Publications

@article{auclair-desrotour_can_2023,

title = {Can one hear supercontinents in the tides of ocean planets?},

author = {P. Auclair-Desrotour and M. Farhat and G. Boué and M. Gastineau and J. Laskar},

url = {https://www.aanda.org/articles/aa/abs/forth/aa47301-23/aa47301-23.html},

doi = {10.1051/0004-6361/202347301},

issn = {0004-6361, 1432-0746},

year  = {2023},

date = {2023-10-01},

urldate = {2023-10-01},

journal = {Astronomy & Astrophysics},

abstract = {Astronomy & Astrophysics (A&A) is an international journal which publishes papers on all aspects of astronomy and astrophysics},

note = {Publisher: EDP Sciences},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{Sinnesael2023a,

title = {Ordovician cyclostratigraphy and astrochronology},

author = {Matthias Sinnesael},

url = {https://www.lyellcollection.org/doi/10.1144/SP532-2022-31},

doi = {10.1144/SP532-2022-31},

issn = {0305-8719, 2041-4927},

year  = {2023},

date = {2023-08-01},

urldate = {2023-08-01},

journal = {Geological Society, London, Special Publications},

volume = {532},

number = {1},

pages = {SP532--2022--31},

abstract = {Abstract 

 Cyclostratigraphy is an important tool for understanding astronomical climate forcing and reconstructing geological time in sedimentary sequences, provided that an imprint of insolation variations caused by Earth's orbital eccentricity, obliquity and precession is preserved (Milankovitch forcing). Understanding astronomical climate forcing has proven fundamental for the study of Cenozoic climate systems and the construction of high-resolution continuous time scales (astrochronologies). Pre-Cenozoic astrochronologies face several challenges:(1) uncertainties in the deep-time astronomical solutions and parameters; (2) less-complete and less-well-preserved strata; and (3) the sparsity of geochronologic anchor points. Consequently, Palaeozoic astrochronologies are typically based on identification of the stable 405-kyr eccentricity cycle instead of shorter astronomical cycles. Here, a state-of-the-art review of Ordovician cyclostratigraphy and astrochronology is presented, as well as suggestions on their robust application in an Ordovician context. Ordovician astronomically driven climate dynamics are suggested to have influenced processes like glacial dynamics, sea-level variations and changes in biodiversity. Ordovician cyclostratigraphic studies can help to construct high-resolution numerical time scales, ideally in combination with high-quality radio-isotopic dating. As such, cyclostratigraphy is becoming an increasingly important part of an integrated stratigraphic approach to help disentangle Ordovician stratigraphy and palaeoenviromental changes.},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{briaud_lunar_2023,

title = {The lunar solid inner core and the mantle overturn},

author = {Arthur Briaud and Clément Ganino and Agn`es Fienga and Anthony Mémin and Nicolas Rambaux},

url = {https://ui.adsabs.harvard.edu/abs/2023Natur.617..743B},

doi = {10.1038/s41586-023-05935-7},

issn = {0028-0836},

year  = {2023},

date = {2023-05-01},

urldate = {2023-05-01},

journal = {Nature},

volume = {617},

pages = {743--746},

abstract = {Seismological models from Apollo missions provided the first records of the Moon inner structure with a decrease in seismic wave velocities at the core-mantle boundary1-3. The resolution of these records prevents a strict detection of a putative lunar solid inner core and the impact of the lunar mantle overturn in the lowest part of the Moon is still discussed4-7. Here we combine geophysical and geodesic constraints from Monte Carlo exploration and thermodynamical simulations for different Moon internal structures to show that only models with a low viscosity zone enriched in ilmenite and an inner core present densities deduced from thermodynamic constraints compatible with densities deduced from tidal deformations. We thus obtain strong indications in favour of the lunar mantle overturn scenario and, in this context, demonstrate the existence of the lunar inner core with a radius of 258 $pm$ 40 km and density 7,822 $pm$ 1,615 kg m−3. Our results question the evolution of the Moon magnetic field thanks to its demonstration of the existence of the inner core and support a global mantle overturn scenario that brings substantial insights on the timeline of the lunar bombardment in the first billion years of the Solar System8.},

note = {ADS Bibcode: 2023Natur.617..743B},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{charbonnier_astrochronology_2023,

title = {Astrochronology of the Aptian stage and evidence for the chaotic orbital motion of Mercury},

author = {Guillaume Charbonnier and Slah Boulila and Jorge E. Spangenberg and Jean Vermeulen and Bruno Galbrun},

