d36 Alessandro SPALLICCI

Alessandro SPALLICCI


ALESSANDRO D.A.M. SPALLICCI (di Filottrano)
Professeur des Universités (PR1C3)
Astronomie et Astrophysique 2006-2017 (section 34 CNU)
Constituants Élementaires 2017 (section 29 CNU) -->
Université d'Orléans
Observatoire des Sciences de l'Univers
Collegium Sciences et Techniques, Pôle de Physique
===============================================
Office address
Centre Nationale de la Recherche Scientifique
LPC2E, 3A Avenue de la Recherche Scientifique
45071 Orléans France

alessandro.spallicci@cnrs-orleans.fr
+ 33 238 25 78 32 (office Orléans)
+ 33 6 23 15 35 84 (cellular F)
+ 39 331 86 53 942 (cellular I)
+ 55 21 98324 7646 (cellular BR)

lpc2e.cnrs-orleans.fr/~aspallicci/

BREAKING SCIENCE NEWS


DISTINCTIONS AND PRIZES, FUNDING











1986 Grant Centre Européen Recherches Spatiales et Technologiques (ESTEC), Noordwijk (40 k€)
1988 Life-Member of the International Society on General Relativity and Gravitation (ISGRG), Life Member of the Società Italiana di Relatività Generale e Gravitazione ( SIGRAV)
1995 Invitation by S. Chandrasekhar (Chicago) for a stay at Inst. E. Fermi
1998 Prize with J.-W van Holten by the Nationaal Instituut Kernfysika en Hoge-Energie Fysica (NIKHEF) Amsterdam
2000-2001 Conseiller Centre Européen Recherches Spatiales et Technologiques (ESTEC), Noordwijk (20 k€)
2002-2004 Excellence Grant Giuseppe Colombo, Agence Spatiale Européenne (90 k€)
2004-2005 CNRS Research Director (Poste Rouge)
2006 Chair in Astronomy and Astrophysics at the Université d’Orléans by French Presidency Decree
2007–2011 National Prize on Doctorate Students Education and Research (15 k€)
2008-2017 Funding by the Centre National d’Etudes Spatiales (CNES) to the LISA team (LPC2E, MAPMO, LIFO) (30 k€)
2010, 2020, 2021 Local Funding CASCIMODOT for Stages Master
2015- Editor of International Journal of Geometric Methods in Modern Physics (World Scientific) and of Special Issues of Foundation of Physics (Springer)
2015 Promotion to the first class of Professorship
2015-2016 Excellence Grant Eiffel to M. Oltean, Doctorate Student
2016- Pesquisador Visitante at the Centro Brasileiro de Pesquisas Físicas (CBPF), Rio de Janeiro
2017 Chair in Particle Physics at the Université d’Orléans
2014-2015 and 2019-2020 Chaire Française - Ministère des Affaires Etrangères et Universidade do Estado do Rio de Janeiro (UERJ), Instituto de Física, Departamento de Física Teórica (20 k€)
2015, 2017, 2018 et 2019 Erasmus Professor Università di Napoli I Federico II, Dipartimento di Fisica
2019 Funding by the Centre National d’Etudes Spatiales (CNES) for MMS satellite data for photon mass search (3 k€)
2019-2020 Half-Sabbatical CNRS, Laboratoire de Physique et Chimie de l’Environnement et de l’Espace
2021-2022 Half-Sabbatical CNRS, Institut Denis Poisson Laboratoire de Mathématiques et Physique Théorique, Tours
2021-2022 ERASMUS Funding to G. Sarracino, Doctorate Student
2022-2023 Half-Sabbatical UO for Agreement with Università di Napoli I Federico II, Dipartimento di Fisica and Scuola Superiore Meridionale
2022-2025 ANR-DFG Generalised Maxwellian Theories (385 k€) with Bremen

RESEARCH


 RESEARCH KEYWORDS:
15% General Relativity and Gravitation (motion, self-force, gravitational waves, entropy, two-body problem)
75% Non-Maxwellian Electromagnetism (photons and light propagation), Cosmology
10% Fundamental Physics Experiments, Mathematical Physics.

SELECTED PUBLICATIONS
Citations Google Scholar
Editor

  • [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. Downloaded more than 42000 times from 2011.
  • [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]
Refereed journals [ACL 16, 19, 20, 22-33, 35-55 Virgo collaboration papers, not listed here]
  • [ACL1] SPALLICCI A.D.A.M., 1990. Orbiting test masses for equivalence principle space experiment, Gen. Rel. Grav., 22, 863.
  • [ACL2] SPALLICCI A.D.A.M., 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.D.A.M., 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.D.A.M., 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.D., 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 di F. A.D.A.M., 2002. Computation of hyperngeometric functions for gravitationally radiating binary stars, Mon. Not. Roy. Astr. Soc., 334, 855.
  • [ACL 12] SPALLICCI A.D.A.M., 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.D.A.M., 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.D.A.M., 2004. Satellite measurement of the Hannay angle, N. Cimento B, 119, 1215. arXiv:astro-ph/0409471
  • [ACL 15] SPALLICCI A.D.A.M., 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.D.A.M., 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. D, 15, 235. arXiv:astro-ph/0510727
  • [ACL 56] Aoudia S., SPALLICCI A.D.A.M., 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.D.A.M., Aoudia S., Cordier S., 2011. A 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.D.A.M., 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.D.A.M., 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.D.A.M., Ritter P., 2014. A fully relativistic radial fall, Int. J. Geom. Meth. Mod. Phys., 11, 1450090. arXiv:1407.5391 [gr-qc]
  • [ACL 61] Ritter P., Aoudia S., SPALLICCI A.D.A.M., Cordier S.,2016. Indirect (source-free) integration method. I. Waveforms from geodesic generic orbits of EMRIs, Int. J. Geom. Meth. Mod. Phys., 13, 1650021. arXiv:1511.04252 [gr-qc]
  • [ACL 62] Ritter P., Aoudia S., SPALLICCI A.D.A.M., Cordier S. 2016. Indirect (source-free) integration method. II. Self-force consistent radial fall, Int. J. Geom. Meth. Mod. Phys., 13, 1650019. arXiv:1511.04277 [gr-qc]
  • [ACL 63] Bonetti L., Ellis J., Mavromatos N.E., Sakharov A.S., Sarkisyan-Grinbaum E.K.G., SPALLICCI A.D.A.M., 2016. Photon mass limits from Fast Radio Bursts, Phys. Lett. B, 757, 548. arXiv:1602.09135 [astro-ph.HE]
  • [ACL 64] Retinò A., SPALLICCI A.D.A.M., Vaivads A., 2016. Solar wind test of the de Broglie-Proca's massive photon with Cluster multi-spacecraft data, Astropart. Phys., 82, 49. arXiv:1302.6168 [hep-ph]
  • [ACL 65] SPALLICCI A.D.A.M., van Putten M.H.P.M., 2016. Gauge dependence and self-force in Galilean and Einsteinian free falls, Pisa tower and evaporating black holes at general relativity centennial, Int. J. Geom. Meth. Mod. Phys., 13, 1630014, special volume in Memory of Mauro Francaviglia. arXiv:1607.02594 [gr-qc]
  • [ACL 66] Oltean M., Bonetti L., SPALLICCI A.D.A.M., Sopuerta C.F., 2016. Entropy theorems in classical mechanics, general relativity, and the gravitational two-body problem, Phys. Rev. D., 94, 064049. arXiv:1607.03118 [gr-qc]
  • [ACL 67] Bonetti L., dos Santos Luis R., Helayël-Neto A. J., SPALLICCI A.D.A.M., 2017. Effective photon mass from Super and Lorentz symmetry breaking, Phys. Lett. B, 764, 203. arXiv:1607.08786 [hep-ph]
  • [ACL 68] Bentum M., Bonetti L., SPALLICCI A.D.A.M., 2017. Dispersion by pulsars, magnetars and massive electromagnetism at very low radio frequencies, Adv. Space Res, 59, 736. arXiv:1607.08820 [astro-ph.IM]
  • [ACL 69] Bonetti L., Ellis J., Mavromatos N.E., Sakharov A.S., Sarkisyan-Grinbaum E.K.G., SPALLICCI A.D.A.M., 2017. FRB 121102 casts new light on the photon mass, Phys. Lett. B, 768, 326. arXiv:1701.03097 [astro-ph.HE]
  • [ACL 70] Oltean M., Sopuerta C.F., SPALLICCI A.D.A.M., 2017. A frequency-domain implementation of the particle-without-particle approach to EMRIs, J. Phys. Conf. Ser., 840, 01256. arXiv:1703.00865 [gr-qc]
  • [ACL 71] Capozziello S., Prokopec T., SPALLICCI A.D.A.M., 2017. Aims and scopes of the special issue: foundations of astrophysics and cosmology, Found. Phys., 47, 709.
  • [ACL 72] SPALLICCI A.D.A.M., 2017. Comment on “Acceleration of particles to high energy via gravitational repulsion in the Schwarzschild field” [Astropart. Phys. 86 (2017) 18–20], Astropart. Phys., 94, 42. arXiv:1708.00799 [gr-qc]
  • [ACL 73] Bonetti L., dos Santos Filho L.R., Helayël-Neto A.J., SPALLICCI A.D.A.M., 2018. Photon sector analysis of Super and Lorentz symmetry breaking: effective photon mass, tri-refringence and dissipation, Eur. Phys. J. C, 78, 811. arXiv:1709.04995 [hep-th]
  • [ACL 74] Oltean M., Sopuerta C.F., SPALLICCI A.D.A.M., 2019. Particle-without-Particle: a practical pseudospectral collocation method for numerical differential equations with distributional sources, J. Scient. Comp., 79, 827. arXiv:1802.03405 [physics.comp-ph]
  • [ACL 75] Helayël-Neto J.A., SPALLICCI A.D.A.M., 2019. Frequency variation for in vacuo photon propagation in the Standard- Model Extension, Eur. Phys. J. C., 79, 590. arXiv: 1904.11035 [hep-ph]
  • [ACL 76] Oltean M., Epp R.J., Sopuerta C.F., SPALLICCI A.D.A.M., Mann R.B., 2020. The motion of localized sources in general relativity: gravitational self-force from quasilocal conservation laws, Phys. Rev. D., 101, 064060. arXiv: 1907.03012 [gr-qc]
  • [ACL 77] Capozziello S., Benetti M., SPALLICCI A.D.A.M., 2020. Addressing the cosmological H0 tension by the Heisenberg uncertainty, Found. Phys., 50, 893. arXiv:2007.00462 [gr-qc]
  • [ACL 78] Barausse E. et al., 2020. Prospects for fundamental physics with LISA, Gen. Rel. Grav., 52, 81. arXiv:2001.09793 [gr-qc]
  • [ACL 79] SPALLICCI A.D.A.M., Helayël-Neto J.A., López-Corredoira M., Capozziello S., 2021. Cosmology and the massive photon frequency shift induced by the Standard-Model Extension, Eur. Phys. J. C., 81, 4. arXiv: 2011.12608 [astro-ph.CO]
  • [ACL 80] Sesana A. et al., 2021, Unveiling the gravitational universe at µ-Hz frequencies, Exp. Astron., 21, 1333. arXiv: 1908.11391 [astro-ph.IM]
  • [ACL 81] SPALLICCI A.D.A.M., Benetti M., Capozziello S., 2022. Heisenberg limit at cosmological scales, Found. Phys., 52, 23. arXiv: 2112.07359 [physics.gen-ph]
  • [ACL 82] SPALLICCI A.D.A.M., Sarracino G., Capozziello S., 2022. Investigating dark energy by electromagnetism frequency shifts (Special Issue on: Tensions in cosmology from early to late universe: the value of the Hubble constant and the question of dark energy), Eur. Phys. J. Plus, 137, 253. arXiv: 2202.02731[astro-ph.CO]
  • [ACL 83] Arun K.G. et al, 2022. New horizons for fundamental physics with LISA, Liv. Rev. Rel., 25, 4. arXiv:2205.01597 [gr-qc]
  • [ACL 84] Sarracino G., SPALLICCI A.D.A.M., Capozziello S., 2022. Investigating dark energy by electromagnetism frequency shifts (Special Issue on: Tensions in cosmology from early to late universe: the value of the Hubble constant and the question of dark energy), Eur. Phys. J. Plus, 137, 1386. arXiv:2211.11438 [astro-ph.CO]
  • [ACL 85] Capozziello S., Sarracino G., SPALLICCI A.D.A.M., 2023. Questioning the H0 tension via the look-back time, Phys. Dark Univ., 40, 101201. arXiv:2302.13671 [astro-ph.CO]
  • [ACL 86] Amaro-Seoane P. et al., 2023. Astrophysics with the Laser Interferometer Space Antenna, to appear in Liv. Rev. Rel. arXiv:2203.06016 [gr-qc]
  • [ACL 87] SPALLICCI A.D.A.M., Sarracino G., Randriamboarison O., Helayël-Neto J.A., 2023. Testing the Ampère-Maxwell law on the photon mass and Lorentz-Poincaré symmetry violation with MMS multi-spacecraft data. arXiv:2205.02487 [hep-ph]
On-going projects and major contributors (Gravitation)

