## Alessandro SPALLICCI

ALESSANDRO SPALLICCI

Professeur des Universités

en Astronomie et Astrophysique

Université d'Orléans

Observatoire des Sciences de l'Univers

LPC2E CNRS

3A, Avenue de la Recherche Scientifique

45071 Orléans France

alessandro.spallicci@cnrs-orleans.fr

+ 33 238 25 78 32 (office Orléans)

French Chair at the Universidade do Estado de Rio de Janeiro

Erasmus responsible Orléans Napoli Federico II

At the Université d'Orléans from 2006 - then just 700 years old since its creation in 1306 - after having spent a period at the Observatoire de la Côte d’Azur as recipient of the Giuseppe Colombo prize, I have previously held professorships in my home town Alessandria, but also Benevento and Salerno - the first university in the modern sense is believed by some to have been the medical school founded in the 9th century at Salerno [pdf] - and worked at the European Space Research & Technology Centre in Noordwijk (ESTEC). Space as laboratory to test current or propose new foundations for physics abides by my vision of astrophysics. I have therefore pursued my investigations covering topics from theoretical physics to space experiments through fundamental metrology, publishing in a variety of scientific journals.## BREAKING NEWS

- Selection of a gravitational wave mission by ESA. For info LISA France and the eLISA website

- Italians (could hardly) do it better, often without a salary.

Number of publications and citations for researcher.

## RESEARCH

General Relativity and Fundamental (Astro-)Physics

Relativistic motion of compacts stars accreted by supermassive black holes; self-force and gravitational waves; non-Maxwellian theories of electromagnetism; fundamental physics with Time & Frequency measurements, pulsars, and space plasma.

CNU 34 keywords: astroparticules, hautes énergies, missions spatiales, objets compacts

SELECTED PUBLICATIONS

Editor

Refereed journals

- [DO1] Blanchet L., SPALLICCI A., Whiting B., 2011. Mass and motion in general relativity, Springer Series on Fundamental Theories of Physics, ISBN: 978-90-481-3014-6. Contributions by Barack, Blanchet, Burko, Damour, Davis, Detweiler, Djouadi, Esposito-Farèse, Gal’tsov, Gourgoulhon, Gralla, Jaekel, Jaramillo, Jennrich, Lämmerzahl, Le Tiec, Nagar, Noui, Poisson, Reynaud, Schäfer, Spallicci, Wald, Whiting. 600 pages, available at Springer.
- [OS1] SPALLICCI A., 2011. Free fall and self-force: an historical perspective, in Mass and motion in general relativity, Springer Series on Fundamental Theories of Physics, Blanchet L., SPALLICCI A., Whiting B. Eds., ISBN: 978-90-481-3014-6. arXiv:1005.0611 [physics.hist-ph]