url = {https://ui.adsabs.harvard.edu/abs/2023E&PSL.61018104C},

doi = {10.1016/j.epsl.2023.118104},

issn = {0012-821X},

year  = {2023},

date = {2023-05-01},

urldate = {2023-05-01},

journal = {Earth and Planetary Science Letters},

volume = {610},

pages = {118104},

abstract = {The Aptian stage, between ∼113 and ∼121 million years ago (Ma), was punctuated by a succession of Oceanic Anoxic Events (OAEs), recording extreme global warmings, dramatic expansions of the ocean's oxygen minimum zones, along with perturbations to the biotic and carbon cycles. However, the chronology of the Aptian stage is poorly constrained, impacting the duration and timing of OAEs. Using a greatly expanded sedimentary composite record (380 m) of key outcropping sections in the Vocontian Basin (SE France) combined with available radiometric dates and correlations to a set of astronomical solutions, we provide a constrained absolute astrochronology of the Aptian stage. The 405 kyr (gVenus-gJupiter) eccentricity astronomical timescale indicates a minimal duration of ∼9.4 Myr for the Aptian stage and an age of 122.6 $pm$ 0.3 Ma for the base of the Aptian, consistent with radioisotope dating. We find a deviation in the periodicity of gMercury-gJupiter eccentricity term in the mid-Aptian stage, at ca. 117.19 $pm$ 0.3 Ma, that we ascribe as an expression of the resonance transition σ = (gMercury - gJupiter) - (sMercury - sVenus), in relation with a strong chaotic orbital motion of Mercury. Such a geological observation is supported by a concomitant resonant transition in the La2004 astronomical model.},

note = {ADS Bibcode: 2023E&PSL.61018104C},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{mogavero_timescales_2023,

title = {Timescales of Chaos in the Inner Solar System: Lyapunov Spectrum and Quasi-integrals of Motion},

author = {Federico Mogavero and Nam H. Hoang and Jacques Laskar},

url = {https://ui.adsabs.harvard.edu/abs/2023PhRvX..13b1018M},

doi = {10.1103/PhysRevX.13.021018},

year  = {2023},

date = {2023-04-01},

urldate = {2023-04-01},

journal = {Physical Review X},

volume = {13},

pages = {021018},

abstract = {Numerical integrations of the Solar System reveal a remarkable stability of the orbits of the inner planets over billions of years, in spite of their chaotic variations characterized by a Lyapunov time of only 5 million years and the lack of integrals of motion able to constrain their dynamics. To open a window on such long-term behavior, we compute the entire Lyapunov spectrum of a forced secular model of the inner planets. We uncover a hierarchy of characteristic exponents that spans 2 orders of magnitude, manifesting a slow-fast dynamics with a broad separation of timescales. A systematic analysis of the Fourier harmonics of the Hamiltonian, based on computer algebra, reveals three symmetries that characterize the strongest resonances responsible for the orbital chaos. These symmetries are broken only by weak resonances, leading to the existence of quasi-integrals of motion that are shown to relate to the smallest Lyapunov exponents. A principal component analysis of the orbital solutions independently confirms that the quasi-integrals are among the slowest degrees of freedom of the dynamics. Strong evidence emerges that they effectively constrain the chaotic diffusion of the orbits, playing a crucial role in the statistical stability over the Solar System lifetime.},

note = {ADS Bibcode: 2023PhRvX..13b1018M},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{DeramFienga2022a,

title = {Correction to: Gaia-DR2 asteroid observations and INPOP planetary ephemerides},

author = {P. Deram and A. Fienga and A. K. Verma and M. Gastineau and J. Laskar},

url = {https://ui.adsabs.harvard.edu/abs/2022CeMDA.134...44D},

doi = {10.1007/s10569-022-10089-1},

issn = {0923-2958},

year  = {2022},

date = {2022-10-01},

urldate = {2022-10-01},

journal = {Celestial Mechanics and Dynamical Astronomy},

volume = {134},

pages = {44},

note = {ADS Bibcode: 2022CeMDA.134...44D},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{FarhatAuclair-Desrotour2022a,

title = {The resonant tidal evolution of the Earth-Moon distance},

author = {Mohammad Farhat and Pierre Auclair-Desrotour and Gwenaël Boué and Jacques Laskar},

url = {https://ui.adsabs.harvard.edu/abs/2022A%26A...665L...1F/abstract},

doi = {10.1051/0004-6361/202243445},

issn = {0004-6361},

year  = {2022},

date = {2022-09-01},

urldate = {2022-09-01},

journal = {Astronomy and Astrophysics},

volume = {665},

pages = {L1},

abstract = {Due to tidal interactions in the Earth-Moon system, the spin of the Earth slows down and the Moon drifts away. This recession of the Moon can now be measured with great precision, but it was noticed more than fifty years ago that simple tidal models extrapolated back in time lead to an age of the Moon that is largely incompatible with the geochronological and geochemical evidence. In order to evade this problem, more elaborate models have been proposed, taking into account the oceanic tidal dissipation. However, these models have not been able to fit both the estimated lunar age and the present rate of lunar recession simultaneously. In the present work, we present a physical model that reconciles these two constraints and yields a unique solution for the tidal history. This solution fits the available geological proxies for the history of the Earth-Moon system well and it consolidates the cyclostratigraphic method. Our work extends the lineage of earlier works on the analytical treatment of fluid tides on varying bounded surfaces that is further coupled with solid tidal deformations. This allows us to take into account the time-varying continental configuration on Earth by considering hemispherical and global ocean models. The resulting evolution of the Earth-Moon system involves multiple crossings of resonances in the oceanic dissipation that are associated with significant and rapid variations in the lunar orbital distance, the length of an Earth day and the Earth's obliquity.},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{farhat_resonant_2022,