  • SPALLICCI A.D.A.M. et al., Newtonian free fall learnt at youth, now revisited with an Einsteinian view
  • Ferraris M., SPALLICCI A.D.A.M., Spacetime matching by transition metrics.
On-going projects and major contributors (Non-Maxwellian Electromagnetism, Astrophysics and Cosmology)

  • SPALLICCI A.D.A.M., Helayël-Neto J.A. et al., Photon energy variation for light propagating in vacuo and its effective mass in a general non-linear electromagnetic theory
  • SPALLICCI A.D.A.M. et al., On the singular Klein-Gordon equation and photon frequency dissipation
    • .
  • Chernodub M., Helayël-Neto J.A., Melo J. P., SPALLICCI A.D.A.M., Running photon velocity and Lorentz symmetry breaking in the Standard-Model.
Future projects
  • Stay tuned.

    • LAST ABSTRACTS






  • [ACL 56] Aoudia S., SPALLICCI A.D.A.M., 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]
    Perturbations of Schwarzschild-Droste black holes in the Regge-Wheeler gauge benefit from the availability of a wave equation and from the gauge invariance of the wave function, but lack smoothness. Nevertheless, the even perturbations belong to the C°continuity class, if the wave function and its derivatives satisfy specific conditions on the discontinuities, known as jump conditions, at the particle position. These conditions suggest a new way for dealing with finite element integration in time domain. The forward time value in the upper node of the (t, r*) grid cell is obtained by the linear combination of the three preceding node values and of analytic expressions based on the jump conditions. The numerical integration does not deal directly with the source term, the associated singularities and the potential. This amounts to an indirect integration of the wave equation. The known wave forms at infinity are recovered and the wave function at the particle position is shown. In this series of papers, the radial trajectory is dealt with first, being this method of integration applicable to generic orbits of EMRI (Extreme Mass Ratio Inspiral).

  • [ACL 57] Ritter P., SPALLICCI A.D.A.M., 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]
    On the basis of a recently proposed strategy of finite element integration in time domain for partial differential equations with a singular source term, we present a fourth-order algorithm for non-rotating black hole perturbations in the Regge–Wheeler gauge. Herein, we address even perturbations induced by a particle plunging in. The forward time value at the upper node of the (r*,t) grid cell is obtained by an algebraic sum of (i) the preceding node values of the same cell, (ii) analytic expressions, related to the jump conditions on the wavefunction and its derivatives and (iii) the values of the wavefunction at adjacent cells. In this approach, the numerical integration does not deal with the source and potential terms directly, for cells crossed by the particle world line. This scheme has also been applied to circular and eccentric orbits and it will be the object of a forthcoming publication.

  • [ACL 58] SPALLICCI A.D.A.M., 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]
    Gravitational waves coming from Super Massive Black Hole Binaries (SMBHBs) are targeted by b0th 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 px10^{-7} Hz (p=4-8), and SLI, which operates from sx10^{-5} up to 1 Hz (s = 1-3). A SMBHB in the range 2x10^{8} - 2x10^{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 4.7x10^{-4} y^{-2} or 3.3x10^{-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.

  • [ACL 59] SPALLICCI A.D.A.M., 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]
    We adopt the Dirac-Detweiler-Whiting radiative and regular effective field in curved spacetime. Thereby, we derive straightforwardly the first order perturbative correction to the geodesic of the background in a covariant form, for the extreme mass ratio two-body problem. The correction contains the self-force contribution and a background metric dependent term.

  • [ACL 60] SPALLICCI A.D.A.M., Ritter P., 2014. A fully relativistic radial fall, Int. J. Geom. Meth. Mod. Phys., 11, 1450090. arXiv:1407.5391 [gr-qc]
    Radial fall has historically played a momentous role. It is one of the most classical problems, the solutions of which represent the level of understanding of gravitation in a given epoch. A {\it gedankenexperiment} in a modern frame is given by a small body, like a compact star or a solar mass black hole, captured by a supermassive black hole. The mass of the small body itself and the emission of gravitational radiation cause the departure from the geodesic path due to the back-action, that is the self-force. For radial fall, as any other non-adiabatic motion, the instantaneous identity of the radiated energy and the loss of orbital energy cannot be imposed and provide the perturbed trajectory. In the first part of this letter, we present the effects due to the self-force computed on the geodesic trajectory in the background field. Compared to the latter trajectory, in the Regge-Wheeler, harmonic and all others smoothly related gauges, a far observer concludes that the self-force pushes inward (not outward) the falling body, with a strength proportional to the mass of the small body for a given large mass; further, the same observer notes an higher value of the maximal coordinate velocity, this value being reached earlier on during infall. In the second part of this letter, we implement a self-consistent approach for which the trajectory is iteratively corrected by the self-force, this time computed on osculating geodesics. Finally, we compare the motion driven by the self-force without and with self-consistent orbital evolution. Subtle differences are noticeable, even if self-force effects have hardly the time to accumulate in such a short orbit.

