, P., Fusco, G., Giacomelli, G., Giannini, N., Giglietto, M., Giorgini, M., Grassi, A., Grillo, C., Gustavino, Alec, Habig, K., Hanson, R., Heinz, E., Iarocci, E., Katsavounidi, I., Katsavounidi, E., Kearn, H., Kim, S., Kyriazopoulou, E., Lamanna, CHARLES E., Lane, D. S., Levin, P., Lipari, M. J., Longo, F., Loparco, F., Maaroufi, G., Mancarella, G., Mandrioli, A., Margiotta, A., Marini, D., Martello, A., MARZARI CHIESA, M. N., Mazziotta, D. G., Michael, P., Monacelli, T., Montaruli, M., Monteno, STUART L., Mufson, J., Musser, D., Nicolo, R., Nolty, C., Orth, G., Osteria, O., Palamara, V., Patera, L., Patrizii, R., Pazzi, C. W., Peck, L., Perrone, S., Petrera, V., Popa, A., Raino, J., Reynoldson, F., Ronga, C., Satriano, E., Scapparone, K., Scholberg, A., Sciubba, M., Sioli, M., Sitta, P., Spinelli, M., Spinetti, M., Spurio, R., Steinberg, J. L., Stone, L. R., Sulak, A., Surdo, G., Tarle, V., Togo, M., Vakili, C. W., Walter, and R., Webb

Published
2004

16. Heliospheric modulation of cosmic rays during prolonged solar minima deduced from cosmogenic radioisotopes in meteorites

Author

G. Bonino, Narendra Bhandari, Carla Taricco, and G. Cini Castagnoli

Subjects
Physics, Atmospheric Science, Aerospace Engineering, Astronomy, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Meteorites, cosmic rays, solar activity, Geophysics, Meteorite, Space and Planetary Science, General Earth and Planetary Sciences, Heliosphere, Production rate
Abstract

Production of cosmogenic radioisotopes in meteorites depends on the galactic cosmic ray flux, which is controlled by the heliospheric magnetic field (HMF), which, in turn, depends on the solar activity. The radioisotopes can, therefore, serve as proxy records of the behaviour of the heliosphere in the past, in particular over prolonged solar quiet periods, such as during Gleissberg or Maunder minima, when the production rate of radioisotopes is expected to change significantly. For this purpose we have measured the 44 Ti (T 1/2 =66.6 yr) in ten stony meteorites, which fell between 1840–1992. The results indicate that the production of 44 Ti was significantly higher when the solar activity was persistently low, indicating that the HMF was weak during such periods, enabling higher flux of cosmic rays to enter the inner heliosphere.

Published
1997
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17. Radiometric and tephroanalysis dating of recent Ionian Sea cores

Author

G. Cini Castagnoli, G. Bonino, E. Callegari, and Guang-Mei Zhu

Subjects
Paleontology, geography, Mediterranean sea, Oceanography, geography.geographical_feature_category, Volcano, Terrace (geology), Absolute dating, Geochronology, Sediment, Radiometric dating, Tephrochronology
Abstract

An accurate dating of recent Ionian Sea sediment cores has been performed by the210Pb radiometric method and by a detailed tephroanalysis. The markers of the historical volcanic eruptions which occurred in the Campanian area (Vesuvius, Phlegrean Fields, Ischia) during the last two millenia have been identified along the cores. Among the others, the famous Plinian Vesuvius eruption of 79 AD, which buried the Roman town of Pompei, has been recognized. Direct210Pb dating is limited to the last two centuries. The tephroanalysis demonstrates that the sedimentation rate estimated by the210Pb method is correct and it is constant, at least for the last 2 ky. The presence of the137Cs peak due to the intense activity of nuclear-weapon testing in the atmosphere in 1963–64 AD assures that the top of the core is present and not disturbed. The high precision of the core dating allows to transform the depth scale into a time scale with an accuracy of ∼1%. The analysis of several cores taken in the same area demonstrates that the results presented here are of general validity, at least in this region. The carbonatic mud deposited in the last millennia in the Gallipoli Terrace can be successfully utilized for investigating the environmental conditions in the recent past.

Published
1993
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18. The hadron calorimeter of EAS-TOP: operation, calibration and resolution

Author

A. Castellina, P. Vallania, F. Arneodo, A. Chiavassa, C. Morello, L. Bergamasco, R. Bertoni, M. Aglietta, Carlotta Castagnoli, A. Campos Fauth, O. Saavedra, R. Adinolfi Falcone, P.L. Ghia, M. E. Bertaina, Pietro Antonioli, W. Fulgione, E. Tatananni, B. D'Ettorre Piazzoli, Bruno Alessandro, G. Cini Castagnoli, M. Iacovacci, G. Navarra, G.C. Trinchero, S. Vernetto, L. Riccati, G. Mannocchi, A. Giuliano, P. Galeotti, G. Di Sciascio, Carlo Vigorito, Helio Nogima, R. A., Falcone, M., Aglietta, B., Alessandro, P., Antonioli, F., Arneodo, L., Bergamasco, M., Bertaina, R., Bertoni, A. C., Fauth, C., Castagnoli, A., Castellina, A., Chiavassa, G. C., Castagnoli, D'ETTORRE PIAZZOLI, Benedetto, G. D., Sciascio, W., Fulgione, P., Galeotti, P. L., Ghia, A., Giuliano, Iacovacci, Michele, G., Mannocchi, C., Morello, G., Navarra, H., Nogima, L., Riccati, O., Saavedra, E., Tatananni, G. C., Trinchero, P., Vallania, S., Vernetto, C., Vigorito, R., Adinolfi Falcone, A., Campos Fauth, G., Cini Castagnoli, and G., Di Sciascio

Subjects
Physics, Nuclear and High Energy Physics, Range (particle radiation), Calorimeter (particle physics), Physics::Instrumentation and Detectors, Calibration curve, Astrophysics::High Energy Astrophysical Phenomena, Resolution (electron density), Hadron, GRAN-SASSO, Nuclear physics, PHYSICS, COSMIC-RAY EVENTS, Calibration, High Energy Physics::Experiment, Detectors and Experimental Techniques, Nuclear Experiment, Instrumentation, Energy (signal processing), Beam (structure)
Abstract

We describe and discuss the operation, calibration and stability of the EAS-TOP calorimeter (Campo Imperatore, National Gran Sasso Laboratories), a large area hadron and muon detector devoted to cosmic-ray physics. It consists of iron slabs (for a total thickness of 818 g cm(-2)) and Iarocci tubes as sensitive layers, operating in the streamer mode and the "quasi proportional" regime. Using a model describing the operation of the "quasi proportional" chambers, we derive a calibration curve in the energy range 50-5000 GeV, whose reliability has been indirectly checked through on-site measurements, by means of an accelerator beam run (up to similar or equal to 600-700 GeV) and by comparing the model predictions on hadron shower transition curves with the data. (C) 1999 Elsevier Science B.V. All rights reserved.

Published
1999

19. Search for high energy GRBs with EASTOP

Author

Carlotta Castagnoli, Gian Carlo Trinchero, M. Iacovacci, G. Di Sciascio, Piero Vallania, L. Bergamasco, F. Arneodo, O. Saavedra, A. Chiavassa, B. D'Ettorre Piazzoli, M. E. Bertaina, G. Cini, Bruno Alessandro, Marco Aglietta, C. Morello, G. Mannocchi, Pietro Antonioli, Antonella Castellina, S. Vernetto, G. Navarra, P. Galeotti, W. Fulgione, P. L. Ghia, Carlo Vigorito, M., Aglietta, B., Alessandro, P., Antonioli, F., Arneodo, L., Bergamasco, M., Bertaina, C., Castagnoli, A., Castellina, A., Chiavassa, G., Cini, D'ETTORRE PIAZZOLI, Benedetto, G. D., Sciascio, W., Fulgione, P., Galeotti, P. L., Ghia, Iacovacci, Michele, G., Mannocchi, C., Morello, G., Navarra, O., Saavedra, G. C., Trinchero, P., Vallania, S., Vernetto, and C., Vigorito

Subjects
Physics, High energy, Astrophysics::High Energy Astrophysical Phenomena, Detector, General Physics and Astronomy, Astronomy, Cosmic ray, Astrophysics, Gamma-ray burst, Zenith, Energy (signal processing), Counting rate, Coincidence
Abstract

A search for GRBs of energy E> 10 GeV has been performed by studying the single particle counting rate of the EAS array EASTOP. No candidates have been observed in coincidence with 292 BATSE GRBs and the typical upper limits obtained on the energy fluence are F (10 GeV 1 TeV) 10 4 10 3 erg cm 2 for the events with zenith angle 10 GeV can reach the detector level; although the number of sec- ondary particles is too small to reconstruct the primary direction, GRBs could be detected as a short time increase in the single particle counting rate. The background con- sists of e and generated by low energy cosmic rays. All sources of background modulation have time scales (hours) much larger than the typical GRB duration (sec- onds), hence they do not aect the GRBs search. The EASTOP experiment is running since 1991 at Campo Imperatore in Italy, at 2000 m a.s.l. The ar- ray is devoted to the measurement of the various com- ponents of extensive air showers. In the GRBs search

Published
1999

20. Randomized trial of adjuvant chemotherapy versus control after curative resection for gastric cancer: 5-year follow-up

Author

Roberto Tarquini, D Francesconi, R Moretti, Roberto Mazzanti, Bruno Neri, A. Mercatelli, Salvatore Mario Romano, L Siliani, B Boffi, F Medi, F Andreoli, and G. Cini

Subjects
Adult, Male, Cancer Research, medicine.medical_specialty, medicine.drug_class, Short Communication, medicine.medical_treatment, Adenocarcinoma, epidoxorubicin, Antimetabolite, law.invention, Randomized controlled trial, Stomach Neoplasms, law, Antineoplastic Combined Chemotherapy Protocols, randomized trial, Humans, Medicine, 5-fluorouracil, Aged, Epirubicin, Chemotherapy, business.industry, gastric cancer, Stomach, Cancer, Middle Aged, medicine.disease, Surgery, adjuvant chemotherapy, Editorial, medicine.anatomical_structure, Oncology, Chemotherapy, Adjuvant, Fluorouracil, Multivariate Analysis, Female, leucovorin, business, Follow-Up Studies, medicine.drug
Abstract