- [ACL1] SPALLICCI A., 1990. Orbiting test masses for equivalence principle space experiment, Gen. Rel. Grav., 22, 863.
- [ACL2] SPALLICCI A., 1991. The fifth force in the Schwarzschild metric, in the field equations and the concept of parageodesic motions, Ann. Phys. (Leipzig), 48, 365.
- [ACL3] SPALLICCI A., Brillet A., Busca G., Fuligni F., Nobili A., Roxburgh I., 1993. Equivalence principle, constant of gravitation, special and general relativity experiments in the Columbus program, Class. Q. Grav., 10, S259.
- [ACL4] SPALLICCI A., 1995. Relativistic time and frequency measurements for spacecraft users of GPS system, Aerotec. Missili Spazio, 74, 41.
- [ACL5] Ferraris M., Francaviglia M., SPALLICCI A., 1996. Associated radius, energy and pressure of McVittie's metric, in its astrophysical application, N. Cimento B, 111, 1031.
- [ACL6] SPALLICCI A., Graf E., Perino M., Matteoni M., Piras A., Arduini C., Catastini G., Ellmers F., Hall D., Härendel G., Nobili A., Iess L., Pinto I., Stöcker J., 1997. Microsatellites and space station for science and technology utilization, Acta Astron., 39, 605.
- [ACL7] SPALLICCI A., Krolak A., Frossati G., 1997. Coalescing binaries and large band resonant spherical detectors, Class. Q. Grav., 14, 577.
- [ACL 8] SPALLICCI A., Brillet A., Busca G., Catastini G., Pinto I., Roxburgh I., Salomon C., Soffel M., Veillet C., 1997. Experiments on fundamental physics on the Space Station, Class. Q. Grav. 14, 2971.
- [ACL 9] SPALLICCI A., 1998. Mathematical methods for quasi-static components of natural perturbative accelerations in microgravity environment analysis, J. Spacecraft Techn., 8, 88.
- [ACL 10] Pierro V., Pinto I., SPALLICCI A., Laserra A., Recano F., 2001. Fast and accurate computational tools for gravitational waveforms from binary systems with any orbital eccentricity, Mon. Not. Roy. Astr. Soc., 325, 358. arXiv:gr-qc/0005044
- [ACL 11] Pierro V., Pinto I., SPALLICCI A., 2002. Computation of hyperngeometric functions for gravitationally radiating binary stars, Mon. Not. Roy. Astr. Soc., 334, 855.
- [ACL 12] SPALLICCI A. Aoudia S., 2004. Perturbation method in the assessment of radiation reaction in the capture of stars by black holes, Class. Q. Grav., 21, S563. arXiv:gr-qc/0309039
- [ACL 13] Ferraris M., SPALLICCI A., 2004. Solutions of all one-dimensional wave equations with time independent potential and separable variables, Gen. Rel. Grav., 36, 1955. arXiv:gr-qc/0309038
- [ACL 14] SPALLICCI A., 2004. Satellite measurement of the Hannay angle, N. Cimento B, 119, 1215. arXiv:astro-ph/0409471
- [ACL 15] SPALLICCI A, Morbidelli A., Metris G., 2005. The three-body problem and the Hannay angle, Nonlinearity, 18, 45. arXiv:astro-ph/0312551
- [ACL 17] Chauvineau B., SPALLICCI A., Fournier J.-D., 2005. Brans-Dicke gravity in the capture of stars by black holes: some asymptotic results, Class. Q. Grav., 22, S457. arXiv:gr-qc/0412053
- [ACL 18] SPALLICCI A., Aoudia S., de Freitas Pacheco J., Regimbau T, Frossati G., 2005. Virgo detector optimization for gravitational waves by coalescing binaries, Class. Q. Grav., 22, S461. arXiv:gr-qc/0406076
- [ACL 21] Regimbau T., de Freitas Pacheco J., SPALLICCI A., Vincent S., 2005. Expected coalescence rates of double neutron stars for ground interferometers, Class. Q. Grav., 22, S935. arXiv:gr-qc/0506058
- [ACL 34] de Freitas Pacheco J., Regimbau T., Vincent S., SPALLICCI A., 2006. Expected coalescence rates of NS-NS binaries for laser beam interferometers, Int. J. Mod. Phys, 15, 235. arXiv:astro-ph/0510727
- [ACL 56] Aoudia S., SPALLICCI A., 2011. A source-free integration method for black hole perturbations and self-force computation: Radial fall, Phys. Rev. D, 83, 064029. arXiv:1008.2507 [gr-qc]
- [ACL 57] Ritter P., SPALLICCI A., Aoudia S., Cordier S., 2011. Fourth order indirect integration method for black hole perturbations: even modes, Class. Q. Grav., 28, 134012. arXiv:1102.2404 [gr-qc]
- [ACL 58] SPALLICCI A., 2013. On the complementarity of pulsar timing and space laser interferometry for the individual detection of supermassive black hole binaries, Astrophys. J., 764, 187. arXiv:1107.5984 [gr-qc]
- [ACL 59] SPALLICCI A., Ritter P., Aoudia S., 2014. Self-force driven motion in curved spacetime, Int. J. Geom. Meth. Mod. Phys., 11, 1450072. arXiv:1405.4155 [gr-qc]
- [ACL 60] SPALLICCI A., Ritter P., 2014. A fully relativistic radial fall, to appear in Int. J. Geom. Meth. Mod. Phys. (invited). arXiv:1407.5391 [gr-qc]
- [ACL 61] Retinò A., SPALLICCI A., Vaivads A., 2014. Solar wind test of the de Broglie-Proca's massive photon with Cluster multi-spacecraft data, arXiv:1302.6168 [hep-ph]
- [ACL 62] SPALLICCI A., 2014. The non-uniqueness of free fall and the relativistic Pisa tower, submitted.
- [ACL 63] Ritter P., SPALLICCI A., Aoudia S., Cordier S. 2014. An (indirect) source-free integration method for EMRIs: geodesic waveforms from generic orbits and self-force consistent radial fall, in preparation.
- [ACL 64] Perez-Bergliaffa S., Bonetti L., SPALLICCI A., The Euler-Heisenberg red-shift in magnetars, in preparation.
- [ACL 65] SPALLICCI A. Relativistic kick and entropy, in preparation.
- [ACL 66] SPALLICCI A. Tired light: the fundamental physics constraints, in preparation.
- [ACL 67] Bonetti L., Perez-Bergliaffa S., SPALLICCI A., Radiation reaction in non-Maxwellian electromagnetism, in preparation.
- [ACL 68] SPALLICCI A., Bonetti L., Helayël-Neto J., Perez-Bergliaffa S. Light propagation in non-Maxwellian theories, in preparation.
- [ACL 69] Ferraris M., SPALLICCI A., Spacetime matching by transition metrics, in preparation.
## THE ORLEANS LISA TEAM