  • [ACL 61] Ritter P., Aoudia S., SPALLICCI A.D.A.M., Cordier S., 2016. Indirect (source-free) integration method. I. Waveforms from geodesic generic orbits of EMRIs, Int. J. Geom. Meth. Mod. Phys., 13, 1650021. arXiv:1511.04252 [gr-qc]
    The Regge-Wheeler-Zerilli (RWZ) wave-equation describes Schwarzschild-Droste black hole perturbations. The source term contains a Dirac distribution and its derivative. We have previously designed a method of integration in time domain. It consists of a finite difference scheme where analytic expressions, dealing with the wave-function discontinuity through the jump conditions, replace the direct integration of the source and the potential. Herein, we successfully apply the same method to the geodesic generic orbits of EMRI (Extreme Mass Ratio Inspiral) sources, at second order. An EMRI is a Compact Star (CS) captured by a Super Massive Black Hole (SMBH). These are considered the best probes for testing gravitation in strong regime. The gravitational wave-forms, the radiated energy and angular momentum at infinity are computed and extensively compared with other methods, for different orbits (circular, elliptic, parabolic, including zoom-whirl).

  • [ACL 62] Ritter P., Aoudia S., SPALLICCI A.D.A.M., Cordier S., 2016. Indirect (source-free) integration method. II. Self-force consistent radial fall, Int. J. Geom. Meth. Mod. Phys., 13, 1650019. arXiv:1511.04277 [gr-qc]
    We apply our method of indirect integration, described in Part I, at fourth order, to the radial fall affected by the self-force. The Mode-Sum regularisation is performed in the Regge-Wheeler gauge using the equivalence with the harmonic gauge for this orbit. We consider also the motion subjected to a self-consistent and iterative correction determined by the self-force through osculating stretches of geodesics. The convergence of the results confirms the validity of the integration method. This work complements and justifies the analysis and the results appeared in Int. J. Geom. Meth. Mod. Phys., 11, 1450090 (2014).

  • [ACL 63] Bonetti L., Ellis J., Mavromatos N.E., Sakharov A.S., Sarkisyan-Grinbaum E.K.G., SPALLICCI A.D.A.M., 2016. Photon mass limits from Fast Radio Bursts, Phys. Lett. B, 757, 548. arXiv:1602.09135 [astro-ph.HE]
    The frequency-dependent time delays in fast radio bursts (FRBs) can be used to constrain the photon mass, if the FRB redshifts are known, but the similarity between the frequency dependences of dispersion due to plasma effects and a photon mass complicates the derivation of a limit on the photon mass. The dispersion measure (DM) of FRB 150418 is known to about 0.1 %, and there is a claim to have measured its redshift with an accuracy of about 2%, but the strength of the constraint on the photon mass is limited by uncertainties in the modelling of the host galaxy and the Milky Way, as well as possible inhomogeneities in the intergalactic medium (IGM). Allowing for these uncertainties, the recent data on FRB 150418 indicate that the photon mass is less than 1.8 x 10^{-14} eV c^{-2} (3.2 x 10^{-50} kg), if FRB 150418 indeed has a redshift z = 0.492 as initially reported. In the future, the different redshift dependences of the plasma and photon mass contributions to DM can be used to improve the sensitivity to the photon mass if more FRB redshifts are measured. For a fixed fractional uncertainty in the extra-galactic contribution to the DM of an FRB, one with a lower redshift would provide greater sensitivity to the photon mass.

  • [ACL 64] Retinò A., SPALLICCI A.D.A.M., Vaivads A., 2016. Solar wind test of the de Broglie-Proca's massive photon with Cluster multi-spacecraft data, Astropart. Phys., 82, 49. arXiv:1302.6168 [hep-ph]
    Our understanding of the universe at large and small scales relies largely on electromagnetic observations. As photons are the messengers, fundamental physics has a concern in testing their properties, including the absence of mass. We use Cluster four spacecraft data in the solar wind at 1 AU to estimate the mass upper limit for the photon. We look for deviations from Ampère's law, through the curlometer technique for the computation of the magnetic field, and through the measurements of ion and electron velocities for the computation of the current. We show that the upper bound for m_\gamma lies between 1.4 x 10^{-49} and 3.4 x 10^{-51}$ kg, and thereby discuss the currently accepted lower limits in the solar wind.

  • [ACL 65] SPALLICCI A.D.A.M., van Putten M.H.P.M., 2016. Gauge dependence and self-force in Galilean and Einsteinian free falls, Pisa tower and evaporating black holes at general relativity centennial, Int. J. Geom. Meth. Mod. Phys., 13, 1630014, special volume in Memory of Mauro Francaviglia. arXiv:1607.02594 [gr-qc]
    Obviously, in Galilean physics, the universality of free fall implies an inertial frame, which in turns implies that the mass m of the falling body is omitted (because it is a test mass; put otherwise, the centre of mass of the system coincides with the centre of the main, and fixed, mass M; or else, we consider only an homogeneous gravitational field). Otherwise, an additional (in the same or opposite direction) acceleration proportional to $m/M$ would rise either for an observer at the centre of mass of the system, or for an observer at a fixed distance from the centre of mass of M. These elementary, but overlooked, considerations fully respect the equivalence principle and the (local) identity of an inertial or a gravitational pull for an observer in the Einstein cabin. They value as fore-runners of the self-force and gauge dependency in general relativity. Because of its importance in teaching and in the history of physics, coupled to the introductory role to Einstein's equivalence principle, the approximate nature of Galilei's law of free fall is explored herein. When stepping into general relativity, we report how the geodesic free fall into a black hole was the subject of an intense debate again centred on coordinate choice. Later, we describe how the infalling mass and the emitted gravitational radiation affect the free fall motion of a body. The general relativistic self-force might be dealt with to perfectly fit into a geodesic conception of motion. Then, embracing quantum mechanics, real black holes are not classical static objects any longer. Free fall has to handle the Hawking radiation, and leads us to new perspectives on the varying mass of the evaporating black hole and on the varying energy of the falling mass. Along the paper, we also estimate our indings for ordinary masses being dropped from a Galilean or Einsteinian Pisa-like tower with respect to the current state of the art drawn from precise measurements in ground and space laboratories, and to the constraints posed by quantum measurements. The appendix describes how education physics and high impact factor journals discuss the free fall. Finally, case studies conducted on undergraduate students and teachers are reviewed.

  • [ACL 66] Oltean M., Bonetti L., SPALLICCI A.D.A.M., Sopuerta C.F., 2016. Entropy theorems in classical mechanics, general relativity, and the gravitational two-body problem, Phys. Rev. D, 94, 064049. arXiv:1607.03118 [gr-qc]
    In classical Hamiltonian theories, entropy may be understood either as a statistical property of canonical systems, or as a mechanical property, that is, as a monotonic function of the phase space along trajectories. In classical mechanics, there are theorems which have been proposed for proving the non-existence of entropy in the latter sense. We explicate, clarify and extend the proofs of these theorems, and then we show why these proofs fail in general relativity; due to properties of the gravitational Hamiltonian and phase space measures, the second law of thermodynamics holds. As a concrete application, we focus on the consequences of these results for the gravitational two-body problem, and in particular, we prove the non-compactness of the phase space of perturbed Schwarzschild-Droste spacetimes. We thus identify the lack of recurring orbits in phase space as a distinct sign of dissipation and thus entropy production

  • [ACL 67] Bonetti L., dos Santos Rodolfo L., Helayël-Neto J., SPALLICCI A.D.A.M., 2017. Effective photon mass from Super and Lorentz symmetry breaking, Phys. Lett. B., 764, 203. arXiv:1607.08786 [hep-ph]
    In the context of Standard Model Extensions (SMEs), we analyse four general classes of Super Symmetry (SuSy) and Lorentz Symmetry (LoSy) breaking, leading to observable imprints at our energy scales. The photon dispersion relations show a non-Maxwellian behaviour for the CPT (Charge-Parity-Time reversal symmetry) odd and even sectors. The group velocities exhibit also a directional dependence with respect to the breaking background vector (odd CPT) or tensor (even CPT). In the former sector, the group velocity may decay following an inverse squared frequency behaviour. Thus, we extract a massive and gauge invariant Carroll-Field-Jackiw photon term in the Lagrangian and show that the effective mass is proportional to the breaking vector and moderately dependent on the direction of observation. The breaking vector absolute value is estimated by ground measurements and leads to a photon mass upper limit of 10^{-19} eV or 2 x 10^{-55} kg and thereby to a potentially measurable delay at low radio frequencies.