Adjuvant chemotherapy of gastric cancer after curative resection is still subject to discussion. In this study 137 patients with gastric adenocarcinoma, all with positive nodes, were randomized after curative resection so that 69 received epidoxorubicin (EPI), leucovorin (LV) and 5-fluorouracil (5-FU) on days 1–3 every 3 weeks for 7 months, whereas the remaining 68 did not. After a follow-up period of 5 years, 21 of the 69 treated patients (30%) and nine controls (13%) were still alive; median survival time was 18 months for the controls and 31 months for the patients treated with adjuvant chemotherapy (P< 0.01). © 2001 Cancer Research Campaign http://www.bjcancer.com

Published
2001
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21. The most powerful scintillator supernovae detector: LVD

Author

Rosario Nania, G. Cini, P. Galeotti, L. G. Dos Santos, Carlotta Castagnoli, Giuseppe Iacobucci, Roy Weinstein, F. Wang, P. Vallania, J. H. Moromisato, O. G. Ryazhskaya, G. Maccarrone, D. Parks, O. Saavedra, K. Lau, W. D. Tian, V. A. Kudryavtsev, A. S. Malguin, Tomonori Wada, E. V. Korolkova, Luisa Cifarelli, E. D. Alyea, I. A. Pless, S. Vernetto, Y. Ban, Gabriella Sartorelli, G. Bruni, K. Chen, X. Lin, R. Weathers, Behcet Alpat, B. Zhuan, J. Qiu, A. Bizzetti, S. Wang, P. Picchi, M. Deutsch, G. T. Zatsepin, Antonino Zichichi, A. Contin, T. Massam, E. S. Hafen, X. Zhu, B. Monteleoni, E. von Goeler, H. Tang, G. Yi, M. Pu, Y. Cao, D. Shen, M. Dardo, V. L. Dadikin, J. Pyrlyk, J. Ma, G. H. Mo, M. Widgoff, B. Mayes, P.G. Pelfer, Jose Chinellato, L. Xu, G. Cara Romeo, A. Turtelli, V. F. Yakushev, P. Pinna, G. Bari, Z. Mao, F. F. Khalchukov, G. Navarra, L. Panaro, R. Chen, L. Votano, Shuang Cong, J. Tang, Isao Yamamoto, Z. Xu, G. Landi, F. Grianti, V. P. Talochkin, Z. Ma, Lawrence Pinsky, N. Inoue, X. Zhou, L. Lu, K. Saitoh, V. S. Berezinsky, R. I. Enikeev, Fabrizio Fabbri, P. Antonioli, Giovanni Badino, P. Giusti, D. Sanders, C. Morello, A. Benelli, P. V. Kortchaguin, P. Haridas, R. Casaccia, Marco Aglietta, Stefano Bianco, M. Basile, A. De Silva, Akeo Misaki, V. G. Ryasny, S. Sarwar, L. Periale, S. Gu, Antonella Castellina, L. Bergamasco, Piera Luisa Ghia, Q. Zhu, W. Fulgione, V. B. Kortchaguin, N. Mengotti Silva, M. A. Markov, H. Wang, I. Uman, G. C. Trinchero, G. Anzivino, and A. Zallo

Subjects
Physics, cosmic neutrinos, scintilation counter, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astronomy, Cosmic ray, Astrophysics, Scintillator, Neutrino interaction, cosmic rays, LVD experiment, Galaxy, Supernova, Scintillation counter, High Energy Physics::Experiment, Neutrino, Large Volume Detector
Abstract

The Large Volume Detector (LVD) in the Gran Sasso underground Laboratory is a multipurpose detector consisting of a large volume of liquid scintillator interleaved with limited streamer tubes. In this paper we discuss its power to study low-energy cosmic neutrinos. The results show that the first LVD tower (368 tons of liquid scintillator) is well suited to detect neutrinos from gravitational stellar collapses within all of our Galaxy over a wide range of burst duration (up to a few hundred seconds). No burst candidates have been observed in the first two months of data taking.

Published
1992
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22. Modulation by lonidamine of the antiproliferative activity of adriamycin on yoshida hepatoma of the rat

Author

G Cini-Neri, Bruno Neri, M. T. Gemelli, G. Lottini, M. Bandinelli, and S. Sambataro

Subjects
Pharmacology, Antitumor activity, medicine.medical_specialty, Chemotherapy, business.industry, medicine.medical_treatment, Lonidamine, Long-term potentiation, Drug interaction, chemistry.chemical_compound, Endocrinology, chemistry, Oral administration, In vivo, Internal medicine, Toxicity, Medicine, Pharmacology (medical), business
Abstract

A study was performed in Yoshida hepatoma-bearing rats to confirm in vivo, in an experimental model, the preliminary data on the potentiation by lonidamine of the antitumor activity of adriamycin. Lonidamine alone, administered orally with food, did not reduce tumor cell proliferation, but in combination with adriamycin (5 mg/kg intraperitoneally 6 days after tumor transplant), it produced a remarkable increase in adriamycin's hepatoma cell toxicity (44% vs controls, P P

Published
1992
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23. The carbonate profile of two recent Ionian Sea cores: Evidence that the sedimentation rate is constant over the last millennia

Author

G. Bonino, F. Caprioglio, Zhu Guang-Mei, A. Provenzale, M. Serio, and G. Cini Castagnoli

Subjects
Delta, paleoclimatology, Carbonate profile, Mineralogy, law.invention, chemistry.chemical_compound, Paleontology, Geophysics, Mediterranean sea, chemistry, periodicities, radiocarbon, Isotopes of carbon, law, General Earth and Planetary Sciences, Carbonate, Carbonate rock, Sedimentary rock, Radiometric dating, Radiocarbon dating, Geology
Abstract

The authors confirm and extend the results previously reported on the carbonate profile of the GT14 Ionian Sea core (Cini Castagnoli et al., 1990). A second, much longer core (2.81 meters) named GT89/3, has been taken about 1 km apart from the previous one. The carbonate profiles of the two cores are impressively similar; the details of the CaCO{sub 3} variations in the two sediments match on the scale of the sampling interval {Delta}d = 2.5 mm used for both cores. The authors show that {Delta}d corresponds to the mud deposited in a time interval {Delta}t = 3.87 {plus minus} 0.04 years, a value which is constant throughout the entire length of the cores. This precision is achieved by the tephroanalysis of the two cores. In this approach the markers of well-known historical eruptions in the Vesuvius area are recognized (Pompei, AD 79, Pollena, AD 472, Ischia, AD 1301), providing a precise dating which accurately tunes that obtained by the radiometric method. The correlation between the carbonate profile of the GT14 core and the tree-ring radiocarbon record has been discussed in (Cini Castagnoli et al., 1990); here the authors extend these results and show that the same correlation holds atmore » least up to 1690 BC. Due to the longer length of the GT89/3 time series, they also show that three periodic components at about 206 yr, 228 yr and 179 yr may now be resolved in the carbonate series, in close agreement with the results already found for the radiocarbon record.« less

Published
1990
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24. The CaCO3profile in a recent Ionian sea core and the tree ring radiocarbon record over the last two millennia

Author

Narendra Bhandari, G. Bonino, F. Caprioglio, M. Serio, A. Provenzale, and G. Cini Castagnoli

Subjects
Delta, 14C tree ring profile, Sediment, Mineralogy, Carbon cycle, law.invention, Geophysics, paleoclimatology xarbonate profile, periodicities, law, Isotopes of carbon, Content (measure theory), Paleoclimatology, Dendrochronology, General Earth and Planetary Sciences, Radiometric dating, Radiocarbon dating, Geology
Abstract

The calcium carbonate (CaCO{sub 3}) profile of a recent sediment core, drilled in the Ionian Sea in 1979, is studied. The CaCO{sub 3} content of the sediment has been measured at regularly spaced intervals of {Delta}d=0.25 cm corresponding to {Delta}t=3.87 yr from AD 170 to the present. The CaCO{sub 3} profile of the core closely resembles the radiocarbon time series as deduced from tree ring data. The two records have a correlation coefficient of about 0.8 and show strikingly similar long-term variations. This result presumably follows from the fact that both systems take part in the carbon cycle. The spectral analysis of the CaCO{sub 3} time series reveals the presence of the well known periodicity with period ca: 200 years, characteristic of the {Delta}{sup 14}C record. Since the CaCO{sub 3} content of sea sediments is governed by biological, physical and chemical processes in surface sea waters, which in turn are strongly influenced by climatic conditions, and since the {approx}200 yr {Delta}{sup 14}C wave is known to be governed by solar modulation of galactic cosmic rays, the tuning of these two records on the same frequencies suggests a strong Sun-climate relationship.

Published
1990
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25. Results On Candidate Uhe Gamma-ray Sources By the Eas-top Array (1989-1993)

Author

Carlotta Castagnoli, P. L. Ghia, M. Iacovacci, P. Galeotti, B. D'Ettorre Piazzoli, Piero Vallania, F. Arneodo, A. Chiavassa, G. Cini, Antonella Castellina, A. Campos Fauth, O. Saavedra, L. Riccati, Bruno Alessandro, G. Navarra, Marco Aglietta, L. Bergamasco, G. Di Sciascio, G. Mannocchi, S. Vernetto, W. Fulgione, C. Morello, Pietro Antonioli, Gian Carlo Trinchero, M., Aglietta, B., Alessandro, P., Antonioli, F., Arneodo, L., Bergamasco, A. C., Fauth, C., Castagnoli, A., Castellina, A., Chiavassa, G., Cini, D'ETTORRE PIAZZOLI, Benedetto, G., Disciascio, W., Fulgione, P., Galeotti, P. L., Ghia, Iacovacci, Michele, G., Mannocchi, C., Morello, G., Navarra, L., Riccati, O., Saavedra, G. C., Trinchero, P., Vallania, and S., Vernetto

Subjects
Physics, Gamma ray, Northern Hemisphere, Other Fields of Physics, Flux, Astronomy, Astronomy and Astrophysics, Astrophysics, GEMINGA, BURST, CRAB-NEBULA, Crab Nebula, Pulsar, HERCULES-X-1, SEARCH, TEV, RADIATION, EMISSION, Zenith, CYGNUS-X-3
Abstract

A search for UHE gamma-rays from 13 candidate point sources observable in the northern hemisphere (the Crab Nebula and Pulsar, Cygnus X-3, Hercules X-1, Geminga and others) has been performed by the EAS-TOP array during four years of operation since January 1989 to December 1993, at different energy thresholds (E(0) = 30-300 TeV). DC, periodic and sporadic emissions have been studied, and no evidence for significant excesses has been found from any of these searches. The derived 90% c.l. upper limits to the d.c. flux, for a source culminating at the zenith such as Cygnus X-3, are Phi(E > 230 TeV) < 2 x 10(-14) cm(-2) s(-1), Phi(E > 90 TeV) < 4.1 x 10(-14) cm(-2) s(-1) and Phi(E > 25 TeV) < 1.9 x 10(-13) cm(-2) s(-1). The excess from the Crab Nebula of February 23, 1989, as reported by the EAS-TOP, Baksan and KGF arrays, remains the only sporadic excess detected with statistically significant confidence level (probability of background imitation approximate to 10(-5)).