- Alessandro D.A.M. Spallicci, PR, spallicci@cnrs-orleans.fr (Theoretical and Fundamental (Astro)Physics, Relativity) Université d’Orléans, Obs. Sciences Univers, LPC2E Webpage
- Stéphane Cordier, PR, stephane.cordier@math.cnrs.fr (Algorithmics, Partial Differential Equations, Modelling) Université d’Orléans, MAPMO Webpage
- Richard Emilion, PR, richard.emilion@univ-orleans.fr (Data analysis, Statistics) Université d’Orléans, MAPMO Webpage
- Sylvain Jubertie, MdC, sylvain.jubertie@univorléans.fr, (Parallel Computing, Informatics) Université d’Orléans, LIFO Webpage
- Patxi Ritter, Post-doc, patxi.ritter@cnrs-orleans.fr (Astrophysics, Numerical Computation) Université d’Orléans, LPC2E-MAPMO Webpage
- Luca Bonetti, Doctorate student, luca.bonetti@cnrs-orleans.fr (Theoretical Physics, Cosmology) Université d’Orléans, LPC2E
## ON-GOING WORKS

Towards a self-consistent orbital evolution for EMRIs

S. Aoudia (MPI Golm), S. Cordier (MAPMO Orléans), S. Jubertie (LIFO Orléans), S. Limet (LIFO Orléans), P. Ritter (LPC2E-MAPMO Orléans), A. Spallicci (LPC2E Orléans)

We intend to develop part of the theoretical tools needed for the detection of gravitational waves coming from the capture of a compact object, 1-100 solar masses, by a Supermassive Black Hole (SMBH), up to a billion solar masses, located at the centres of most galaxies. The analysis of the accretion activity of SBMHs unveils the star population around the galactic nuclei, and tests the physics of black holes and motion in general relativity. In this context, we focus on the implications of radiation reaction (self-force), complex and traditional problem of general relativity, on the eLISA-NGO project. The captured small mass is considered a probe of the gravitational field of the massive body, allowing a precise measurement of its motion up to the final absorption by the SMBH. The knowledge of the gravitational signal, strongly affected by radiation reaction - the orbital displacement due to gravitational radiation emission - is imperative for a successful detection by eLISA-NGO. At Orléans (a CNRS school on Mass and the Capra conference in 2008, two doctorate thesis, master stages and scientific visits, a topical book and recent publications), the results include an efficient computational strategy for wave equations with singular source terms for all type of orbits. We are now tackling the evolution problem, first for radial orbit in Regge-Wheeler gauge, and later we will consider generic orbits in de Donder (harmonic) gauge for Schwarzschild-Droste black holes. In the Extreme Mass Ratio Inspiral (EMRI) two-body problem, the determination of the orbital evolution demands that the motion of the small mass be continuously corrected by the self-force, i.e. the self-consistent evolution. The latter has been evoked by S. Gralla and R. Wald, but yet not implemented. The project wishes to stretch beyond the first applications, up to encompassing any non-adiabatic orbit in non-rotating SMBH geometry, though it is desirable that the acquired expertise serves as a future path for stepping towards rotating SMBHs. The objective being the first description ever of a self-consistent evolved orbit, any partial accomplishment along this road constitutes an achievement at this time. Subtle gauge issues may render the task difficult to handle. Numerically, a self-consistent approach is a cumbersome task. At each of the integration steps, the self-force must be computed over an adequate number of modes; further, a complex differential-integral system of general relativistic equations is to be solved and the outputs regularised for suppressing divergences. For provision of the computational power needed to solve the EMRI problem, several levels of parallelisation are to consider: a parametric computation level, i.e. several simulations running with different inputs parameters; a data parallel level i.e. splitting the domain into sub-domains; a task parallel level to solve independent modes required to compute the self-force. Multi-scale modelling techniques are also considered, since the computation time of the integration steps is tied to the locality of the particle, while radiation is also evaluated at infinity.