  • [ACL 68] Bentum M., Bonetti L, SPALLICCI A.D.A.M., 2017. Dispersion by pulsars, magnetars and massive electromagnetism at very low radio frequencies, Adv. Space Res, 59, 736. arXiv:1607.08820 [astro-ph.IM]
    Our understanding of the universe relies mostly on electromagnetism. As photons are the messengers, fundamental physics is concerned in testing their properties. Photon mass upper limits have been earlier set through pulsar observations, but new investigations are offered by the excess of dispersion measure (DM) sometimes observed with pulsar and magnetar data at low frequencies, or with the fast radio bursts (FRBs), of yet unknown origin. Arguments for the excess of DM do not reach a consensus, but are not mutually exclusive. Thus, we remind that for massive electromagnetism, dispersion goes as the inverse of the frequency squared. Thereby, new avenues are offered also by the recently operating ground observatories in 10-80 MHz domain and by the proposed Orbiting Low Frequency Antennas for Radio astronomy (OLFAR). The latter acts as a large aperture dish by employing a swarm of nano-satellites observing the sky for the first time in the 0.1 - 15 MHz spectrum. The swarm must be deployed sufficiently away from the ionosphere to avoid distortions especially during the solar maxima, terrestrial interference and offer stable conditions for calibration during observations.

  • [ACL 69] Bonetti L., Ellis J., Mavromatos N.E., Sakharov A.S., Sarkisyan-Grinbaum E.K.G., SPALLICCI A.D.A.M., 2017. FRB 121102 casts new light on the photon mass, Phys. Lett. B, 768, 326. arXiv:1701.03097 [astro-ph.HE]
    The photon mass, m_gamma, can in principle be constrained using measurements of the dispersion measures (DMs) of fast radio bursts (FRBs), once the FRB redshifts are known. The DM of the repeating FRB 121102 is known to <1 %, a host galaxy has now been identified with high confidence,and its redshift, z , has now been determined with high accuracy: z=0.19273(8). Taking into account the plasma contributions to the DM from the Intergalactic medium (IGM) and the Milky Way, we use the data on FRB 121102 to derive the constraint m_gamma < 2.2×10^{-14} eV c^{-2} (3.9 × 10^{-50} kg). Since the plasma and photon mass contributions to DMs have different redshift dependences, they could in principle be distinguished by measurements of more FRB redshifts, enabling the sensitivity to m_gamma to be improved.

  • [ACL 70] Oltean M., Sopuerta C.F., SPALLICCI A.D.A.M., 2017. A frequency-domain implementation of the particle-without-particle approach to EMRIs, J. Phys. Conf. Ser., 840, 012056. arXiv:1703.00865 [gr-qc]
    The gravitational waves emitted by binary systems with extreme mass ratios carry unique astrophysical information expected to be probed by the next generation of gravitational wave detectors such as LISA. The detection of these binaries rely on an accurate modeling of the gravitational self-force that drives their orbital evolution. Although the theoretical formalism to compute the self-force has been largely established, the mathematical tools needed to implement it are still under development, and the self-force computation remains an open problem. We present here a frequency-domain implementation of the particle-without-particle (PwP) technique previously developed for the computation of the scalar self-force a helpful testbed for the gravitational self-force.

  • [ACL 71] Capozziello S., Prokopec T., SPALLICCI A.D.A.M., 2017. Aims and Scopes of the Special Issue: Foundations of Astrophysics and Cosmology, Found. Phys., 47, 709.

  • [ACL 72] SPALLICCI A.D.A.M., 2017. Comment on “Acceleration of particles to high energy via gravitational repulsion in the Schwarzschild field” [Astropart. Phys. 86 (2017) 18–20], Astropart. Phys., 94, 42. arXiv:1708.00799 [gr-qc]
    uComments are due on a recent paper by McGruder III (2017) in which the author deals with the concept of gravitational repulsion in the context of the Schwarzschild–Droste solution. Repulsion (deceleration) for ingoing particles into a black hole is a concept proposed several times starting from Droste himself in 1916. It is a coordinate effect appearing to an observer at a remote distance from the black hole and when coordinate time is employed. Repulsion has no bearing and relation to the local physics of the black hole, and moreover it cannot be held responsible for accelerating outgoing particles. Thereby, the energy boost of cosmic rays cannot be produced by repulsion.

  • [ACL 73] Bonetti L., dos Santos L.R., Helayël-Neto A.J., SPALLICCI A.D.A.M., 2018. Photon sector analysis of Super and Lorentz symmetry breaking: effective photon mass, tri-refringence and dissipation, Eur. Phys. J. C, 78, 811. arXiv.org/abs/1709.04995 [hep-th]
    Within the standard model extension (SME), we expand our previous findings on four classes of violations of Super-Symmetry (SuSy) and Lorentz Symmetry (LoSy), differing in the handedness of the Charge conjugation-Parity-Time reversal (CPT) symmetry and in whether considering the impact of photinos on photon propagation. The violations, occurring at the early universe high energies, show visible traces at present in the Dispersion Relations (DRs). For the CPT-odd classes (Vµ breaking vector) associated with the Carroll–Field–Jackiw (CFJ) model, the DRs and the Lagrangian show for the photon an effective mass, gauge invariant, proportional to |V|. The group velocity exhibits a classic dependency on the inverse of the frequency squared. For the CPT-even classes (kF breaking tensor), when the photino is considered, the DRs display also a massive behaviour inversely proportional to a coefficient in the Lagrangian and to a term linearly dependent on kF. All DRs display an angular dependence and lack LoSy invariance. In describing our results, we also point out the following properties: (i) the appearance of complex or simply imaginary frequencies and super-luminal speeds and (ii) the emergence of bi-refringence. Finally, we point out the circumstances for which SuSy and LoSy breakings, possibly in presence of an external field, lead to the non-conservation of the photon energy-momentum tensor. We do so for both CPT sectors.

  • [ACL 74] Oltean M., Sopuerta C.F., SPALLICCI A.D.A.M., 2019. Particle-without-Particle: a practical pseudospectral collocation method for numerical differential equations with distributional sources, J. Scient. Comp., 79, 827. arXiv:1802.03405 [physics.comp-ph]
    Partial differential equations with distributional sources—in particular, involving (derivatives of) delta distributions—have become increasingly ubiquitous in numerous areas of physics and applied mathematics. It is often of considerable interest to obtain numerical solutions for such equations, but any singular (“particle”-like) source modeling invariably introduces nontrivial computational obstacles. A common method to circumvent these is through some form of delta function approximation procedure on the computational grid; however, this often carries significant limitations on the efficiency of the numerical convergence rates, or sometimes even the resolvability of the problem at all. In this paper, we present an alternative technique for tackling such equations which avoids the singular behavior entirely: the “Particle-without-Particle” method. Previously introduced in the context of the self-force problem in gravitational physics, the idea is to discretize the computational domain into two (or more) disjoint pseudospectral (Chebyshev–Lobatto) grids such that the “particle” is always at the interface between them; thus, one only needs to solve homogeneous equations in each domain, with the source effectively replaced by jump (boundary) conditions thereon. We prove here that this method yields solutions to any linear PDE the source of which is any linear combination of delta distributions and derivatives thereof supported on a one-dimensional subspace of the problem domain. We then implement it to numerically solve a variety of relevant PDEs: hyperbolic (with applications to neuroscience and acoustics), parabolic (with applications to finance), and elliptic. We generically obtain improved convergence rates relative to typical past implementations relying on delta function approximations.

  • [ACL 75] Helayël-Neto J.A., SPALLICCI A.D.A.M., 2019. Frequency variation for in vacuo photon propagation in the Standard- Model Extension, Eur. Phys. J. C., 79, 590. arXiv: 1904.11035 [hep-ph]
    In the presence of Lorentz Symmetry Violation (LSV) associated with the Standard-Model Extension (SME), we have recently shown the non-conservation of the energy-momentum tensor of a light-wave crossing an Electro-Magnetic (EM) background field even when the latter and the LSV are constant. Incidentally, for a space-time dependent LSV, the presence of an EM field is not necessary. Herein, we infer that in a particle description, the energy non-conservation for a photon implies violation of frequency invariance in vacuo, giving rise to a red or blue shift. We discuss the potential consequences on cosmology.

  • [ACL 76] Oltean M., Epp R.J., Sopuerta C.F., SPALLICCI A.D.A.M., Mann R.B., 2020. The motion of localized sources in general relativity: gravitational self-force from quasilocal conservation laws, Phys. Rev. D., 101, 064060. arXiv: 1907.03012 [gr-qc]
    An idealized ''test'' object in general relativity moves along a geodesic. However, if the object has a finite mass, this will create additional curvature in the spacetime, causing it to deviate from geodesic motion. If the mass is nonetheless sufficiently small, such an effect is usually treated perturbatively and is known as the gravitational self-force due to the object. This issue is still an open problem in gravitational physics today, motivated not only by basic foundational interest, but also by the need for its direct application in gravitational wave astronomy. In particular, the observation of extreme-mass-ratio inspirals by the future space-based detector LISA will rely crucially on an accurate modeling of the self-force driving the orbital evolution and gravitational wave emission of such systems. In this paper, we present a novel derivation, based on conservation laws, of the basic equations of motion for this problem. They are formulated with the use of a quasilocal (rather than matter) stress-energy-momentum tensor—in particular, the Brown-York tensor—so as to capture gravitational effects in the momentum flux of the object, including the self-force. Our formulation and resulting equations of motion are independent of the choice of the perturbative gauge. We show that, in addition to the usual gravitational self-force term, they also lead to an additional ''self-pressure'' force not found in previous analyses, and also that our results correctly recover known formulas under appropriate conditions. Our approach thus offers a fresh geometrical picture from which to understand the self-force fundamentally, and potentially useful new avenues for computing it practically.