Published
1995

26. Study of the primary cosmic ray composition around the knee of the energy spectrum

Author

C. W. Peck, G. Giannini, M. Goretti, F. Guarino, G. Liu, R. Baker, A. Marzari Chiesa, A. Corona, N. Giglietto, L. Patrizii, V. Valente, O. Erriquez, M. Severi, Fabrizio Cei, G. Mandrioli, Vincenzo Patera, M. Aglietta, M. Spinetti, J. L. Stone, B. Pavesi, M. Mittelbrun, V. Bisi, C. DeMarzo, C. R. Bower, L. Satta, A. Sciubba, G.C. Trinchero, M. Ambrosio, D. Martello, O. Palamara, Pietro Antonioli, C. Melagrana, C. Bloise, Erik Katsavounidis, B. C. Barish, P. Fusco, P. Serra Lugaresi, M. E. Bertaina, J. A. Musser, D. Ficenec, C. W. Walter, Steven Ahlen, E. Kearns, H. Dekhissi, S. L. Mufson, A. Margiotta-Neri, G. Ludlam, Andrea Carlo Marini, F. Sartogo, M. Iacovacci, P. Pistilli, D. Campana, J. Petrakis, S. Klein, D. G. Michael, P. Bernardini, S. L. Nutter, A. Rainò, C. Morello, G. Cini, M. N. Mazziotta, C. E. Lane, Giuseppe Osteria, A. Sanzgiri, F. Cafagna, G. Mancarella, C. Bemporad, R. Pazzi, J. Reynoldson, Teresa Montaruli, S. Parlati, M. De Mitri, A. Marin, A. Di Credico, Robert A. Cormack, Lawrence Sulak, Kate Scholberg, Paolo Lipari, S. Kyriazopoulou, M. Carboni, A. Campos Fauth, Marco Grassi, Marco Monteno, O. Saavedra, R. Liu, R. C. Webb, C. Okada, Bruno Alessandro, R. Steinberg, Kael Hanson, Maurizio Spurio, A. Surdo, S. Vernetto, L. Bergamasco, G. Battistoni, Edward Diehl, G.L. Sanzani, E. Iarocci, P. Green, R. Nolty, P. Guarnaccia, C. Satriano, S. Cecchini, P. Vallania, P.L. Ghia, Alec Habig, M. Calicchio, Roberto Bellotti, R.M. Heinz, S. Petrera, Halina Bilokon, G. Navarra, G. Mannocchi, G. Di Sciascio, Donato Nicolo, L. Miller, D. Levin, Severino Angelo Maria Bussino, Y. Lu, W. Fulgione, N. D. Pignatano, E. Lamanna, B. D'Ettorre Piazzoli, J. Steele, M. J. Longo, Carlotta Castagnoli, A. Baldini, P. Spinelli, F. Arneodo, G. C. Barbarino, R. Antolini, A. Chiavassa, Eugenio Scapparone, L. Riccati, J. T. Hong, M. De Vincenzi, V. Togo, G. Auriemma, Gregory Tarle, P. Matteuzzi, G. DeCataldo, Mario Sitta, C. Gustavino, A. Castellina, C. Favuzzi, A. A. Grillo, C. Cattadori, V. Chiarella, P. Monacelli, P. Galeotti, S. Coutu, W. A. Worstell, C. Forti, G. Giacomelli, S P Mikheyev, F.J. Ronga, Aglietta, M, Alessandro, B, Antonioli, P, Arneodo, F, Bergamasco, L, Bertaina, M, Fauth, Ac, Castagnoli, C, Castellina, A, Cattadori, C, Chiavassa, A, Cini, G, Piazzoli, Bd, Disciascio, G, Fulgione, W, Galeotti, P, Ghia, Pl, Iacovacci, M, Mannocchi, G, Melagrana, C, Morello, C, Navarra, G, Riccati, L, Saavedra, O, Trinchero, Gc, Vallania, P, Vernetto, S, Ahlen, S, Ambrosio, M, Antolini, R, Auriemma, G, Baker, R, Baldini, A, Barbarino, Gc, Barish, Bc, Battistoni, G, Bellotti, R, Bemporad, C, Bernardini, P, Bilokon, H, Bisi, V, Bloise, C, Bower, C, Bussino, Severino Angelo Maria, Cafagna, F, Calicchio, M, Campana, D, Carboni, M, Cecchini, S, Cei, F, Chiarella, V, Cormack, R, Corona, A, Coutu, S, Decataldo, G, Dekhissi, H, Demarzo, C, Demitri, L, Devincenzi, M, Dicredico, A, Diehl, E, Erriquez, O, Favuzzi, C, Ficenec, D, Forti, C, Fusco, P, Giacomelli, G, Giannini, G, Giglietto, N, Goretti, M, Grassi, M, Green, P, Grillo, A, Guarino, F, Guarnaccia, P, Gustavino, C, Habig, A, Hanson, K, Heinz, R, Hong, Jt, Iarocci, E, Katsavounidis, E, Kearns, E, Klein, S, Kyriazopoulou, S, Lamanna, E, Lane, C, Levin, D, Lipari, P, Liu, G, Liu, R, Longo, Mj, Lu, Y, Ludlam, G, Mancarella, G, Mandrioli, G, Margiottaneri, A, Marin, A, Marini, A, Martello, D, Chiesa, Am, Matteuzzi, P, Mazziotta, Mn, Michael, Dg, Mikheyev, S, Miller, L, Mittelbrun, M, Monacelli, P, Montaruli, T, Monteno, M, Mufson, S, Musser, J, Nicolo, D, Nolty, R, Nutter, S, Okada, C, Osteria, G, Palamara, O, Parlati, S, Patera, V, Patrizii, L, Pavesi, B, Pazzi, R, Peck, Cw, Petrakis, J, Petrera, S, Pignatano, Nd, Pistilli, P, Raino, A, Reynoldson, J, Ronga, F, Sanzani, G, Sanzgiri, A, Sartogo, F, Satriano, C, Satta, L, Scapparone, E, Scholberg, K, Sciubba, A, Lugaresi, P, Severi, M, Sitta, M, Spinelli, P, Spinetti, M, Spurio, M, Steele, J, Steinberg, R, Stone, Jl, Sulak, Lr, Surdo, A, Tarle, G, Togo, V, Valente, V, Walter, Cw, Webb, R, Worstell, W., M., Aglietta, B., Alessandro, P., Antonioli, F., Arneodo, L., Bergamasco, M., Bertaina, A., Campos Fauth, C., Castagnoli, A., Castellina, C., Cattadori, A., Chiavassa, G., Cini, B., D'Ettorre Piazzoli, G., Di Sciascio, W., Fulgione, P., Galeotti, P. L., Ghia, M., Iacovacci, G., Mannocchi, C., Melagrana, C., Morello, G., Navarra, L., Riccati, O., Saavedra, G. C., Trinchero, P., Vallania, S., Vernetto, S., Ahlen, M., Ambrosio, R., Antolini, G., Auriemma, R., Baker, A., Baldini, G. C., Barbarino, B. C., Barish, G., Battistoni, R., Bellotti, C., Bemporad, P., Bernardini, H., Bilokon, V., Bisi, C., Bloise, C., Bower, S., Bussino, F., Cafagna, M., Calicchio, D., Campana, M., Carboni, S., Cecchini, F., Cei, V., Chiarella, R., Cormack, A., Corona, S., Coutu, G., Decataldo, H., Dekhissi, C., Demarzo, M., De Mitri, M., De Vincenzi, A., Di Credico, E., Diehl, O., Erriquez, C., Favuzzi, D., Ficenec, C., Forti, P., Fusco, G., Giacomelli, G., Giannini, N., Giglietto, M., Goretti, M., Grassi, P., Green, A., Grillo, F., Guarino, P., Guarnaccia, C., Gustavino, A., Habig, K., Hanson, R., Heinz, J. T., Hong, E., Iarocci, E., Katsavounidi, E., Kearn, S., Klein, S., Kyriazopoulou, E., Lamanna, C., Lane, D. S., Levin, P., Lipari, G., Liu, R., Liu, M. J., Longo, Y., Lu, G., Ludlam, Mancarella, Giovanni, G., Mandrioli, A., Margiotta Neri, A., Marin, A., Marini, Martello, Daniele, A., Marzari Chiesa, P., Matteuzzi, M. N., Mazziotta, D. G., Michael, S., Mikheyev, L., Miller, M., Mittelbrun, P., Monacelli, T., Montaruli, M., Monteno, S., Mufson, J., Musser, D., Nicoló, R., Nolty, S., Nutter, C., Okada, G., Osteria, O., Palamara, S., Parlati, V., Patera, L., Patrizii, B., Pavesi, R., Pazzi, C. W., Peck, J., Petraki, S., Petrera, N. D., Pignatano, P., Pistilli, A., Rainó, J., Reynoldson, F., Ronga, G., Sanzani, A., Sanzgiri, F., Sartogo, C., Satriano, L., Satta, E., Scapparone, K., Scholberg, A., Sciubba, P., Serra Lugaresi, M., Severi, M., Sitta, P., Spinelli, M., Spinetti, M., Spurio, J., Steele, R., Steinberg, J. L., Stone, L. R., Sulak, A., Surdo, G., Tarlé, V., Togo, V., Valente, C. W., Walter, R., Webb, W., Worstell, A. C., Fauth, D'ETTORRE PIAZZOLI, Benedetto, G., Disciascio, Iacovacci, Michele, Barbarino, Giancarlo, L., Demitri, M., Devincenzi, A., Dicredico, Guarino, Fausto, G., Mancarella, A., Margiottaneri, D., Martello, A. M., Chiesa, D., Nicolo, A., Raino, P. S., Lugaresi, G., Tarle, Aglietta M., Alessandro B., Antonioli P., Arneodo F., Bergamasco L., Bertaina M., Fauth A.C., Castagnoli C., Castellina A., Cattadori C., Chiavassa A., Cini G., D'Ettorre Piazzoli B., Di Sciascio G., Fulgione W., Galeotti P., Ghia P.L., Iacovacci M., Mannocchi G., Melagrana C., Morello C., Navarra G., Riccati L., Saavedra O., Trinchero G.C., Vallania P., Vernetto S., Ahlen S., Ambrosio M., Antolini R., Auriemma G., Baker R., Baldini A., Barbarino G.C., Barish B.C., Battistoni G., Bellotti R., Bemporad C., Bernardini P., Bilokon H., Bisi V., Bloise C., Bower C., Bussino S., Cafagna F., Calicchio M., Campana D., Carboni M., Cecchini S., Cei F., Chiarella V., Cormack R., Corona A., Coutu S., DeCataldo G., Dekhissi H., DeMarzo C., De Mitri M., De Vincenzi M., Di Credico A., Diehl E., Erriquez O., Favuzzi C., Ficenec D., Forti C., Fusco P., Giacomelli G., Giannini G., Giglietto N., Goretti M., Grassi M., Green P., Grillo A., Guarino F., Guarnaccia P., Gustavino C., Habig A., Hanson K., Heinz R., Hong J.T., Iarocci E., Katsavounidis E., Kearns E., Klein S., Kyriazopoulou S., Lamanna E., Lane C., Levin D.S., Lipari P., Liu G., Liu R., Longo M.J., Lu Y., Ludlam G., Mancarella G., Mandrioli G., Margiotta-Neri A., Marin A., Marini A., Martello D., Chiesa A.M., Matteuzzi P., Mazziotta M.N., Michael D.G., Mikheyev S., Miller L., Mittelbrun M., Monacelli P., Montaruli T., Monteno M., Mufson S., Musser J., Nicolo D., Nolty R., Nutter S., Okada C., Osteria G., Palamara O., Parlati S., Patera V., Patrizii L., Pavesi B., Pazzi R., Peck C.W., Petrakis J., Petrera S., Pignatano N.D., Pistilli P., Raino A., Reynoldson J., Ronga F., Sanzani G., Sanzgiri A., Sartogo F., Satriano C., Satta L., Scapparone E., Scholberg K., Sciubba A., Lugaresi P.S., Severi M., Sitta M., Spinelli P., Spinetti M., Spurio M., Steele J., Steinberg R., Stone J.L., Sulak L.R., Surdo A., Tarle G., Togo V., Valente V., Walter C.W., Webb R., and Worstell W.