Solar wind test of the de Broglie-Proca's massive photon with Cluster multi-spacecraft data

A. Retinò (LPP Paris), A. Spallicci (LPC2E Orléans), A. Vaivads (IRF Uppsala)

We use spacecraft data in the solar wind at 1 AU to estimate the mass upper limit of the de Broglie-Proca’s photon, by looking for deviations from the Ampère’s law. We take advantage of the Cluster spacecraft which both allow the direct computation of curl B from simultaneous four-point measurements of the magnetic field and provide measurements of particle currents. We estimate the upper bound for the mass m? to be 1.4 × 10-49 kg, without using any ad-hoc model. Finally, we discuss how this limit can be lowered and compare with currently accepted values in the solar wind.

Laboratory experiment on photon frequency stability through a Kennedy-Thorndike interferometer

A. Spallicci (LPC2E Orléans) + ...

Under construction.

Non-Maxwellian theories

J.A. Helaÿel Neto (CBPF Rio de Janeiro), S.E. Perez Bergliaffa (UERJ Rio de Janeiro), A. Spallicci (LPC2E Orléans)

Non-linear theories

Linear theories, such as Maxwell´s Electro-Magnetism (EM), are useful in a wide range of applications. However, non-linear theories such as hydrodynamics, gravity, quantum electrodynamics, and quantum chromodynamics are unavoidable in the description of many physical situations. In particular, non-linear theories constitute a branch of classical and quantum field theories relevant in a variety of theoretical and observational situations, see for instance [Goulart and Perez Bergliaffa, 2011] and references therein. From its conception [Born and Infeld, 1934], non-linear theories have been at the heart of the description of a plethora of phenomena. On the theoretical side: string theory [Gibbons and Herdeiro, 2001], hairy black holes [Bretón, 2005], and the effective metric [De Lorenci, 2000], vacuum polarization [Heisenberg and Euler, 1936] - and its effects on wave propagation both in flat [De Lorenci et al., 2002] and curved spacetimes [Hollowood and Shore G., 2008]; these latter works address vacuum polarization predicted by quantum electrodynamics. On the observational side, magnetars [Gualtieri et al., 2011] and the PVLAS experiment [Bregant M. et al., 2008] and, on a more speculative vein, superconducting cosmic strings [Hartmann and Carter, 2008]. In some cases, the analysis was fairly general, by working with an unspecified Lagrangian, while in others a specific Lagrangian was used. In both cases, the U(1) gauge symmetry was preserved. It is also worthwhile to consider other extensions of Maxwell’s EM, dictated by the way in which fundamental theories and models for the most elementary fields of Nature and their unification are constructed. The dynamics of superstring theories, for instance, may induce Lorentz symmetry violation and this, in turn, may affect Electro-Dynamics and the Standard Model itself, as currently discussed in the literature [Kostelecký and Samuel, 1989; Aguilar-Arevalo A. et al., 2010].