  • [ACL 77] Capozziello S., Benetti M., SPALLICCI A.D.A.M., 2020. Addressing the cosmological H0 tension by the Heisenberg uncertainty, Found. Phys., 50, 893. arXiv:2007.00462 [gr-qc]
    The uncertainty on measurements, given by the Heisenberg principle, is a quantum concept usually not taken into account in General Relativity. From a cosmological point of view, several authors wonder how such a principle can be reconciled with the Big Bang singularity, but, generally, not whether it may affect the reliability of cosmological measurements. In this letter, we express the Compton mass as a function of the cosmological redshift. The cosmological application of the indetermination principle unveils the differences of the Hubble-Lemaître constant value, H0, as measured from the Cepheids estimates and from the Cosmic Microwave Background radiation constraints. In conclusion, the H0 tension could be nothing else but the effect of indetermination derived in comparing a kinematic with a dynamic measurement.

  • [ACL 78] Barausse E. et al., 2020. Prospects for fundamental physics with LISA, Gen. Rel. Grav., 52, 81. arXiv:2001.09793 [gr-qc]
    We provide an updated assessment of the fundamental physics potential of LISA. Given the very broad range of topics that might be relevant to LISA, we present here a sample of what we view as particularly promising directions, based in part on the current research interests of the LISA scientific community in the area of fundamental physics. We organize these directions through a “science first” approach that allows us to classify how LISA data can inform theoretical physics in a variety of areas. For each of these theoretical physics classes, we identify the sources that are currently expected to provide the principal contribution to our knowledge, and the areas that need further development. The classification presented here should not be thought of as cast in stone, but rather as a fluid framework that is amenable to change with the flow of new insights in theoretical physics.

  • [ACL 79] SPALLICCI A.D.A.M., Helayël-Neto J.A., López-Corredoira M., Capozziello S., 2021. Cosmology and the massive photon frequency shift induced by the Standard-Model Extension, Eur. Phys. J. C., 81, 4. arXiv:2011.12608 [astro-ph.CO]
    The total red-shift z might be recast as a combination of the expansion red-shift and of a static shift due to the energy-momentum tensor non-conservation of a photon propagating through Electro-Magnetic (EM) fields. If massive the photon may be described by the de Broglie-Proca (dBP) theory which satisfies the Lorentz(-Poincaré) Symmetry (LoSy) but not gauge-invariance. The latter is regained in the Standard-Model Extension (SME), associated to LoSy Violation (LSV), that naturally dresses photons of a mass. The non-conservation stems from the vacuum expectation value of the vector and tensor LSV fields. The final colour (red or blue) and size of the static shift depend on the orientations and strength of the LSV and EM multiple fields encountered along the path by the photon. Turning to cosmology, for a zero ΩΛ energy density, the discrepancy between luminosity and red-shift distances of SNeIa disappears thanks to the recasting of z. Massive photons induce an effective dark energy acting 'optically' but not dynamically.

  • [ACL 80] Sesana A., Korsakova N., Arca Sedda M., Baibhav V., Barausse E., Barke S., Berti E., Bonetti M., Capelo P.R., Caprini C., Garcia-Bellido J., Haiman Z., Jani K., Jennrich O., Johansson P., Khan F.M., Korol V., Lamberts A., Lupi A., Mangiagli A., Mayer L., Nardini G., Pacucci F., Petiteau A., Raccanelli A., Rajendran S., Regan J., Shao L., SPALLICCI A., Tamanini N., Volonteri M., Warburton N., Wong K., Zumalacarregui M., 2019. Unveiling the gravitational universe at µ-Hz frequencies, Exp. Astron. arXiv: 1908.11391 [astro-ph.IM]
    We propose a space-based interferometer surveying the gravitational wave (GW) sky in the milli-Hz to µ-Hz frequency range. By the 2040s', the µ-Hz frequency band, bracketed in between the Laser Interferometer Space Antenna (LISA) and pulsar timing arrays, will constitute the largest gap in the coverage of the astrophysically relevant GW spectrum. Yet many outstanding questions related to astrophysics and cosmology are best answered by GW observations in this band. We show that a µ-Hz GW detector will be a truly overarching observatory for the scientific community at large, greatly extending the potential of LISA. Conceived to detect massive black hole binaries from their early inspiral with high signal-to-noise ratio, and low-frequency stellar binaries in the Galaxy, this instrument will be a cornerstone for multimessenger astronomy from the solar neighbourhood to the high-redshift Universe.

  • [ACL 81] SPALLICCI A.D.A.M., Benetti M., Capozziello S., 2022. Heisenberg limit at cosmological scales, Found. Phys., 52, 23. arXiv: 2112.07359 [physics.gen-ph]
    For an observation time equal to the universe age, the Heisenberg principle fixes the value of the smallest measurable mass at mH = 1.35 x 10-69 kg and prevents to probe the masslessness for any particle using a balance. The corresponding reduced Compton length to mH is ƛH, and represents the length limit beyond which masslessness cannot be proved using a metre ruler. In turns, ƛH is equated to the luminosity distance dH which corresponds to a red shift zH. When using the Concordance-Model parameters, we get dH = 8.4 Gpc and zH = 1.3. Remarkably, dH$ falls quite short to the radius of the observable universe. According to this result, tensions in cosmological parameters could be nothing else but due to comparing data inside and beyond zH. Finally, in terms of quantum quantities, the expansion constant H0 reveals to be one order of magnitude above the smallest measurable energy, divided by the Planck constant.

  • [ACL 82] SPALLICCI A.D.A.M., Sarracino G., Capozziello S., 2022. Investigating dark energy by electromagnetism frequency shifts (Special Issue on: Tensions in cosmology from early to late universe: the value of the Hubble constant and the question of dark energy), Eur. Phys. J. Plus, 137, 253. arXiv: 2202.02731[astro-ph.CO]
    The observed red shift z might be composed by the expansion red shift zC and an additional frequency shift zS, towards the red or the blue, by considering extended theories of electromagnetism (ETE). Indeed, massive photon theories—the photon has a real mass as in the de Broglie–Proca theory or an effective mass as in the standard-model extension, based on Lorentz–Poincaré symmetry violation (LSV)—or nonlinear electromagnetism theories may induce a cosmological expansion-independent frequency shift in the presence of background (inter-) galactic electromagnetic fields, and where of relevance LSV fields, even when both fields are constant. We have tested this prediction considering the Pantheon Catalogue, composed by 1048 SNe Ia, and 15 BAO data, for different cosmological models characterised by the absence of a cosmological constant. From the data, we compute which values of zS match the observations, spanning cosmological parameters (densities and Hubble–Lemaître constant) domains. We conclude that the frequency shift zS can support an alternative to accelerated expansion, naturally accommodating each SN Ia position in the distance modulus versus red shift diagram, due to the light-path dependency of zS. Finally, we briefly mention laboratory test approaches to investigate the additional shift from ETE predictions.

  • [ACL 83] Arun K.G. et al, 2022. New horizons for fundamental physics with LISA, Liv. Rev. Rel., 25, 4. arXiv:2205.01597 [gr-qc]
    The Laser Interferometer Space Antenna (LISA) has the potential to reveal wonders about the fundamental theory of nature at play in the extreme gravity regime, where the gravitational interaction is both strong and dynamical. In this white paper, the Fundamental Physics Working Group of the LISA Consortium summarizes the current topics in fundamental physics where LISA observations of gravitational waves can be expected to provide key input. We provide the briefest of reviews to then delineate avenues for future research directions and to discuss connections between this working group, other working groups and the consortium work package teams. These connections must be developed for LISA to live up to its science potential in these areas.

  • [ACL 84] Sarracino G., SPALLICCI A.D.A.M., Capozziello S., 2022. Investigating dark energy by electromagnetism frequency shifts (Special Issue on: Tensions in cosmology from early to late universe: the value of the Hubble constant and the question of dark energy), Eur. Phys. J. Plus, 137, 1386. arXiv:2211.11438 [astro-ph.CO]
    Following results presented in Spallicci et al. (Eur Phys J Plus 137, 2022) by the same authors, we investigate the observed red shift z, working under the hypothesis that it might be composed by the expansion red shift zC and an additional frequency shift zS, towards the red or the blue, due to Extended Theories of Electromagnetism (ETE).We have tested this prediction considering the novel Pantheon+ Catalogue, composed by 1701 light curves collected by 1550 SNe Ia, and 16 BAO data, for different cosmological models characterised by the absence of a dark energy component. In particular, we shall derive which values of zS match the observations, comparing the new results with the ones obtained considering the older Pantheon Catalogue. We find interesting differences in the resulting zS distributions, highlighted in the text. Later, we also add a discussion regarding Extended Theories of Gravity and how to incorporate them in our methodology.