Subjects
Nuclear and High Energy Physics, Proton, EAS-TOP, Astrophysics::High Energy Astrophysical Phenomena, Other Fields of Physics, chemistry.chemical_element, Cosmic ray, MACRO, Astrophysics, CASCADES, Coincidence, Spectral line, DEEP-UNDERGROUND MUONS, Nuclear physics, Primary (astronomy), Nuclear Experiment, Helium, Physics, Range (particle radiation), Muon, GRAN-SASSO, MACRO DETECTOR, Astrophysics::Instrumentation and Methods for Astrophysics, Gran Sasso, chemistry, High Energy Physics::Experiment
Abstract

A study of the primary cosmic ray composition in the energy range 5ṡ1014−5ṡ1015 eV is performed through the analysis of the deep underground muons and of the e.m. component of Extensive Air Showers detected in coincidence by the MACRO and EAS-TOP experiments at the Gran Sasso Laboratory. We conclude that: a) pure proton and Iron primary beams are excluded by the experimental data; b) a fraction of nuclei heavier than Helium is necessary to explain the experimental data both below and above the knee; c) a mixed composition, obtained a priori from extrapolations of the spectra directly measured below 100 TeV, yields a reasonable account of the observations up to the knee of the primary spectrum.

Published
1994

27. The cosmic ray primary composition between 10(15) and 10(16) eV from Extensive Air Showers electromagnetic and TeV muon data

Author

L. Patrizii, M. Ambrosio, G. Sirri, Pietro Antonioli, F. Cafagna, S. Valchierotti, A. Rainò, C. Bemporad, Carlo Vigorito, I. De Mitri, C. R. Bower, B. D'Ettorre Piazzoli, Annarita Margiotta, V. Popa, Donato Nicolo, P. L. Ghia, Alec Habig, Paolo Lipari, C. De Marzo, M. Cozzi, F.J. Ronga, R. Caruso, A. Marzari-Chiesa, Marco Monteno, D. G. Michael, J. A. Musser, D. Levin, R.M. Heinz, Np Longley, E. Katsavounidis, G. Mannocchi, A. Di Credico, Yvonne Becherini, M. Vakili, C. E. Lane, C. Morello, S. Kyriazopoulou, F. Maaroufi, Fabrizio Cei, P. Serra, M. Brigida, M. Calicchio, Halina Bilokon, M. N. Mazziotta, R. C. Webb, M. Iacovacci, Maximiliano Sioli, W. Fulgione, M. J. Longo, M. Grassi, E. Iarocci, F. Guarino, S. Vernetto, Kate Scholberg, O. Saavedra, J. Derkaoui, S. L. Mufson, P. Vallania, V. Togo, Marco Aglietta, D. Martello, P. Spinelli, Kael Hanson, G. Di Sciascio, L. R. Sulak, L. Perrone, G. Battistoni, R. Steinberg, C. W. Walter, R. Nolty, H. Dekhissi, E. Lamanna, B. C. Choudhary, D. Campana, R. Pazzi, C. Satriano, M. Spinetti, Gregory Tarle, Giuseppe Osteria, P. Fusco, Antonio Stamerra, M. Giorgini, P. Galeotti, Andrea Carlo Marini, Maurizio Spurio, Roberto Bellotti, S. Petrera, O. Erriquez, E. Kearns, C. Orth, S. Cecchini, C. Favuzzi, C. W. Peck, G. Navarra, L. Bergamasco, Ioannis Katsavounidis, C. Forti, G. Giacomelli, Hyun-Chul Kim, Severino Angelo Maria Bussino, G. C. Barbarino, Eugenio Scapparone, M. De Vincenzi, F. Arneodo, R. Antolini, G. Giannini, G. Mandrioli, S. Coutu, N. Giglietto, A. A. Grillo, G. C. Trinchero, Mario Sitta, G. de Cataldo, C. Gustavino, J. L. Stone, F. Loparco, M. E. Bertaina, V. Chiarella, P. Monacelli, M. Carboni, C. Castagnoli, Bruno Alessandro, G. Cini, A. Surdo, A. Chiavassa, P. Bernardini, Antonella Castellina, Vincenzo Patera, A. Sciubba, A. Baldini, O. Palamara, B. C. Barish, G. Mancarella, J. Reynoldson, Teresa Montaruli, Aglietta, M, Alessandro, B, Antonioli, P, Arneodo, F, Bergamasco, L, Bertaina, M, Castagnoli, C, Castellina, A, Chiavassa, A, Cini, G, Piazzoli, Bd, Di Sicascio, G, Fulgione, W, Galeotti, P, Ghia, Pl, Iacovacci, M, Mannocchi, G, Morello, C, Navarra, G, Saavedra, O, Stamerra, A, Trinchero, Gc, Valchierotti, S, Vallania, P, Vernetto, S, Vigorito, C, Ambrosio, M, Antolini, R, Baldini, A, Barbarino, Gc, Barish, Bc, Battistoni, G, Becherini, Y, Bellotti, R, Bemporad, C, Bernardini, P, Bilokon, H, Bower, C, Brigida, M, Bussino, Severino Angelo Maria, Cafagna, F, Calicchio, M, Campana, D, Carboni, M, Caruso, R, Cecchini, S, Cei, F, Chiarella, V, Choudhary, Bc, Coutu, S, Cozzi, M, De Cataldo, G, Dekhissi, H, De Marzo, C, De Mitri, I, Derkaoui, J, De Vincenzi, M, Di Credico, A, Erriquez, O, Favuzzi, C, Forti, C, Fusco, P, Giacomelli, G, Giannini, G, Giglietto, N, Giorgini, M, Grassi, M, Grillo, A, Guarino, F, Gustavino, C, Habig, A, Hanson, K, Heinz, R, Iarocci, E, Katsavounidis, E, Katsavounidis, I, Kearns, E, Kim, H, Kyriazopoulou, S, Lamanna, E, Lane, C, Levin, D, Lipari, P, Longley, Np, Longo, Mj, Loparco, F, Maaroufi, F, Mancarella, G, Mandrioli, G, Margiotta, A, Marini, A, Martello, D, Marzari Chiesa, A, Mazziotta, Mn, Michael, Dg, Monacelli, P, Montaruli, T, Monteno, M, Mufson, S, Musser, J, Nicolo, D, Nolty, R, Orth, C, Osteria, G, Palamara, O, Patera, V, Patrizii, L, Pazzi, R, Peck, Cw, Perrone, L, Petrera, S, Popa, V, Raino, A, Reynoldson, J, Ronga, F, Satriano, C, Scapparone, E, Scholberg, K, Sciubba, A, Serra, P, Sioli, M, Sirri, G, Sitta, M, Spinelli, P, Spinetti, M, Spurio, M, Steinberg, R, Stone, Jl, Sulak, Lr, Surdo, A, Tarle, G, Togo, V, Vakili, M, Walter, Cw, and Webb, R.