Massive photon theories

The photon and the graviton, i.e. the bosons of the eldest forces discovered, are supposed to be massless particles in the Standard Model. In connection with Supersymmetry and Loop Quantum Gravity [Gambini and Pullin, 1999], the discussion of extended electromagnetic theories with the appearance of massive photons and/or photinos becomes a relevant matter. A partial list of the extensions of Maxwell’s EM along these lines includes: de Broglie-Proca, magnetic monopoles, Maxwell–Kalb–Ramond, the electrodynamical sector of the Standard Model Extension, Myers–Pospel, Gambini-Pullin, Axionic, Supersymmetry with Lorentz symmetry violation, Horava; other (older) massive photon theories include that of Carrol et al. [1990]. Breaking of gauge invariance is not obligatory. Stueckelberg (1938 a,b,c; 1957) has made the first successful attempt to overcome this problem by adding a scalar field; for the same purpose, Podolsky [1942; and Kikuchi, 1944; and Schwed, 1948], uses higher derivatives of the gauge field in the Lagrangian; Chern and Simons [1974] propose an electrodynamics that couple the field and the potential in the Lagrangian through the Levi-Civita tensor. In these models, the dispersion relations may point to the presence of a massive photon, which, if Supersymmetry is also present, appears accompanied by a massive photino [Myers and Pospelov, 2003; Nibbelink and Pospelov, 2005; Bolokhov and Pospelov, 2008]. It becomes relevant to identify a possible fundamental mechanism behind the emergence of a massive photon and to relate the photon mass to some parameter or energy scale dictated by some more fundamental theory which the massive model stems from.

Some consequences of non-Maxwellian theories

The consequences of non-Maxwellian theories may concern most important topics, among which the standard model, the Higgs boson, the cosmic microwave background, the Hubble law, dark matter and dark energy. Herein, we address one experimental consequence of non Maxwellian theories on condensed matter physics, and one implications on high energy astrophysics. Recently non-Maxwellian regime for the electromagnetic interactions has been boosted in connection with the so-called topological states of matter. New materials – the so-called topological insulators [Qi and Zhang, 2011] – were theoretically predicted in 2008 and, are now a reality for condensed matter physics. To understand the behaviour of such materials, Electrodynamics in a non-Maxwellian regime is required; more specifically, Axionic Electrodynamics [Wilczek, 1987] may account for many peculiar aspects of this new category of materials. Also recently, Qi et al. [2012] have written a very stimulating paper on the possibility of building up another class of new material in the category of matter in its topological state: the topological superconductors. The latter are still to be physically realised in a laboratory. Here, the non-Maxwellian dynamics underneath electromagnetic interactions relies on a 5-dimensional Chern-Simons theory, intrinsically non-linear; further, a massive photon emerges in connection with the Meissner and Josephson effects. In view of these very recent and far-reaching new scenarios for the electromagnetic interactions, it would be natural to pursue an investigation of the direct consequences of these new proposals on the Maxwell equations: Gauss law for the electric field and Ampère-Maxwell equation for the magnetic field receive new terms and non-linearity becomes relevant. In the presence of very strong magnetic fields produced by astrophysical structures, the effects of non-linearity may be suitably enhanced and may drive new phenomena at a very large scale. This motivates an in depth study of the possible macroscopic effects of extensions of Electrodynamics dictated by some fundamental theories, as it is the case of the QCD-inspired Axionic Electrodynamics and the 5-dimensional Chern-Simons version of Electromagnetism. A non-trivial set of photon dispersion relations may be generated in these extended models and the appearance of extra neutral gauge bosons may be a particular feature to be understood, and further exploited in connection with Astrophysics in the X- and gamma-ray regions of the spectrum [Cocuroci et al., 2013]. A reassessment of topological defects in these new scenarios, and its possible consequences on the study of large scale structures, is a rich and open problem.

de Broglie-Proca (dB-P) theory

From the dB-P Lagrangian, it is possible to evince the Maxwell modified laws. Two laws are modified with respect to the original Maxwell laws: the curl of the magnetic field (Ampère, 1826; Maxwell, 1861) and the divergence of the electric field (Gauss, 1840). The dates of these 19th century publications are in striking contrast with those related to the sophisticated, complex and multi-parameterised modern physical (and cosmological) theories of our current days. The dB-P theory is Lorentz invariant but not Lorenz invariant due to the presence of the potential (scalar and vector components) in the equations.