  • [ACL 85] Capozziello S., Sarracino G., SPALLICCI A.D.A.M., 2023. Questioning the H0 tension via the look-back time, Phys. Dark Univ., 40, 101201. arXiv:2302.13671 [astro-ph.CO]
    e Hubble tension is investigated taking into account the cosmological look-back time. Specifically, considering a single equation, widely used in standard cosmology, it is possible to recover both values of the Hubble constant H0 reported by the SH0ES and Planck collaborations: the former is obtained through cosmological ladder methods (e.g. Cepheids, Supernovae Type IA) and the latter through measurements of the Cosmic Microwave Background. Also, other values obtained in the literature are achieved with the same approach. We conclude that the Hubble tension can be removed if the look-back time is correctly referred to the redshift where the measurement is performed.

  • [ACL 86] Amaro-Seoane P. et al., 2023. Astrophysics with the Laser Interferometer Space Antenna, to appear in Liv. Rev. Rel. arXiv:2203.06016 [gr-qc]


  • [ACL 87] SPALLICCI A.D.A.M., Sarracino G., Randriamboarison O., Helayël-Neto J.A., 2023. Testing the Ampère-Maxwell law on the photon mass and Lorentz-Poincaré symmetry violation with MMS multi-spacecraft data. arXiv:2205.02487 [hep-ph]
    The photon, main messenger for interpreting the universe, is the only free massless particle in the Standard-Model (SM). Deviations from the Ampère-Maxwell law, due to a photon mass for the de Broglie-Proca theory or the Lorentz-Poincaré Symmetry Violation (LSV) in the SM Extension (SME), were sought in six years of data of the Magnetospheric Multi-Scale (MMS) mission, a four-satellite constellation, crossing mostly turbulent regions of magnetic reconnection and collecting about 95% of the data outside the quieter solar wind. We examined 3.8 million data points from the solar wind, magnetosheath, and magnetosphere regions. Beyond the upper limits on which we duly report, in a minority of cases, for the highest time resolution burst data and best tetrahedron configurations (2.2% in modulus and 4.8% in Cartesian components for all regions, but 21% in modulus and 29.9% in Cartesian components in the solar wind), deviations have been found. The deviations might be due to unaccounted experimental errors or to non-Maxwellian terms. Possibly, we are at the boundaries of measurability for non-dedicated missions. We discuss our experimental results versus more stringent but model-dependent limits.

    • THE ORLEANS TEAM

    • Alessandro D.A.M. Spallicci, Orélien Randriamboarison (plasma physics), Abedennour Dib (Doctorate student), Tom Cooper (Master student) plus students (see below)
    • Past permanent members: S. Cordier (MAPMO), R. Emilion (MAPMO), D. Fall (MAPMO), S. Jubertie (LIFO).
    • Visitors: B. Whiting (Univ. Florida) 2008, 2012, M. van Putten (MIT-LIGO) Chaire Le STUDIUM 2008-2009, S. Aoudia (Max Planck Inst. Golm, Univ. Bejaya) 2011, 2012, 2016, 2018, L. Burko (Univ. Huntsville) 2012, C. Sopuerta (IEEC Barcelona) 2013, S. Perez-Bergliaffa (UERJ Rio de Janeiro) 2014, 2015, M. Benetti (Univ. Napoli 1) 2019, S. Capozziello (Univ. Napoli I) 2019, R. Cimino (Univ. Napoli I) 2019.

    TEACHING

    My teaching service amounts to 150 hours per year, mostly lectures, and to a lesser extent exercise classes; this is counted as 192 hours equivalent per year in the French system, the recognised national standard).
    Responsible of the following courses at the Université d'Orléans

    Occasional external lecturers from LPC2E, MAPMO, ESA, CNES, APC Paris, ENS Paris, IAP Paris, LPP Paris, OCA-Sophia Antipolis



    Master en Physique Fondamentale et Applications
  • Space Exploration and Space Systems - Master 2 (previously: Exploration du milieu spatial et systèmes spatiaux - Master 1 SAE)
    •
  • Relativité Générale - Master 1 (previously: Introduction à la gravitation et à l'astrophysique relativiste - Master 1 SAE)

    • Licence de Physique
  • Relativité et Physique Subatomique - L3

    • Dismissed courses
  • Expériences Spatiales en Physique Fondamentale - Master 2 SAE

  • Physique des (Astro-)Particules - Ouverture Licence L1, L2, L3, pour tous les parcours

  • Relativité, Sciences spatiales, Astrophysique - Ouverture Licence L1, L2, L3 pour tous les parcours
    •

    =

    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

    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.

    1984-1986 Honeywell, Caluso
    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

    Visits and Seminars
    - Dip. Matematica, Univ. Pisa, 1988-1990 (in fragments).
    - Univ. Groningen Univ., 24 Februay 1989.
    - Center of Relativity, Univ. of Texas at Austin, 30 April - 4 May 1990.
    - Istituto di Fisica dello Spazio Interplanetario, Frascati, 10 July 1990.
    - ESTEC Space Science Dept., Noordwijk, 7 December 1990.
    - Istituto Nazionale di Fisica Nucleare, Pisa, 14 December 1990.
    - Gravitation Research Group, Univ. Salerno, April 1992.
    - Physics and Astr. Dept., Univ. of Wales at Cardiff, 6-10 December 1993.
    - Ist. di Fisica Matematica, J.-L. Lagrange, Univ. Torino, 1993-1994 (in fragments).
    - Gravitation Research Group, Univ. Salerno, 9-14 January 1995.
    - Physics and Astr. Dept., Univ. of Wales at Cardiff, 20-22 March 1995.
    - Univ. Chicago, Enrico Fermi Inst., 29 May - 2 June 1995 (by S. Chandrasekhar).
    - Physics Dept. Univ. of Utah at Salt Lake City, 26-30 October 1995.
    - Gravitation Research Group, Univ. Salerno, 6-21 May 1996.
    - A. Einstein Max Planck Institut für Gravitationsphysik Potsdam, 10-13 June 1996.
    - Gravitation Research Group, Univ. Salerno, 16-26 September 1996.
    - Imperial College, London Univ., 14 October 1996.
    - Gravitation Research Group, Univ. Salerno, 5-14 February 1997.
    - Osservatorio Monte Mario, Roma, 10 March 1997.
    - Scuola Ingegneria Aerospaziale, Roma, 12 March 1997.
    - Obs. Neuchâtel, March 1997.
    - SRON Space Research Organization Nederland, Utrecht, 27 March 1997.
    - Dip. Matematica R. Caccioppoli, Univ. Napoli Federico II, 6 June 1997.
    - Univ. Bologna, 15 July 1997.
    - Nationaal Instituut voor Kernfysica en Hoge-Energie Fysica, Stichting voor Fundamenteel Onderzoek der Materie, Amsterdam, 1998-1999 (in fragments).
    - Dipartimento di Matematica G. Castelnuovo Univ. di Roma 1 La Sapienza, 1999-2002 (in fragments).
    - Int. Centre of Relativistic Astrophysics, ICRA, Dip. Fisica, Univ. Roma La Sapienza, 2000.
    - UTINAM, Obs. Besançon, 18 April 2002.
    - LPTA Montpellier, 24 April 2002.
    - Inst. Ciencias del Espacio y Inst. d'Estudis Espacials de Catalunya, Barcelona, 30 November 2005.
    - LAL Orsay, 10 April 2006.
    - APC Paris, 11 April 2006.
    - LPCE Orléans, 13 April 2006.
    - LAPTH Annecy, 14 April 2006.
    - Facoltà di Scienze Mat. Fis. Nat., Univ. del Piemonte Orientale, Alessandria, 14 June 2006.
    - Univ. Chicago, E. Fermi Inst., 19 May – 27 May 2009.
    - Univ. Southampton, 17-21 August 2009.
    - A. Einstein Max Planck Institut für Gravitationsphysik Golm, 7 - 14 April 2010.
    - UERJ Universidade do Estado de Rio de Janeiro and CBPF Centro Brasileiro des Pequiscas Físicas, Rio de Janeiro, 11-18 November 2012.
    - UERJ Universidade do Estado de Rio de Janeiro and CBPF Centro Brasileiro des Pequiscas Físicas, Rio de Janeiro, 29 October - 23 November 2014.
    - IPN Instituto Politécnico Nacional and CINVESTAV (Tesis doctoral A. Avalos Vargas, Prof. G. Ares de Parga), Cidad de Mexico, 15-19 December 2014.
    - Dipartimento di Fisica, Università di Napoli Federico II, 9-13 February 2015.
    - UERJ Universidade do Estado de Rio de Janeiro and CBPF Centro Brasileiro des Pequiscas Físicas, Rio de Janeiro, 20 April-29 May 2015.
    - UERJ Universidade do Estado de Rio de Janeiro and CBPF Centro Brasileiro des Pequiscas Físicas, Rio de Janeiro, 6-28 September 2015.
    - CBPF Centro Brasileiro des Pequiscas Físicas, Rio de Janeiro, 16 April-26 May 2016.
    - Dipartimento di Fisica, Università di Napoli Federico II, 17-24 February 2017.
    - Universität Bremen, 3 March 2017.
    - CBPF Centro Brasileiro des Pequiscas Físicas, Rio de Janeiro, 9-19 March 2017.
    - CBPF Centro Brasileiro des Pequiscas Físicas, Rio de Janeiro, 1-23 June 2017.
    - CBPF Centro Brasileiro des Pequiscas Físicas, Rio de Janeiro, 29 August – 19 September 2017.
    - CBPF Centro Brasileiro des Pequiscas Físicas, Rio de Janeiro, 29 October - 25 November 2017.
    - CBPF Centro Brasileiro des Pequiscas Físicas, Rio de Janeiro, 9 January - 22 January 2018.
    - LPNHE Laboratoire de Physique Nucléaire et de Hautes Énergies, 29 January 2018.
    - CBPF Centro Brasileiro des Pesquisas Físicas, Rio de Janeiro, 3-19 March 2018.
    - Dipartimento di Fisica, Università di Napoli Federico II, 27 May – 1 June 2018 .
    - CBPF Centro Brasileiro des Pesquisas Físicas, Rio de Janeiro, 13 July -11 August 2018.
    - IAC, Instituto de Astrofísica de Canarias, La Laguna, 27 August – 8 September 2018.
    - CBPF Centro Brasileiro des Pesquisas Físicas, Rio de Janeiro, 28 October-17 November 2018.
    - CBPF Centro Brasileiro des Pesquisas Físicas, Rio de Janeiro, 9-22 January 2019.
    - CBPF Centro Brasileiro des Pesquisas Físicas, Rio de Janeiro, 3-21 April 2019.
    - Dipartimento di Fisica, Università di Napoli Federico II, 20 – 28 May 2019.
    - UERJ Universidade do Estado de Rio de Janeiro and CBPF Centro Brasileiro des Pequiscas Físicas, Rio de Janeiro, 18 August-28 September 2019.
    - UERJ Universidade do Estado de Rio de Janeiro and CBPF Centro Brasileiro des Pequiscas Físicas, Rio de Janeiro, 28 November-23 December 2019.
    - UERJ Universidade do Estado de Rio de Janeiro and CBPF Centro Brasileiro des Pequiscas Físicas, Rio de Janeiro, 8 January-31 January 2020.
    - Institut d’Astrophysique de Paris, 24 September 2020.
    - CBPF Centro Brasileiro des Pesquisas Físicas, Rio de Janeiro, 29 Aout – 14 September 2021.
    - IDP, Institut Denis Poisson, Tours 7 February 2022.
    - Kungliga Tekniska Högskolan (KTH), Stockholm 28 September 2022.