Subjects
Astroparticle physics, Physics, Muon, Air shower, cosmic rays, Hadron, Astronomy and Astrophysics, Rapidity, Cosmic ray, Astrophysics, Zenith, Spectral line
Abstract

The cosmic ray primary composition in the energy range between 10(15) and 10(16) eV, i.e., around the "knee" of the primary spectrum, has been studied through the combined measurements of the EAS-TOP air shower array (2005 m a. s.l., 10(5) m(2) collecting area) and the MACRO underground detector (963 m.a.s.l., 3100 m w.e. of minimum rock overburden, 920 m(2) effective area) at the National Gran Sasso Laboratories. The used observables are the air shower size (N-c) measured by EAS-TOP and the muon number (N-mu) recorded by MACRO. The two detectors are separated on average by 1200 m of rock, and located at a respective zenith angle of about 30degrees. The energy threshold at the surface for muons reaching the MACRO depth is approximately 1.3 TeV. Such muons are produced in the early stages of the shower development and in a kinematic region quite different from the one relevant for the usual N-mu - N-e studies. The measurement leads to a primary composition becoming heavier at the knee of the primary spectrum, the knee itself resulting from the steepening of the spectrum of a primary light component (p, He) of Deltay = 0.7 +/- 0.4 at E-0 similar to 4 x 10(15) eV. The result confirms the ones reported from the observation of the low energy muons at the surface (typically in the GeV energy range), showing that the conclusions do not depend on the production region kinematics. Thus, the hadronic interaction model used (CORSIKA/QGSJET) provides consistent composition results from data related to secondaries produced in a rapidity region exceeding the central one. Such an evolution of the composition in the knee region supports the "standard" galactic acceleration/propagation models that imply rigidity dependent breaks of the different components.. and therefore breaks occurring at lower energies in the spectra of the light nuclei. (C) 2003 Elsevier B.V. All rights reserved.

Published
2004

28. Behavior of the Heliosphere over Prolonged Solar Quiet Periods by 44 Ti Measurements in Meteorites

Author

G. Bonino, Narendra Bhandari, Carla Taricco, and G. Cini Castagnoli

Subjects
Physics, Sunspot, Multidisciplinary, Meteorite, QUIET, Astronomical unit, Astronomy, Flux, Cosmic ray, Astrophysics, Heliosphere, Magnetic field
Abstract

The heliospheric magnetic field (HMF) is controlled by solar activity, as established by measurements over the last few decades, but its characteristics when the sun was quiet for prolonged periods, such as during Gleissberg or Maunder minima, are not known. Titanium-44, produced in meteorites, provides a monitor of the galactic cosmic ray (GCR) flux and allows estimation of the modulation effect of the sun for the period 1883 to 1992. The titanium-44 activity is consistent with the expected value, but the increase, due to the last Gleissberg minimum, is four times greater than expected for a GCR modulation based solely on sunspot numbers. This result implies that the HMF was weaker than at present and as a result the GCR flux (for energy greater than 1 gigaelectron volt) was higher between 2.2 to 3.6 protons per square centimeter per second per 4π steradians at 1 to 3 astronomical units in solar cycles 12 to 15.

Published
1995
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29. Measurement of the cosmic ray hadron spectrum up to 30 TeV at mountain altitude: the primary proton spectrum

Author

O. Saavedra, C. Morello, P.L. Ghia, C. Castagnoli, F. Arneodo, A. Castellina, P. Galeotti, B. D'Ettorre Piazzoli, G. Cini Castagnoli, Carlo Vigorito, Pietro Antonioli, G. Mannocchi, P. Vallania, W. Fulgione, L. Riccati, S. Vernetto, G. Di Sciascio, M. Aglietta, G. Navarra, Bruno Alessandro, M. E. Bertaina, G.C. Trinchero, S. Valchierotti, M. Iacovacci, L. Bergamasco, A. Chiavassa, M., Aglietta, B., Alessandro, P., Antonioli, F., Arneodo, L., Bergamasco, M., Bertaina, C., Castagnoli, A., Castellina, A., Chiavassa, G. C., Castagnoli, D'ETTORRE PIAZZOLI, Benedetto, G. D., Sciascio, W., Fulgione, P., Galeotti, P. L., Ghia, Iacovacci, Michele, G., Mannocchi, C., Morello, G., Navarra, L., Riccati, O., Saavedra, G. C., Trinchero, S., Valchierotti, P., Vallania, S., Vernetto, and C., Vigorito

Subjects
Physics, FLUX, Range (particle radiation), Particle physics, Proton, NUCLEI, Hadron, Astronomy and Astrophysics, Cosmic ray, HELIUM SPECTRA, ATMOSPHERE, Astrophysics, Power law, Nuclear physics, Altitude, KASCADE, Cosmic rays, Energy (signal processing)
Abstract

The flux of cosmic ray hadrons at the atmospheric depth of 820 g/cm^2 has been measured by means of the EAS-TOP hadron calorimeter (Campo Imperatore, National Gran Sasso Laboratories, 2005 m a.s.l.). The hadron spectrum is well described by a single power law : S(E_h) = (2.25 +- 0.21 +- 0.34(sys)) 10^(-7)(E_h/1000)^(-2.79 +- 0.05) m^(-2) s^(-1) sr^(-1) GeV^(-1) over the energy range 30 GeV-30 TeV. The procedure and the accuracy of the measurement are discussed. The primary proton spectrum is derived from the data by using the CORSIKA/QGSJET code to compute the local hadron flux as a function of the primary proton spectrum and to calculate and subtract the heavy nuclei contribution (basing on direct measurements). Over a wide energy range E_0 = 0.5-50 TeV its best fit is given by a single power law : S(E_0) = (9.8 +- 1.1 +- 1.6(sys)) 10^(-5) (E_0/1000)^(-2.80 +- 0.06) m^(-2) s^(-1) sr^(-1) GeV^(-1). The validity of the CORSIKA/QGSJET code for such application has been checked using the EAS-TOP and KASCADE experimental data by reproducing the ratio of the measured hadron fluxes at the two experimental depths (820 and 1030 g/cm^2 respectively) at better than 10% in the considered energy range., Comment: 16 pages, 9 figures, accepted for publication in Astroparticle Physics

Published
2002

30. Simultaneous observation of extensive air showers and deep-underground muons at the Gran Sasso Laboratory

Author

V. Chiarella, Paolo Giubellino, C. Bloise, P. Monacelli, M. Caliccio, Andrea Carlo Marini, M. Spinetti, Halina Bilokon, Piero Vallania, L. Patrizii, P. Chrysicopoulou, C. Morello, Lawrence Sulak, W. Fulgione, L. Bergamasco, G.C. Trinchero, D. Solie, S. L. Mufson, V. Bisi, S. Vernetto, C. Castagnoli, G. Giannini, Pio Pistilli, G. Mannocchi, M. J. Longo, B. Pal, R. Steinberg, Steven Ahlen, J. T. Hong, M. De Vincenzi, C. E. Lane, V. Flaminio, E. Hazen, G. Navarra, S. Coutu, O. Saavedra, P. Spinelli, G. Auriemma, Gregory Tarle, N. Giglietto, R.M. Heinz, Roberto Bellotti, F. Guarino, M. Fabbri, C. W. Peck, Marco Monteno, G. Battistoni, G. de Cataldo, G. Badino, G. Liu, Marco Aglietta, G. Mancarella, S. Cecchini, F.J. Ronga, J. Reynoldson, W. A. Worstell, B. D'Ettorre-Piazzoli, M. Ambrosio, P. Picchi, F. Predieri, C. Favuzzi, G.L. Sanzani, M. Severi, M. Iori, P. Serra, Paolo Lipari, R. Pazzi, G. Cini, A. Marin, C. Smith, Bruno Alessandro, P. Galeotti, Maurizio Spurio, G. C. Barbarino, J. Petrakis, O. Palamara, P. Green, R. C. Webb, C. Bemporad, P. Campana, L. Ramello, D. Ficenec, A. Surdo, D. Levin, O. Erriquez, G. Mandrioli, C. Forti, Massimo Masera, G. Giacomelli, S. Klein, P. Bernardini, S. Petrera, E. Iarocci, Vincenzo Patera, F. Cafagna, G. Martellotti, C. R. Bower, A. Sciubba, C. De Marzo, A. A. Grillo, J. A. Musser, L. Periale, B. C. Barish, V. Valente, Antonella Castellina, A. Marzari Chiesa, J. Steele, L. Petrillo, Marco Grassi, P. Matteuzzi, A. Baldini, P. L. Ghia, J. L. Stone, L. Satta, E. Lamanna, G. Rosa, Eugenio Nappi, L. Riccati, Barbarino, Giancarlo, Guarino, Fausto, The, Macro, EAS TOP, Collaborations, R., Bellotti, F., Cafagna, M., Caliccio, G., De Cataldo, C., De Marzo, O., Erriquez, C., Favuzzi, N., Giglietto, E., Nappi, P., Spinelli, S., Cecchini, M., Fabbri, G., Giacomelli, G., Mandrioli, P., Matteuzzi, B., Pal, L., Patrizii, F., Predieri, G., Sanzani, P., Serra, M., Spurio, S., Ahlen, D., Ficenec, E., Hazen, S., Klein, D., Levin, A., Marin, J., Stone, L., Sulak, W., Worstell, B., Barish, S., Coutu, J., Hong, G., Liu, C., Peck, D., Solie, J., Steele, C., Lane, R., Steinberg, G., Battistoni, H., Bilokon, C., Bloise, P., Campana, V., Chiarella, C., Forti, A., Grillo, E., Iarocci, A., Marini, V., Patera, J., Reynoldson, F., Ronga, L., Satta, M., Spinetti, V., Valente, C., Bower, R., Heinz, S., Mufson, J., Petraki, P., Monacelli, P., Bernardini, Mancarella, Giovanni, O., Palamara, P., Pistilli, A., Surdo, M., Longo, J., Musser, C., Smith, G., Tarlé, M., Ambrosio, G., Barbarino, F., Guarino, A., Baldini, C., Bemporad, V., Flaminio, G., Giannini, M., Grassi, R., Pazzi, G., Auriemma, P., Chrysicopoulou, M., De Vincenzi, M., Iori, E., Lamanna, P., Lipari, G., Martellotti, S., Petrera, L., Petrillo, G., Rosa, A., Sciubba, M., Severi, P., Green, R., Webb, V., Bisi, P., Giubellino, A., Chiesa, M., Masera, M., Monteno, L., Ramello, M., Aglietta, B., Alessandro, G., Badino, L., Bergamasco, C., Castagnoli, A., Castellina, G., Cini, B., D'Ettorre Piazzoli, W., Fulgione, P., Ghia, P., Galeotti, G., Mannocchi, C., Morello, G., Navarra, L., Periale, P., Picchi, L., Riccati, O., Saavedra, G., Trinchero, P., Vallania, S., Vernetto, Bellotti R., Cafagna F., Caliccio M., De Cataldo G., De Marzo C., Erriquez O., Favuzzi C., Giglietto N., Nappi E., Spinelli P., Cecchini S., Fabbri M., Giacomelli G., Mandrioli G., Matteuzzi P., Pal B., Patrizii L., Predieri F., Sanzani G.L., Serra P., Spurio M., Ahlen S., Ficenec D., Hazen E., Klein S., Levin D., Marin A., Stone J.L., Sulak L.R., Worstell W., Barish B., Coutu S., Hong J., Liu G., Peck C., Solie D., Steele J., Lane C., Steinberg R., Battistoni G., Bilokon H., Bloise C., Campana P., Chiarella V., Forti C., Grillo A., Iarocci E., Marini A., Patera V., Reynoldson J., Ronga F., Satta L., Spinetti M., Valente V., Bower C., Heinz R., Mufson S., Petrakis J., Monacelli P., Bernardini P., Mancarella G., Palamara O., Pistilli P., Surdo A., Longo M., Musser J., Smith C., Tarle G., Ambrosio M., Barbarino G.C., Guarino F., Baldini A., Bemporad C., Flaminio V., Giannini G., Grassi M., Pazzi R., Auriemma G., Chrysicopoulou P., De Vincenzi M., Iori M., Lamanna E., Lipari P., Martellotti G., Petrera S., Petrillo L., Rosa G., Sciubba A., Severi M., Green P., Webb R., Bisi V., Giubellino P., Chiesa A.M., Masera M., Monteno M., Ramello L., Aglietta M., Alessandro B., Badino G., Bergamasco L., Castagnoli C., Castellina A., Cini G., D'Ettorre-Piazzoli B., Fulgione W., Ghia P., Galeotti P., Mannocchi G., Morello C., Navarra G., Periale L., Picchi P., Riccati L., Saavedra O., Trinchero G., Vallania P., and Vernetto S.