Testable predictions of dB-P theory

Schrödinger (1941, 1943a, 1943b; Bass and Schrödinger, 1955) emphasized the link between photon mass and a finite range of static forces, à la Yukawa. A small mass needs a very precise experiment. Alternatively, since a small mass is associated to a very large (reduced) Compton wavelength, a very large apparatus. A precise experiment can measure very small deviations from unity in a slowly falling exponential, while a very large apparatus has the advantage of having a large exponential fall-off versus unity. One of the predictions of the dB-P theory is the different speed that photons of different frequencies would travel at. More precisely the lower energy photons would travel at lower speed than those at higher energies. This prediction imposes a dispersion plasma like behaviour. One opportunity of measurement could be in principle be provided by pulsar timing. Indeed, different arrival times according to the wavelengths of the incoming photons are routinely measured, but lacking any other independent measurement on the electron density, the differences are solely attributed to plasma dispersion. In other words, if photons were to behave according to dB-P theory, such effect would be anyhow masked by, and interpreted as, dispersion from plasma (Tu et al., 2005). The limit set by Bay and White (1972) is 3 x 10^{-49} kg. Incidentally, this prediction is of opposite proportionality to that associated to some of the theories in loop quantum gravity (higher energy photon travelling at lower speed), which were discussed in the context of Gamma Ray Bursts and the Fermi satellite (Abdo et al., 2009; Amelino-Camelia, 2009). The other testable predictions concern the modified Maxwell laws. The divergence of the electric field has led Williams et al. (1971) to estimate a mass below 2 x 10^{-50} kg.

We are investigating the modified Ampére’s law (see above).

Complementarity of pulsar timing and space laser interferometry for the individual detection of supermassive black hole binaries

A. Spallicci (LPC2E Orléans)

Gravitational waves coming from Super Massive Black Hole Binaries (SMBHBs) are targeted by both Pulsar Timing Array (PTA) and Space Laser Interferometry (SLI). The possibility of a { single} SMBHB being tracked first by PTA, through inspiral, and later by SLI, up to { merger} and { ring down}, has been previously suggested. Although the bounding parameters are drawn by the current PTA or the upcoming Square Kilometer Array (SKA), and by the New Gravitational Observatory (NGO), derived from the Laser Interferometer Space Antenna (LISA), { this paper also addresses} sequential detection beyond specific project constraints. We consider PTA-SKA, which is sensitive from 10^{-9} to p x 10^{-7} Hz (p=4, 8), and SLI, which operates from s x 10^{-5} up to 1 Hz (s = 1,~~3). A SMBHB in the range 2 x 10^8 - 2 x 10^9 solar masses (the masses are normalised to a (1+z) factor, the red shift lying between z = 0.2 and z=1.5) moves from the PTA-SKA to the SLI band over a period ranging from two months to fifty years. By combining three Super Massive Black Hole (SMBH)-host relations with three accretion prescriptions, nine astrophysical scenarios are formed. They are then related to three levels of pulsar timing residuals (50, 5, 1 ns), generating twenty-seven cases. For residuals of 1 ns, sequential detection probability will never be better than 4.7 x 10^{-4} y^{-2} or 3.3 x 10^{-6} y^{-2} (per year to merger and per year of survey), according to the best and worst astrophysical scenarios, respectively; put differently this means one sequential detection every 46 or 550 years for an equivalent maximum time to merger and duration of the survey. The chances of sequential detection are further reduced by increasing values of the s parameter (they vanish for s = 10) and of the SLI noise, and by decreasing values of the remnant spin. The spread in the predictions diminishes when timing precision is improved or the SLI low frequency cut-off is lowered. So while transit times and the SLI Signal to Noise Ratio (SNR) may be adequate, the likelihood of sequential detection is severely hampered by the current estimates on the number - just an handful - of individual inspirals observable by PTA-SKA, and to a lesser extent by the wide gap between the pulsar timing and space interferometry bands, and by the severe requirements on pulsar timing residuals. Optimisation of future operational scenarios for SKA and SLI is briefly dealt with, since a detection of even a single event would be of paramount importance for the understanding of SMBHBs and of the astrophysical processes connected to their formation and evolution.

