Welcome to my WebPage.

I am an astronomer working at the Osservatorio Astrofisico di Arcetri, in Italy. I study relativistic magneto-hydrodynamics, relativistic winds, compact objects like Pulsars, and Neutron Stars, and X-rays. I am involved in the development of numerical algorithms for the study of fluids in Special and General Relativity, and for the modelling of magnetized Neutron Stars.
I also teach the High Energy Astrophysics class at the University of Firenze. Finally, I am in charge of the Outreach program of my Institute.

My Asteroid

The Asteroid 235999 has been named "Bucciantini" after me. My thanks to the "Gruppo Astrofili Montagna Pistoiese" for this great gift. It sits somewhere between Mars and Jupiter (search for 235999).


A PostDoc Abroad

In recent years, a small but steadily increasing number of funding programs have been put in place to help postdocs pursue their own research projects while remaining in someone else's lab. One such program--the Hubble Fellowships offered by NASA--has given Italian astronomer Niccolò Bucciantini unprecedented independence......


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«NON MI SONO mai sentito un cervello in fuga». Parola di Niccolò Bucciantini, astrofisico, 38 anni, aglianese trasferito a San Casciano Val di Pesa, ricercatore permanente all’osservatorio fiorentino di Arcetri dopo avere svolto progetti di ricerca negli Usa e in Svezia e tenuto conferenze in tutto il mondo. A 23 anni laurea in fisica ....


Magnetic Field Structure and Faraday Rotation of the Plerionic Supernova Remnant G21.5-0.9

We present a polarimetric study of the pulsar wind nebula (PWN) in supernova remnant G21.5-0.9, using archival Very Large Array data taken at 5 and 7.4 GHz. The rotation measure (RM) map of the PWN shows a symmetric pattern that aligns with the presumed pulsar spin axis direction, implying a significant contribution to the RM from the nebula. We suggest that the spatial variation of the internal RM is mostly caused by the nonuniform distribution of electrons originating from the supernova ejecta. Our high-resolution radio polarization .... [...]

Lai, P.C.W.. et al. 2022, ApJ, 930, 1

Revisiting the evolution of non-radiative supernova remnants: a hydrodynamical-informed parametrization of the shock positions

Understanding the evolution of a supernova remnant shell in time is fundamental. Such understanding is critical to build reliable models of the dynamics of the supernova remnant shell interaction with any pulsar wind nebula it might contain. Here, we perform a large study of the parameter space for the 1D spherically symmetric evolution of a supernova remnant, accompanying it by analytical analysis. Assuming, as is usual, an ejecta density profile with a power-law core and an envelope, and a uniform ambient medium, we provide a set of highly accurate approximations ..... [...]

R. Bandiera et al., 2022, MNRAS, 508, 3194

Formation and evaporation of strangelets during the merger of two compact stars

We study the partial fragmentation of a strange quark star into strangelets during the process of merger of two strange quark stars. We discuss the fate of the fragments considering their possible evaporation into nucleons. We show that only a rather small amount of large size strangelets, ejected from the spiral arms in the post-merger, survives a total evaporation into nucleons. In this way we demonstrate that: 1) the density of strangelets in the galaxy is too low to trigger the conversion of all neutron stars into strange quark stars ...... [...]

N. Bucciantini et al., 2022, PRD in press