Subjects
Astroparticle physics, Physics, Particle physics, Muon, Physics::Instrumentation and Detectors, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic ray, MACRO, Extensive air showers, Particle identification, Particle detector, Gran Sasso, Nuclear physics, extensive air showers, Scintillation counter, High Energy Physics::Experiment, Supermodule, Lepton
Abstract

Combined measurements of extensive air showers at the surface and high-energy muons deep underground have been initiated at the Gran Sasso Laboratory. The underground detector is the first supermodule of MACRO (area = 140 ${\mathrm{m}}^{2}$, depth = 3100 m of water equivalent, ${E}_{\ensuremath{\mu}}g1.3$ TeV) and the surface detector is the EAS-TOP array (altitude 2000 m above sea level, total enclosed area $A\ensuremath{\sim}{10}^{5}$ ${\mathrm{m}}^{2}$). We discuss the correlation technique, the comparison between the shower parameters as determined by the two detectors, and some of the characteristics of the reconstructed events.

Published
1990

31. The high energy muon spectrum in extensive air showers: first data from LVD and EAS-TOP at Gran Sasso

Author

T. Massam, Isao Yamamoto, Giovanni Badino, P. Giusti, Rosario Nania, L. G. Dos Santos, M. Selvi, L. Periale, J. H. Moromisato, A. Chiavassa, G. Cara Romeo, Carlotta Castagnoli, P. L. Ghia, R. Mantovani, N. Inoue, A. Campos Fauth, G. Bari, O. Saavedra, G. Di Sciascio, H. Nogima, B. D'Ettorre Piazzoli, W. Fulgione, R. Bertoni, J. Pyrlik, O. G. Ryazhskaya, V. S. Berezinsky, E. D. Alyea, P. Haridas, Antonino Zichichi, V. B. Korchaguin, B. Mayes, L. Bergamasco, V. P. Talochkin, A. Pesci, E. S. Hafen, R. I. Enikeev, I. A. Pless, S. Tsuji, C. Ghetti, V. L. Dadykin, G. Navarra, A. Turtelli, G. Guidi, L. Emaldi, C. Morello, I. Uman, G. C. Trinchero, M. Iacovacci, M. Basile, A. Megna, A. De Silva, Kwong Lau, Andrea Contin, A. S. Malguin, Tomonori Wada, M. Widgoff, V. A. Kudryavtsev, Giuseppe Iacobucci, F. Vetrano, M. Deutsch, F. Grianti, Behcet Alpat, E. V. Korolkova, Pietro Antonioli, L. Panaro, Luisa Cifarelli, V. F. Yakushev, N. Taborgna, A. Bosco, K. Saitoh, Marco Aglietta, F. Bersani, Stefano Santini, Lawrence Pinsky, G. Bruni, M. Luvisetto, P. Vallania, G. Cini Castagnoli, M. E. Bertaina, G. T. Zatsepin, G. Bonoli, F. Arneodo, G. Maccarrone, S. Vernetto, P. Dominici, R. Granella, A. Lima de Godoi, G. Mannocchi, F. F. Khalchukov, V. G. Ryasny, G. Conforto, N. Mengotti Silva, F. Cindolo, Jose Chinellato, P. V. Korchaguin, P. Picchi, Carlo Vigorito, J. Tang, E. Kemp, P. Galeotti, Roy Weinstein, Gabriella Sartorelli, E. von Goeler, Antonella Castellina, L. Votano, Bruno Alessandro, Fabrizio Fabbri, M., Aglietta, B., Alessandro, B., Alpat, E. D., Alyea, P., Antonioli, F., Arneodo, G., Badino, G., Bari, M., Basile, V. S., Berezinsky, L., Bergamasco, F., Bersani, M., Bertaina, R., Bertoni, G., Bonoli, A., Bosco, G., Bruni, A. C., Fauth, G. C., Romeo, C., Castagnoli, A., Castellina, A., Chiavassa, J. A., Chinellato, L., Cifarelli, F., Cindolo, G. C., Castagnoli, G., Conforto, A., Contin, V. L., Dadykin, A. D., Silva, M., Deutsch, D'ETTORRE PIAZZOLI, Benedetto, G. D., Sciascio, P., Dominici, L. G., Do, L., Emaldi, R. I., Enikeev, F. L., Fabbri, W., Fulgione, P., Galeotti, C., Ghetti, P. L., Ghia, P., Giusti, R., Granella, F., Grianti, G., Guidi, E. S., Hafen, P., Harida, G., Iacobucci, Iacovacci, Michele, N., Inoue, E., Kemp, F. F., Khalchukov, E. V., Korolkova, P. V., Korchaguin, V. B., Korchaguin, V. A., Kudryavtsev, K., Lau, A. L., De, M. L., Luvisetto, G., Maccarrone, A. S., Malguin, G., Mannocchi, R., Mantovani, T., Massam, B., Maye, A., Megna, N. M., Silva, C., Morello, J., Moromisato, R., Nania, G., Navarra, H., Nogima, L., Panaro, L., Periale, A., Pesci, P., Picchi, L., Pinsky, I. A., Ple, J., Pyrlik, V. G., Ryasny, O. G., Ryazhskaya, O., Saavedra, K., Saitoh, S., Santini, G., Sartorelli, M., Selvi, N., Taborgna, V. P., Talochkin, J., Tang, G. C., Trinchero, S., Tsuji, A., Turtelli, I., Uman, P., Vallania, S., Vernetto, F., Vetrano, C., Vigorito, E. v., Goeler, L., Votano, T., Wada, R., Weinstein, M., Widgoff, V. F., Yakushev, I., Yamamoto, G. T., Zatsepin, and A., Zichichi

Subjects
Nuclear physics, Physics, High energy, Muon, Coincident, SIMULATION, Astronomy and Astrophysics, Cosmic ray, DETECTOR
Abstract

We present evidence for a dependence of the average deep underground muon energies on shower size in the coincident EAS-TOP and LVD data at the Gran Sasso laboratories. The measured relation agrees with a mixed chemical composition of the cosmic ray primary spectrum at energies around 10(15) eV. (C) 1998 Elsevier Science B.V.

Published
1998

32. Adjuvant chemotherapy after gastric resection in node-positive cancer patients: a multicentre randomised study

Author

A Valeri, Bruno Neri, F Andreoli, L. Bruno, L. M. Pernice, C. Intini, V. de Leonardis, S Fabbroni, Salvatore Mario Romano, G. Cini, and D. Borrelli

Subjects
Cancer Research, medicine.medical_specialty, Time Factors, medicine.medical_treatment, Leucovorin, Adenocarcinoma, Drug Administration Schedule, Gastrectomy, Recurrence, Stomach Neoplasms, Antineoplastic Combined Chemotherapy Protocols, medicine, Humans, Survival rate, Epirubicin, Neoplasm Staging, Proportional Hazards Models, Chemotherapy, business.industry, Stomach, Cancer, medicine.disease, Surgery, Survival Rate, Regimen, medicine.anatomical_structure, Oncology, Fluorouracil, Chemotherapy, Adjuvant, Lymphatic Metastasis, business, medicine.drug, Follow-Up Studies, Research Article
Abstract

After curative resection for gastric adenocarcinoma, 103 patients, all with positive nodes, were randomised so that 48 received adjuvant chemotherapy of epidoxorubicin (EPI) 75 mg m-2 on day 1, leucovorin (LV) 200 mg m-2 on days 1-3 and 5-fluorouracil (5-FU) 450 mg m-2 on days 1-3, every 21 days for 7 months, whereas the remaining 55 did not. During the first year of observation, 21 control patients (38%) and five treated patients had recurrences. After a follow-up period of 36 months, 12 of the treated patients (25%) and only seven controls (13%) were still alive. At that point, the median survival was 13.6 months for the 55 untreated patients and 20.4 months for the 48 treated patients, a significant difference. We found a survival advantage for patients treated with the EPI-LV-5-FU regimen and a consistent delay in the appearance of recurrent or metastatic cancer. Acute toxicity was mild and treatment was well accepted by all patients. There was no long-term toxicity or any cardiac toxicity. We conclude that this particular chemotherapy, administered shortly after gastric resection, improves survival rate in node-positive gastric cancer patients, even although final assessment of this particular adjuvant approach must await completion of the trial.