## TEACHING

Responsible of the following courses at the Université d'Orléans

- Exploration du milieu spatial et systèmes spatiaux (Master 1)

Intervenants : LPC2E, MAPMO, ESA, CNES- Introduction à la gravitation et à l'astrophysique relativiste (Master 1) [Cours-IGAR.pdf][TD-IGAR.pdf]

Intervenants : LPC2E, MAPMO, IAP Paris- Expériences spatiales en physique fondamentale (Master 2)

Intervenants : LPC2E, IAP Paris, APC Paris, ENS Paris, OCA Grasse- Relativité et physique subatomique (Licence Physique L2, L3) [Cours-RPsA.pdf][rpsa-TD-CC-CT.pdf]

- Physique des (astro-)particules (Ouverture Licence L1, L2, L3)

- Relativité, Sciences spatiales, Astrophysique (Ouverture Licence L1, L2, L3) [Cours-RSSA.pdf]
## CURRICULUM VITAE

Dottore In Ingegneria, Politecnico di Torino, Thesis at Ist. Elettrotecnico Naz. G. Ferraris, Sez. Metrologia Tempo e Frequenza

Dottore in Fisica, Università di Pavia, Thesis at Ist. Fisica Matematica J.-L. Lagrange, Torino

1986-1996 European Space Research and Technology Centre, Noordwijk

1996-1997 Università di Salerno

1997-2001 Università del Sannio di Benevento

1998-2002 Parco Scientifico e Tecnologico di Salerno

2002-2005 Observatoire de la Côte d'Azur, Nice

2005-2006 Università del Piemonte Orientale, Alessandria

2006-present Université d'Orléans

## PRIZES, DISTINCTIONS

Invitation at the E. Fermi Inst. Chicago by S. Chandrasekhar 1995

Visiting Prize NIKHEF-FOM 1998

Nationaal Instituut voor Kernfysica en Hoge-Energie Fysica, Stichting voor Fundamenteel Onderzoek der Materie

ESA European Space Agency Conseiller, 2001-2001

ESA European Space Agency G. Colombo Senior Research Fellow 2002-2004

next

## PROJECTS

next

- SILEX Semi conductor Intersatellite Link Experiment

- ESA Study scientist for Time & Frequency Science Utilization and Space Station Study, Contract 11287/94/NL/VK with Un. Stuttgart, CERGA Grasse, Lab. de Spectroscopie Herzienne ENS Paris, Un. Tübingen (Un. Dresden), Un. München, DLR, DASA-RI. The study has conceived ACES, Atomic Clock Ensemble in Space.

- eLISA/NGO Evolved Laser Interferometer Space Antenna / New Gravitational Wave Observatory. LISA France

- Virgo gravitational wave detector. VESF

## SOME DOCTORATE STUDENTS - POST-DOCS

next

- Vincenzo Pierro, Professore Associato at the Università del Sannio, Benevento

- Sofiane Aoudia, post-doc at the Max Planck Institut für Gravitationphysik A. Einstein, Golm

- Patxi Ritter, Doctorate student from Toulouse, 2010

- Luca Bonetti, Doctorate student from Trento, 2013-

## TEACHING, RESEARCH AND POLITICS IN FRANCE

University Professors are named by the President of the Republic. Though Italian, I was honoured by the former President Jacques Chirac. [pdf]

Foreign researchers are sometime victims of discrimination, as it occurred to one of my previous non-EU students for a visa renewal. Lately, the government had to step back as the Washington Post reports herein.

## USEFUL LINKS

## MY FULL NAME

## NOVELIST

## WHERE I HANG MOST

## SOME RELATIVES

## PEOPLE I HAVE MET

Some people I have met [pdf]

## HOW TO GET TO LPC2E

Visit the page of the CNRS campus (in French) herein. Else, once arrived at one of the stations (Les Aubrais or Gare d'Orléans), get bus n. 7 (ticket in the bus), drop off at the stop "Recherche Scientifique", and then walk for 10-15 minutes, see map. It takes 30-40 minutes from the railway station.

Yes – the springtimes needed you. Often a star was waiting for you to notice it. A wave rolled toward you out of the distant past, or as you walked under an open window, a violin yielded itself to your hearing. All this was mission. But could you accomplish it ?