Stars:abundances; Nuclear reactions, nucleosynthesis and abundances; Atomic data; Hydrodynamics; Stars: AGB and post-AGB; Stars: chemically peculiar; Stars: supernovae; Galaxy: abundances
Mishenina Tamara V., Pignatari Marco, Korotin Sergey A., Soubiran Caroline, Charbonnel Corinne, Thielemann Friedrich Karl, Gorbaneva T. I., Basak N. Yu (2013), Abundances of neutron-capture elements in stars of the Galactic disk substructures, in Astronomy and Astrophysics
, 552, A128.
Praena Juan M., Mastinu Pierfrancesco F., Pignatari Marco, Quesada José Manuel, García-López Javier Hugo, Lozano Manuel, Dzysiuk Nataliya R., Capote Roberto, Martín-Hernández G. (2013), Measurement of the MACS of Ta 181 (n, γ) at kT=30 keV as a test of a method for Maxwellian neutron spectra generation, in Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detecto
, 727, 1-6.
Best Andreas, Beard M., Görres Joachim, Couder Manoel, Deboer R. J., Falahat Sascha, Güray R. T., Kontos Antonios, Kratz Karl Ludwig, Leblanc P. J., Li Q., O'Brien Sheila, Özkan N., Pignatari Marco, Sonnabend Kerstin, Talwar Rashi, Tan Wanpeng, Uberseder Ethan, Wiescher Michael C. (2013), Measurement of the reaction 17O(α,n )20Ne and its impact on the s process in massive stars, in Physical Review C - Nuclear Physics
, 87(4), 045805.
Lederer C., Massimi C., Altstadt S., Andrzejewski J., Audouin L., Barbagallo M., Becares V., Becvar F., Belloni F., Berthoumieux E., Billowes J., Boccone V., Bosnar D., Brugger M., Calviani M., Calvino F., Cano-Ott D., Carrapico C., Cerutti F., Chiaveri E., Chin M., Colonna N., Cortes G., Cortes-Giraldo M. A., Diakaki M. (2013), Neutron Capture Cross Section of Unstable Ni-63: Implications for Stellar Nucleosynthesis, in PHYSICAL REVIEW LETTERS
, 110(2), 022501.
D'Orazi Valentina D Orazi, Campbell Simon W., Lugaro Maria A., Lattanzio John C., Pignatari Marco, Carretta Eugenio (2013), On the internal pollution mechanisms in the globular cluster NGC 6121(M4): Heavy-element abundances and AGB models, in Monthly Notices of the Royal Astronomical Society
, 433(1), 366-381.
Pignatari M., Wiescher M., Timmes F. X., de Boer R. J., Thielemann F. -K., Fryer C., Heger A., Herwig F., Hirschi R. (2013), PRODUCTION OF CARBON-RICH PRESOLAR GRAINS FROM MASSIVE STARS, in ASTROPHYSICAL JOURNAL LETTERS
, 767(2), L22.
Menon Athira, Herwig Falk, Denissenkov Pavel A., Clayton Geoffrey C., Staff Jan, Pignatari Marco, Paxton Bill (2013), REPRODUCING THE OBSERVED ABUNDANCES IN RCB AND HdC STARS WITH POST-DOUBLE-DEGENERATE MERGER MODELS-CONSTRAINTS ON MERGER AND POST-MERGER SIMULATIONS AND PHYSICS PROCESSES, in ASTROPHYSICAL JOURNAL
, 772(1), 59.
Pignatari M., Zinner E., Bertolli M. G., Trappitsch R., Hoppe P., Rauscher T., Fryer C., Herwig F., Hirschi R., Timmes F. X., Thielemann F. -K. (2013), SILICON CARBIDE GRAINS OF TYPE C PROVIDE EVIDENCE FOR THE PRODUCTION OF THE UNSTABLE ISOTOPE Si-32 IN SUPERNOVAE, in ASTROPHYSICAL JOURNAL LETTERS
, 771(1), L7.
Pignatari Marco, Herwig Falk (2013), The NuGrid research platform: a comprehensive simulation approach for nuclear astrophysics, in Nuclear Physics News
, 22(4), 18.
Dressler Rugard, Thielemann Friederich, Pignatari Marco et al. (2012), 44Ti, 26Al and 53Mn samples for nuclear astrophysics: the needs, the possibilities and the sources, in Journal of Physics G
Staff Jan, Menon Athira, Herwig Falk, Pignatari Marco et al. (2012), Do R Coronae Borealis Stars Form from Double White Dwarf Mergers?, in The Astrophysical Journal
Massimi Cristian, Gallino Roberto, Pignatari Marco et al. (2012), Resonance neutron-capture cross sections of stable magnesium isotopes and their astrophysical implications, in Phys. Rev. C
Pignatari M., Hirschi R., Wiescher M., Gallino R., Bennett M., Beard M., Fryer C., Herwig F., Rockefeller G., Timmes F. X. (2012), THE C-12+C-12 REACTION AND THE IMPACT ON NUCLEOSYNTHESIS IN MASSIVE STARS, in ASTROPHYSICAL JOURNAL
, 762(1), 31.
Bennett Michael, Hirschi Raphael, Pignatari Marco, Diehl S., Fryer C., Herwig F., Hungerford A., Nomoto K., Rockefeller G., Timmes F., Wiescher (2012), The effect of 12C +12C rate uncertainties on the evolution and nucleosynthesis of massive stars, in MNRAS
, 420(4), 3047-3070.
Chiappini C, Frischknecht U, Meynet G, Hirschi R, Barbuy B, Pignatari M, Decressin T, Maeder A (2011), Imprints of fast-rotating massive stars in the Galactic Bulge, in Nature
, 472(7344), 454-457.
With the exception of hydrogen and helium, all the other elements in nature that are fundamental for life, like carbon and oxygen, or that we see every day, like iron or silver, are produced in stars.One of the greatest tasks for human knowledge today is to understand how such elements form in stars.A lot of information required to address this question is obtained from stellar spectroscopic observations, where element abundances can be measured in different type of stars in our Galaxy or much further away, at distances billions of kilometers further away from the Earth.Another crucial source of information on how the elements form in stars is hidden in primitive meteorites.Few parts per million of the meteorite material is made of small particles ofdust of presolar origin, that were produced in ancient stars that finished their life before the formation of our solar system.In order to correctly understand all these observations, we need to create computational models of stars to reproduce their evolution, and to correctly simulate all the nuclear processes responsible for the element production.A good knowledge of the nuclear reaction rates is a fundamental requirement to obtain reliable stellar model predictions to compare with observations, since reaction rates control the formation of the elements in the stellar interior. In this cross disciplinary context, involving different disciplines from astrophysics to astronomy, nuclear physics and chemistry, my project for AMBIZIONE is a bridge between all these different fields, addressing in the first instance the fundamental question of how elements form in our galaxy and in the universe. The fundamental goal of my research is to create a comprehensive set of abundances for light and heavy elements produced in stars, enabling me to test stellar model predictions with stellar observations and presolar grains measurements. The central tool to achieve this goal is a new post-processing code called "PPN", able to accurately follow all relevant nuclear processes responsible for element production in stellar conditions.