Published
1996

33. Evidence for enhanced 10Be deposition in Mediterranean sediments 35kyr BP

Author

Guang-Mei Zhu, G. Bonino, E. Callegari, Ch. Shen, Carla Taricco, P. W. Kubik, Juerg Beer, Beate Dittrich-Hannen, Marc J.-F. Suter, G. Cini Castagnoli, and A. Albrecht

Subjects
Marine sediments, cosmogenic radioisotopes, cosmic rays, geography, geography.geographical_feature_category, Volcanic rock, Paleontology, Geophysics, Mediterranean sea, Ice core, Absolute dating, Geochronology, General Earth and Planetary Sciences, Tephra, Quaternary, Holocene, Geology
Abstract

In this letter, we report the profiles (∼160 samples) of 10Be, 9Be, Zn in a Mediterranean sediment core spanning the last 60 kyr. We show the existence of a 10Be peak, whose absolute age is estimated to be 34±3 kyr BP, based on its stratigraphic position between two tephra layers originating from two volcanic eruptions (Campanian Ignimbrite and Citara), dated by K-Ar, 40Ar-39Ar and 14C methods. This peak is similar to the increase in the 10Be concentration observed in Vostok and Dome C ice cores at the same age. The increase with approximately similar amplitude in both ice and sediment cores at different latitudes and hemispheres cannot be explained by changes in the archives. The present result supports the view of a well defined global enhancement of the 10Be flux, related to an increase of the 10Be production rate and not to a redistribution of the 10Be fallout between different latitudes.

Published
1995

34. Multiple muon events observed in the LVD experiment

Author

Rosario Nania, G. Cini, L. G. Dos Santos, J. H. Moromisato, Andrea Contin, G. T. Zatsepin, A. S. Malguin, Tomonori Wada, O. Saavedra, Q. Q. Zhu, M. Basile, M. Pu, A. De Silva, W. D. Tian, Z. Mao, K. Chen, X. Zhu, B. Monteleoni, I. Uman, G. C. Trinchero, L. Panaro, Y. Cao, J. Ma, Z. Xu, G. Bruni, Isao Yamamoto, Lawrence S. Pinsky, M. Widgoff, G. Brugnola, A. Bosco, L. Lu, V. L. Dadykin, Andrea Bizzeti, G. Navarra, M. Luvisetto, G. Maccarrone, G. H. Mo, D. Shen, S. Gu, J. Tang, O. G. Ryazhskaya, S. Vernetto, Y. Guo, V. P. Talochkin, G. Anzivino, Z. Ma, K. Saitoh, Giovanni Badino, P. Giusti, E. D. Alyea, A. Benelli, P. V. Kortchaguin, G. Cara Romero, N. Taborgna, I. A. Pless, E. V. Korolkova, F. Grianti, N. Mengotti Silva, P. Vallania, Stefano Bianco, C. Morello, B. Zhuang, J. Qiu, M. A. Markov, R. I. Enikeev, Drew Parks, Luisa Cifarelli, L. Bergamasco, F. Wang, E. S. Hafen, Marco Aglietta, M. Dardo, L. Xu, A. Turtelli, W. Fulgione, X. Zhou, H. Tang, V. G. Ryasny, D. Sanders, V. A. Kudryavtsev, V. S. Berezinsky, V. F. Yakushev, N. Inoue, R. Chen, P. Haridas, A. Zallo, G. Sartorelli, Giuseppe Iacobucci, R. Casaccia, X. Lin, S. Wang, P. Galeotti, J. Pyrlik, Behcet Alpat, Roy Weinstein, G. Bari, Y. Ban, B. W. Mayes, F. Cindolo, V. B. Kortchaguin, Jose Chinellato, P. Picchi, M. Deutsch, C. Castagnoli, F. L. Fabbri, Shuang Cong, Kwong Lau, S. Sarwar, L. Periale, P. L. Ghia, E. von Goeler, Akeo Misaki, Antonella Castellina, L. Votano, P. Antonioli, T. Massam, P. Pinna, F. F. Khalchukov, Hongwei Wang, R. Bertoni, Antonino Zichichi, P.G. Pelfer, and G. Landi

Subjects
Physics, Nuclear physics, Nuclear and High Energy Physics, Particle physics, Muon, Distribution (number theory), Physics::Instrumentation and Detectors, multiple muon events, Detector, High Energy Physics::Experiment, Tower, Atomic and Molecular Physics, and Optics, Multiplicity distribution
Abstract

This is a progress report on the multiple muon events recorded by the first tower of the LVD detector at the Gran Sasso Laboratory. About 17,000 multiple muon events have been observed since the LVD first tower started operation in June 1992. Presented here are the measured multiplicity distribution and separation distribution of muon pairs in the bundles.

Published
1994

35. Single muon angular distributions observed in the LVD particle astrophysics experiment

Author

X. Zhou, Q. Q. Zhu, M. Gatta, V. S. Berezinsky, S. Wang, W. D. Tian, P. Haridas, F. Grianti, N. Taborgna, G. Bruni, D. Sanders, D. Parks, R. Casaccia, E. D. Alyea, F. Wang, O. Saavedra, F. Cindolo, Jose Chinellato, B. Zhuang, G. Brugnola, C. Morello, A. Zallo, M. Luvisetto, V. A. Kudryavtsev, K. Chen, S. Gu, X. Lin, Marco Aglietta, Behcet Alpat, G. Bari, Isao Yamamoto, P. Vallania, E. V. Korolkova, S. Vernetto, I. A. Pless, Z. Mao, D. Hungerford, B. Monteleoni, L. Panaro, P. Picchi, E. S. Hafen, R. I. Enikeev, A. Bosco, Giovanni Badino, P. Giusti, M. Widgoff, Pietro Antonioli, Luisa Cifarelli, X. Zhu, L. Lu, M. Dardo, L. Xu, S. De Pasquale, A. Turtelli, K. Saitoh, P. V. Kortchaguin, Y. Cao, D. Shen, Andrea Contin, J. Ma, A. S. Malguin, I. Uman, G. C. Trinchero, H. Tang, Tomonori Wada, A. Benelli, M. Basile, D. Fabbri, A. De Silva, J. Pyrlik, Stefano Bianco, G. Navarra, Z. Xu, Andrea Bizzeti, V. L. Dadykin, V. P. Talochkin, Z. Ma, G. Anzivino, V. F. Yakushev, T. Massam, Shuang Cong, V. B. Kortchaguin, G. Landi, Kwong Lau, R. Chen, Giuseppe Iacobucci, G. Maccarrone, Lawrence Pinsky, M. Pu, Y. Ban, L. Periale, M. Deutsch, W. Fulgione, G. T. Zatsepin, P. L. Ghia, N. Inoue, Rosario Nania, G. Cini, S. Sarwar, Y. Guo, L. G. Dos Santos, L. Bergamasco, J. H. Moromisato, N. Mengotti Silva, M. A. Markov, V. G. Ryasny, F. F. Khalchukov, Hongwei Wang, P. Galeotti, Roy Weinstein, M. Ventura, J. Tang, L. Votano, Fabrizio Fabbri, G. Cara Romeo, Gabriella Sartorelli, M. Lindozzi, J. Qiu, E. von Goeler, Akeo Misaki, Antonella Castellina, Antonino Zichichi, B. Mayes, P.G. Pelfer, R. Bertoni, O. G. Ryazhskaya, and Carlotta Castagnoli

Subjects
Physics, cosmic rays, muons, LVD, Muon, Square Centimeter, Physics::Instrumentation and Detectors, muon angular distribution, Astrophysics::Instrumentation and Methods for Astrophysics, Flux, Steradian, Astronomy and Astrophysics, Cosmic ray, Square meter, Nuclear physics, High Energy Physics::Experiment, Zenith, Intensity (heat transfer)
Abstract

The first angular distribution data from 5547 hours of operation of the LVD detector are presented. The technique of track reconstruction is described. A total of 452 657 single muons were reconstructed for this period. The data are acceptance corrected in our final plots. The total single muon flux (the total flux from above impinging on a sphere of unit cross sectional area) in the Gran Sasso Laboratory is 1.03 muons per hour per square meter. The total flux crossing a unit horizontal area from above is 0.79 muons per hour per square meter. The acceptance-corrected intensity at cos θ = 1 is 0.349 muons per hour per square meter per steradian (9.7× l0 − 9 muons per second per square centimeter per steradian). We present, for the first time from Gran Sasso Laboratory, data at near-horizontal zenith angles.