    Conferences and Schools
    - Vulcan Science Meeting, 8 September 1986 Noordwijk.
    - Vulcan Science Meeting, 24 October 1986 Noordwijk.
    - Optical Systems for Space Applications, 30 March - 1 April 1987 Den Haag.
    - Vulcan Science Meeting, 3-4 May 1988 Noordwijk.
    - 8th It. Conf. on General Relativity and Gravitational Physics, 30 August-3 September 1988 Cavalese, Trento.
    - 12th Internat. Conf. on General Relativity and Gravitation, 3-8 July 1989 Boulder.
    - Gravitational waves data analysis workshop, 2-5 December 1989 Roma.
    - VIRGO Mtg. on software issues, 7-8 January 1991 Annecy.
    - 25th Rencontre de Moriond, New and exotic phenomena, 20-27 January 1990 Les Arcs.
    - Radio Science Mtg. of URSI, 7-11 May 1990 Dallas.
    - 1st Fairbank Mtg. on Relativistic Gravitational Experiments in Space, 10-14 September 1990 Roma.
    - 9th It. Conf. on General Relativity and Gravitational Physics, 25-28 September 1990 Capri.
    - 6th European Frequency and Time forum, 17-19 March 1992 Noordwijk.
    - Data Analysis for Interferometric Gravitational Wave Detectors, 29-30 April 1992 Cardiff.
    - Journées Relativistes, 14-16 May 1992 Amsterdam.
    - 13th Int. Conf. on Gen. Rel. and Gravitation, 28 June - 4 July 1992 Huerta Grande, Cordoba.
    - 10th It. Conf. on General Relativity and Gravitational Physics, 1-5 September 1992 Bardonecchia.
    - ESA Gravitational Wave Detection Workshop, 6-7 October 1992 Paris.
    - STEP symposium, 6-8 April 1993 Pisa.
    - Detection of Gravitational Radiation Workshop, 24 May 1994 Amsterdam.
    - 11th It. Conf. on General Relativity and Gravitational Physics, 26-30 September 1994 Trieste.
    - GRAIL workshop, 27-29 March 1995 Twente University.
    - 3rd Ann.Penn State Conf., Astrophysical sources of gravitational radiation, 7-10 July 1995 Penn State Univ.
    - 14th Internat. Conf. on General Relativity and Gravitation, 6-12 August 1995 Firenze.
    - Symposium on Fundamental Physics in Space, 16-19 October 1995 London.
    - 12th It. Conf. on General Relativity and Gravitational Physics, 23-27 September 1996 Roma.
    - 1st Symp. on the Utilization of the International Space Station, 30 September - 2 October 1996 Darmstadt.
    - TAMA Workshop on Gravitational Waves Detection, 12-14 November 1996 Saitama.
    - 11th European Frequency and Time forum, 7 March 1997 Neuchâtel.
    - Problemi Attuali di Fisica Teorica, Onde Gravitazionali, 21 March 1997 Vietri sul Mare, Salerno.
    - 8th Marcel Grossmann Mtg., 22-28 June 1997 Jerusalem.
    - 2nd Amaldi Conf. on Gravitational Waves, 1-4 July 1997 Geneve.
    - 48th IAF Congress 6-10 October 1997 Torino.
    - 15th Internat. Conf. on General Relativity and Gravitation, 16-21 December 1997 Pune.
    - 13th Italian Conf. on General Rel. and Grav. Physics, 21-25 September 1998 Monopoli, Bari.
    - 3rd Capra Mtg. on radiation reaction, 5-9 June 2000 Pasadena.
    - 9th Marcel Grossmann Mtg., 2-8 July 2000 Roma.
    - 1st Int. Symp. Microgravity Res. & Appl. Physical Sciences Biotechnology, 10-15 September 2000 Sorrento.
    - Assemblea scientifica GNFM, 2-3 November 2000 Montecatini Terme, Pistoia.
    - 15th European Frequency and Time Forum, 6-8 March 2001 Neuchâtel.
    - 5th Amaldi Conf. on Gravitational Waves, 6-11 July 2003 Tirrenia, Pisa.
    - Conf. on Sources of gravitational waves, 22-26 September 2003 Trieste.
    - GREX Gravitation et Expériences Spatiales, 8-10 October 2003 Paris.
    - ASSNA Action Spécifique pour la simulation numérique en astrophysique, 15-18 December 2003 Paris.
    - GPS Meeting, 31 March 2004 Paris.
    - VIRGO Mtg., 3-5 May 2004 Pisa.
    - 7th Capra Mtg. on radiation reaction, 28 May-4 June 2004 Brownsville.
    - Galileo Mtg., 16 June 2004 Paris.
    - 38th ESLAB Symp., 5th Intern. LISA Symp., 12-15 July 2004 Noordwijk.
    - GREX Gravitation et Expérience, 27-29 October 2004 Nice.
    - VIRGO Mtg., 2-3 November 2004 Orsay.
    - VESF, Virgo Eur. Scientific Forum, 9-10 December 2004 Pisa.
    - GWDAW9 15-18 December 2004 Annecy.
    - 1e Journées LISA France, 20-21 January 2005 Paris.
    - 8th Capra Mtg. on radiation reaction, 11-14 July 2005 Oxford.
    - 2e Journées LISA France, 5-6 October 2005 Nice.
    - GREX Gravitation et Expériences Spatiales, 12-15 October 2005 Paris.
    - LISA Data Analysis Mtg., 31 October 2005 Noordwijk.
    - The 1st Bego scientific meeting, 6-15 February 2006 Nice.
    - 3e Journées LISA France, 15-16 May 2006 Meudon.
    - VESF, Virgo Eur. Scientific Forum, 23-24 April 2007 Pisa.
    - 2nd Workshop on Pulsars: theories et observations, 3-4 May 2007 Paris.
    - Journés Tourangelles Relativistes, 1 June 2007 Tours.
    - 10th Capra Mtg. on radiation reaction, 25-30 June 2007 Huntsville.
    - 18th Internat. Conf. on General Relativity and Gravitation, 8-14 July 2007 Sydney.
    - 7th Amaldi Conf. on Gravitational Waves, 8-14 July 2007 Sydney.
    - 1st Int. Scientific & Fundamental Aspects of the Galileo Progr., 1-4 October 2007 Toulouse.
    - 4e Journées LISA France, 13-14 March 2008 Paris.
    - Organisation of the Ecole Thématique CNRS sur la Masse et Conf. Internationale Capra in Orléans 23-29 June 2008 .
    - 3rd Workshop on Pulsars: theories et observations, 24-26 November 2008 Paris.
    - Journée GREX sur l’exploration de la gravitation à l’echelle du système solaire, 2 December 2008 Meudon.
    - 5e Journées LISA France, 26-27 February 2009 Paris.
    - 12th Capra Mtg. on radiation reaction, 15-19 June 2009 Bloomington.
    - 21st Rencontre de Blois: Windows on the Universe, 22-26 June 2009 Blois.
    - 12th Marcel Grossmann Mtg., 12-18 July 2009 Paris.
    - 4th LISA Astro-GR@BCN, 7-11 September 2009 Barcelona.
    - Séminaire de prospective – GDR PCHE, 28-29 September 2009 Paris.
    - 2nd Int. Scientific & Fundamental Aspects of the Galileo Progr., COSPAR Coll., 14-16 October 2009 Padova.
    - Gravitation and Fundamental Physics in Space, GPhyS "Kick-Off " Coll., 20-22 October 2009 Les Houches.
    - 6e Journées LISA France, 9-10 November 2009 Nice.
    - 7e Journées LISA France, 1-2 June 2010 Chatillon.
    - Fundamental Physics Laws: Gravity, Lorentz Symmetry and Quantum Gravity, 2-3 June 2010 Paris.
    - 13th Capra Mtg. on radiation reaction (Theory Meets Data Analysis at Comparable and Extreme Mass Ratios), 20-26 June 2010 Waterloo, Toronto.
    - 11th Frontiers of Fundamental Physics, 6-9 July 2010 Paris.
    - LISA Astro-GR@Paris, 13-17 September 2010 Paris.
    - Call for a medium size mission for a lunch in 2022 Briefing Meeting ESTEC, 1 October 2010 Noordwijk.
    - Int. Fall Workshop on Geometry and Physics, 29 October 2010 Paris.
    - Variation of fundamental constants, IAP, 8 November 2010 Paris.
    - Séminaire par G. ‘t Hooft, Univ. Pierre et Marie Curie, 8 November 2010 Paris.
    - J. Action Specifique GRAM (Gravitation, Références, Astronomie, Metrologie), 29-30 November 2010 Nice.
    - 8e Journées LISA France, APC, 9-10 May 2011 Paris.
    - Cosmological frontiers in Fundamental Physics, APC, 14-17 June 2011 Paris.
    - 14th Capra Mtg. on radiation reaction, 4-8 July 2011 Southampton.
    - 12th Frontiers of Fundamental Physics, 21-23 November 2011 Udine.
    - 9th LISA Symposium, 21-25 May 2012 Paris.
    - 15th Capra Mtg. on radiation reaction, 11-15 June 2012 Maryland College Park.
    - 16th Capra Mtg. on radiation reaction, 15-22 July 2013 Dublin.
    - 99th Congr. Naz. Soc. It. Fis., 23-27 September 2013 Trieste.
    - Journées LISA France, APC, 7-8 April 2014 Paris.
    - Hot topics in Modern Cosmology Spontaneous Workshop VIII, 12-17 May 2014 Carghjese.
    - X LISA symposium, 18-23 May 2014 Gainesville.
    - 9th IARD Conference, 9-13 June 2014 Storrs.
    - 17th Capra Mtg. on radiation reaction, 23-27 June 2014 Pasadena.
    - 14th Frontiers of Fundamental Physics, 15-18 July 2014 Marseille.
    - 21th It. Conf. on General Relativity and Gravitational Physics, 15-19 September 2014 Alessandria.
    - Escola Brasileira de Cosmologia e Gravitação, Vargas Grande, 31 October 2014.
    - Fundação Planetário da Cidade do Rio de Janeiro, 19 November 2014, Seminar for the 44th anniversary.
    - 14th Marcel Grossmann Mtg., 12-18 July 2015 Roma.
    - Journées Scientifiques GRAM, 2-3 June 2016 Paris.
    - Estate Quantistica, 13-17 June 2016 Scalea.
    - 19th Capra Meeting on Radiation Reaction in General Relativity, 27 June – 1 July 2016 Meudon.
    - Cosmology on small scales, 20-23 September 2016 Praha.
    - ACES Workshop Fundamental and applied science with clocks and cold atoms in space, 29-30 June 2017 Zurich.
    - Semaine de l’Astrophysique Française, 4-7 July 2017 Paris.
    - 2nd Workshop FQXI Project Quantum Rogue Waves as Emerging Quantum Events, 11-13 July 2017 Marseille.
    - Workhop on testing fundamental physics principles, 22-28 September 2017 Kérkyra.
    - Probing quantum spacetime with astrophysical sources: the CTA era and beyond, 29-30 November 2017 Paris.
    - 15th Marcel Grossmann Mtg., 30 June - 7 July 2018 Roma.
    - Cosmology on small scales, 25-29 September 2018 Praha.
    - Cosmic controversies, Kavli Inst., 5- 8 October 2019 Chicago.
    - Louis de Broglie: theory of the double solution and quantum trajectories, 4 November 2019 Inst. H. Poincaré Paris.
    - Atélier Théories de l’action Dark Energy, 19 November 2019 Paris.
    - 8th MMS Workshop, 13 May 2022 Daytona Beach.
    - Challenges to Lambda-CDMP Cosmology, 7 September 2022 Thessaloniki.
    - International Physics Education Conference, 8 December 2022 Sydney.