Published
1994

36. First results of a search for neutrinos from collapsing stars with the LVD at Gran Sasso

Author

M. Aglietta, B. Alpat, E.D. Aleya, P. Antonioli, G. Anzivino, G. Badino, Y. Ban, G. Bari, M. Basile, A. Benelli, V.S. Berezinsky, L. Bergamasco, S. Bianco, A. Bizzetti, G. Bruni, Y. Cao, G. Cara Romeo, R. Casaccia, C. Castagnoli, A. Castellina, K. Chen, R. Chen, J.A. Chinellato, L. Cifarelli, G. Cini, S. Cong, A. Contin, V.L. Dadikin, M. Dardo, A. De Silva, M. Deutsch, L.G. Dos Santos, R.I. Enikeev, F.L. Fabbri, W. Fulgione, P. Galeotti, P. Ghia, P. Giusti, F. Grianti, S. Gu, E.S. Hafen, P. Haridas, G. Iacobucci, N. Inoue, F.F. Khalchukov, E.V. Korolkova, P.V. Kortchaguin, V.B. Kortchaguin, V.A. Kudryavtsev, G. Landi, K. Lau, X. Lin, L. Lu, J. Ma, Z. Ma, G. Maccarone, A.S. Malguin, Z. Mao, M.A. Markov, T. Massam, B. Mayes, N. Mengotti Silva, A. Misaki, G.H. Mo, B. Monteleoni, C. Morello, J. Moromisato, R. Nania, G. Navarra, L. Panaro, D. Parks, P.G. Pelfer, L. Periale, P. Picchi, P. Pinna, L. Pinsky, I.A. Pless, M. Pu, J. Pyrlyk, J. Qiu, V.G. Ryasny, O.G. Ryazhskaya, O. Saavedra, K. Saitoh, D. Sanders, G. Sartorelli, S. Sarwar, D. Shen, G. Susinno, V.P. Talochkin, H. Tang, J. Tang, W. Tian, G.C. Trinchero, A. Turtelli, I. Uman, P. Vallania, S. Vernetto, E. von Goeler, L. Votano, T. Wada, F. Wang, H. Wang, S. Wang, R. Weathers, R. Weinstein, M. Widgoff, L. Xu, Z. Xu, V.F. Yakushev, I. Yamamoto, G. Yi, A. Zallo, G.T. Zatsepin, X. Zhou, X. Zhu, B. Zhuan, and A. Zichichi

Subjects
ICARUS, Physics, Nuclear and High Energy Physics, COSMIC cancer database, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Detector, Other Fields of Physics, Astronomy, Astrophysics, Scintillator, Atomic and Molecular Physics, and Optics, Galaxy, Stars, High Energy Physics::Experiment, Neutrino, Large Volume Detector
Abstract

The Large Volume Detector (LVD) in the Gran Sasso underground Laboratory is a multipurpose detector consisting of a large volume of liquid scintillator interleaved with limited streamer tubes. In this paper we discuss its power to study low energy cosmic neutrinos. The results show that the first LVD tower (368 tons of liquid scintillator) is well suited to detect neutrinos from gravitational stellar collapses within all of our Galaxy over a wide range of burst duration (up to a few hundred seconds). No burst candidates have been observed in the first two months of data taking.

Published
1993

37. Amlodipine in the treatment of Raynaud's phenomenon

Author

I Gambini, Marco Rossi, N. Pitaro, G. Cini, Clodoveo Ferri, L. La Civita, and Dilia Giuggioli

Subjects
medicine.medical_specialty, business.industry, Antagonist, chemistry.chemical_element, Mean age, Calcium, Crossover study, Raynaud's phenomenon, Rheumatology, Underlying disease, chemistry, Internal medicine, medicine, Amlodipine, Pharmacology (medical), In patient, business, medicine.drug
Abstract

Treatment with calcium antagonists has been shown to be beneficial in patients with primary and secondary Raynaud’s phenomenon. A double-blind placebo-controlled crossover trial was performed to assess the efficacy of amlodipine, a new long-acting calcium antagonist, in patients with Raynaud’s phenomenon without underlying disease. 20 of the 24 patients enrolled (20 women and 4 men, mean age 45 years) completed the trial.

Published
1993

38. Search For 100 Tev Gamma-ray Emission From the Galactic Disk

Author

G.C. Trinchero, G. Mannocchi, A. Campos Fauth, O. Saavedra, P.L. Ghia, L. Riccati, Carlotta Castagnoli, C. Cattadori, A. Castellina, F. Arneodo, P. Vallania, M. Aglietta, W. Fulgione, G. Cini, L. Bergamasco, B. D'Ettorre Piazzoli, A. Chiavassa, Bruno Alessandro, P. Galeotti, C. Morello, S. Vernetto, and G. Navarra

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Milky Way, Bremsstrahlung, Gamma ray, Astronomy and Astrophysics, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spectral line, Interstellar medium, Space and Planetary Science, Emission spectrum, Disc, Astrophysics::Galaxy Astrophysics
Abstract

Upper limits have been obtained to the diffuse gamma-ray emission from the Galactic disk. The limits I(gamma)/I(p) less than 0.2 percent, i.e., I(gamma)(greater than 130 TeV) less than 3.2 x 10 exp -13/q cm/s/rad provide the first measurement obtained in the angular window corresponding to the distribution of the ISM. It is still, however, a factor of about 30 higher than the flux calculated from the cosmic ray interactions by Berezinsky and Kudryavtsev (1990). A lower limit of gamma greater than 2.3 is obtained to the power-law index of the differential energy spectrum of Galactic gamma rays from 100 MeV to 100 TeV, setting a limit to the possibility of a hard extrapolation of the Galactic gamma-ray spectrum to the 100 TeV region. 21 refs.

Published
1992

43. A Measurement of the Solar and Sidereal Cosmic-Ray Anisotropy at E 0 approximately 10 14 eV

Author

M. Aglietta, B. Alessandro, P. Antonioli, F. Arneodo, L. Bergamasco, M. Bertaina, A. Bosio, A. Castellina, C. Castagnoli, A. Chiavassa, G. Cini Castagnoli, B. D'Ettorre Piazzoli, G. di Sciascio, W. Fulgione, P. Galeotti, P. L. Ghia, M. Iacovacci, G. Mannocchi, C. Melagrana, N. Mengotti Silva, C. Morello, G. Navarra, L. Riccati, O. Saavedra, G. C. Trinchero, P. Vallania, S. Vernetto, and null EAS-Top Collaboration

Subjects
Physics, Space and Planetary Science, Sidereal time, Astronomy, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Anisotropy
Published
1996
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44. Search for Gamma-Ray Bursts at Photon Energies E >= 10 GeV and E >= 80 TeV

Author

W. Fulgione, Carlotta Castagnoli, Pietro Antonioli, F. Arneodo, P. Vallania, A. Castellina, C. Morello, M. Aglietta, G. Cini Castagnoli, R. Granella, M. E. Bertaina, G. Mannocchi, C. Melagrana, M. Iacovacci, N. Mengotti Silva, S. Vernetto, B. D'Ettorre Piazzoli, Bruno Alessandro, G. Navarra, P.L. Ghia, L. Riccati, Carlo Vigorito, G. Di Sciascio, L. Bergamasco, G.C. Trinchero, P. Galeotti, O. Saavedra, A. Chiavassa, M., Aglietta, B., Alessandro, P., Antonioli, F., Arneodo, L., Bergamasco, M., Bertaina, A., Castellina, C., Castagnoli, A., Chiavassa, G. C., Castagnoli, D'ETTORRE PIAZZOLI, Benedetto, G., Disciascio, W., Fulgione, P., Galeotti, P. L., Ghia, R., Granella, Iacovacci, Michele, G., Mannocchi, C., Melagrana, N. M., Silva, C., Morello, G., Navarra, L., Riccati, O., Saavedra, G. C., Trinchero, P., Vallania, S., Vernetto, and C., Vigorito

Subjects
Nuclear physics, Physics, Photon, Space and Planetary Science, Astronomy and Astrophysics, EASTOP experiment, Gamma-ray burst, GRB search
Abstract

The EAS-TOP extensive air shower array has been operating since 1992 in the search for gamma-ray bursts at primary energies E(1) greater than or equal to 10 GeV and E(2) greater than or equal to 80 TeV. The study is performed by searching for short transients in the cosmic-ray intensity in the single particle (E(1)) and extensive air shower (E(2)) counting rates at mountain altitude (2005 m above sea level). We discuss the method and the results obtained both in sky survey and in correlation with BATSE events. In both energy ranges, the observed fluctuations in the event rate obtained in the sky survey during similar to 800 days of live time are compatible with the statistical fluctuations of the cosmic-ray background. A single candidate of time duration Delta t similar to 2 s and energy fluence F(10 < E < 100 GeV) = 1.7 x 10(-4)/(cos theta)(10.5) ergs cm(-2) (where theta is the unknown zenith angle) has been observed on 1992 July 15 at 13:22:26 UT in the energy range E(1) greater than or equal to 10 GeV with significance 10.6 and 20.1 sigma in two measurement channels. In the analysis made in correlation with similar to 50 events detected by BATSE, no burst candidate was found in time coincidence or in the 2 hr interval, around the BATSE detection time. The following ranges of upper limits F-max to the energy fluence in the time interval Delta t(90) in which BATSE detected 90% of the counts are obtained: F-max = 2.3 x 10(-5)-7.4 x 10(-3) ergs cm(-2) (10 < E < 100 GeV) F-max = 1.6 x 10(-6)-3.3 x 10(-5) ergs cm(-2) (100 < E < 1000 TeV).

Published
1996
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48. Long term solar-terrestrial records from sediments: carbon isotopes in planktonic foraminifera during the last millennium

Author

Castagnoli, G. Cini, Bonino, G., and Taricco, C.

Subjects
*SOLAR-terrestrial physics, *NUCLEAR activation analysis
Abstract

We show the δ13C profile of Globigerinoides ruber measured in the GT90/3 shallow-water Ionian sea core. This core is dated with high accuracy (better than 1%) using radiometric and tephroanalysis methods, for the last 2000 years. The core, extracted from the Gallipoli platform, was sampled at contiguous steps of thickness 2.5 mm, corresponding to 3.87 years. The δ13C profile covers the period 1147–1975 AD. During the first seven centuries it appears fairly flat, while it shows a steep increase between 1760 and 1950 of ∼0.3‰. The analysis of the time series performed using different methods shows a dominant decadal periodicity throughout the record. The 11-year component is identified at high significance level by Monte Carlo singular spectrum analysis (MC-SSA); the SSA-reconstructed-11-year component is in phase with the sunspot solar cycle. The average amplitude of this component is A11y=0.04‰. It is commonly accepted that δ13C variations in symbiontic foraminifera mainly record the effects of symbiont density and of photosynthetic activity, varying with ambient light level. The δ13C peak-to-trough 11-year variation (0.08‰) can be related to solar irradiance variation of 0.1% on decadal time scale, like that measured in space in the last 20 years. By supposing that the observed δ13C modern increase of ∼0.3‰ is also produced by a solar irradiance variability on a longer time scale, through the same mechanisms, we estimate a secular increase of the total solar irradiance between 1760 and 1950 of (0.3/0.08)&ast;0.1% ≅ 0.37%. This value is at the higher limit of the long term variability estimates (0.25%–0.35%) that are currently proposed.Finally, in the light of the available experimental evidences, we discuss possible ways in which direct solar forcing can be modified by atmospheric processes in order to give the observed δ13C signal. [Copyright &y& Elsevier]

Published
2002
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