    PROJECTS

    • 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

    DOCTORATE STUDENTS - POST-DOCS

    • Vincenzo Pierro (Salerno-I), post-doc, now Professore Associato at the Università del Sannio, Benevento

    • Sofiane Aoudia (Béjaïa-DZ), Doctorate student (Thesis 2008), post-doc at the Max Planck Institut für Gravitationphysik A. Einstein, Golm, now Maître de Conférences at the Université de Béjaïa, MESR grant

    • Patxi Ritter (Romorantin Lanthenay-F), Doctorate student (Thesis 2013), post-doc in Praha, MESR grant

    • Luca Bonetti (Cles-I), Doctorate student (Thesis 2016), MESR grant

    • Marius Oltean (Waterloo-CA), Doctorate student (Thesis 2019) Codirection with C. F. Sopuerta (Barcelona), now lecturer in Barcelona, Eiffel and NRC grants

    • Wellisson Barbosa de Lima (BR), Doctorate student (Thesis 2023), Codirection with J.A. Helayël-Neto (Rio de Janeiro), FAPERJ grant

    • Giuseppe Sarracino (Napoli-I), Doctorate student (Thesis 2023), Codirection with S. Capozziello (Napoli)

    • Abedennour Dib (Oran-DZ), Doctorate student (Thesis started on 1 March 2023), ANR grant

    top page

    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.



    LEASURE AND SCIENCE LINKS

    La grande bellezza
    Tracery
    In trutina
    The Book human race should save
    An easy vivid way to explain gravitational waves
    Dio esiste? September 2000, Teatro Quirino Roma, a debate between P. Flores d'Arcais et J. Ratzinger on Fides et Ratio

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

    • Number of publications and citations for researcher.

    FUNNY STATEMENTS MEANT SERIOUSLY

    • Student: I don't need to understand. I am a chemistry student.

    • Editor Phys. Rev. Lett.: We cannot accept your letter correcting the work of xx, because even if the letter of xx contains a mistake, the letter was published more than 10 years ago.

    • Junior scientist : You do not need to know general relativity to do a thesis on gravitational waves.

    • Professor : (Discussing undergraduate courses, id est 'Special') Relativity has nothing to do with quantum mechanics.

    • Senior Scientist : I did all my career without having to do with the four interactions.

    • The same Senior Scientist : It is offensive to do a theoretical presentation to this laboratory.

    • And again improving : I know about black holes except general relativity.

    MY FULL NAME

    Alessandro Domenico Aloisio Maria Spallicci di Filottrano
    Nicknames: Mimino, Picitrè, Mimmo, Cicci, Ale, Alex, Sandro



    NOVELIST






    Some novels under the title 'Antologia del Fiume Oglio' have appeared in February 2015 by Arnoldo Mondadori Editore, in the 'Gialli' series as winner of the Suzzara prize for unpblished stories.





    WHERE I HANG MOST

    My list of best world cities: 1. Venezia, 2. Roma, 3. Amsterdam, 4. Rio de Janeiro, 5. Barcelona, 6. Praha, 7. London, 8. Fort Cochin, 9. Nice, 10. Paris.












    SOME RELATIVES

    Aldo Spallicci
    Mario Spallicci
    Emilio Spallicci with Sandro Pertini and Oscar Scalfaro [pdf]



    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. Public transport: once arrived at one of the train stations, Les Aubrais or Gare d'Orléans, get the tram and drop off at 'L'Indien' and ask the indigeneous about the CNRS campus; else at the Gare d'Orléans station, fetch the 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.




    WHO IS LOOKING AT MY WEBPAGE
    (CLUSTRMAPS often stuck and not working)

    Clustrmaps data 10 Jun 2012 to 16 Mar 2015 before crash server : 2,589 visits, click the pdf link

    Quotes

    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? (Rainer Maria Rilke)


    Quatuor sunt urbes cæteris præeminentes, Parisius in scientiis, Salernum in medicinis, Bononia in legibus, Aurelianis in actoribus (Tommaso d'Acquino XIII seculum )
    Four are the cities that are preminent over the others, Paris in sciences, Salerno in medicine, Bologna in law, Orléans in actuarial sciences


    top page