title = {The resonant tidal evolution of the Earth-Moon distance},

author = {Mohammad Farhat and Pierre Auclair-Desrotour and Gwena"el Boué and Jacques Laskar},

url = {https://ui.adsabs.harvard.edu/abs/2022A&A...665L...1F},

doi = {10.1051/0004-6361/202243445},

issn = {0004-6361},

year  = {2022},

date = {2022-09-01},

urldate = {2022-09-01},

journal = {Astronomy and Astrophysics},

volume = {665},

pages = {L1},

abstract = {Due to tidal interactions in the Earth-Moon system, the spin of the Earth slows down and the Moon drifts away. This recession of the Moon can now be measured with great precision, but it was noticed more than fifty years ago that simple tidal models extrapolated back in time lead to an age of the Moon that is largely incompatible with the geochronological and geochemical evidence. In order to evade this problem, more elaborate models have been proposed, taking into account the oceanic tidal dissipation. However, these models have not been able to fit both the estimated lunar age and the present rate of lunar recession simultaneously. In the present work, we present a physical model that reconciles these two constraints and yields a unique solution for the tidal history. This solution fits the available geological proxies for the history of the Earth-Moon system well and it consolidates the cyclostratigraphic method. Our work extends the lineage of earlier works on the analytical treatment of fluid tides on varying bounded surfaces that is further coupled with solid tidal deformations. This allows us to take into account the time-varying continental configuration on Earth by considering hemispherical and global ocean models. The resulting evolution of the Earth-Moon system involves multiple crossings of resonances in the oceanic dissipation that are associated with significant and rapid variations in the lunar orbital distance, the length of an Earth day and the Earth's obliquity.},

note = {ADS Bibcode: 2022A&A...665L...1F},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{HoangMogavero2022a,

title = {Long-term instability of the inner Solar system: numerical experiments},

author = {Nam H. Hoang and Federico Mogavero and Jacques Laskar},

url = {https://ui.adsabs.harvard.edu/abs/2022MNRAS.514.1342H},

doi = {10.1093/mnras/stac1299},

issn = {0035-8711},

year  = {2022},

date = {2022-07-01},

urldate = {2022-12-01},

journal = {Monthly Notices of the Royal Astronomical Society},

volume = {514},

pages = {1342--1350},

abstract = {Apart from being chaotic, the inner planets in the Solar system constitute an open system, as they are forced by the regular long-term motion of the outer ones. No integrals of motion can bound a priori the stochastic wanderings in their high-dimensional phase space. Still, the probability of a dynamical instability is remarkably low over the next 5 billion years, a time-scale 1000 times longer than the Lyapunov time. The dynamical half-life of Mercury has indeed been estimated recently at 40 billion years. By means of the computer algebra system TRIP, we consider a set of dynamical models resulting from truncation of the forced secular dynamics recently proposed for the inner planets at different degrees in eccentricities and inclinations. Through ensembles of 103-105 numerical integrations spanning 5-100 Gyr, we find that the Hamiltonian truncated at degree 4 practically does not allow any instability over 5 Gyr. The destabilization is mainly due to terms of degree 6. This surprising result suggests an analogy to the Fermi-Pasta-Ulam-Tsingou problem, in which tangency to Toda Hamiltonian explains the very long time-scale of thermalization, which Fermi unsuccessfully looked for.},

note = {ADS Bibcode: 2022MNRAS.514.1342H},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{hoang_long-term_2022,

title = {Long-term instability of the inner Solar system: numerical experiments},

author = {Nam H. Hoang and Federico Mogavero and Jacques Laskar},

url = {https://ui.adsabs.harvard.edu/abs/2022MNRAS.514.1342H},

doi = {10.1093/mnras/stac1299},

issn = {0035-8711},

year  = {2022},

date = {2022-07-01},

urldate = {2022-07-01},

journal = {Monthly Notices of the Royal Astronomical Society},

volume = {514},

pages = {1342--1350},

abstract = {Apart from being chaotic, the inner planets in the Solar system constitute an open system, as they are forced by the regular long-term motion of the outer ones. No integrals of motion can bound a priori the stochastic wanderings in their high-dimensional phase space. Still, the probability of a dynamical instability is remarkably low over the next 5 billion years, a time-scale 1000 times longer than the Lyapunov time. The dynamical half-life of Mercury has indeed been estimated recently at 40 billion years. By means of the computer algebra system TRIP, we consider a set of dynamical models resulting from truncation of the forced secular dynamics recently proposed for the inner planets at different degrees in eccentricities and inclinations. Through ensembles of 103-105 numerical integrations spanning 5-100 Gyr, we find that the Hamiltonian truncated at degree 4 practically does not allow any instability over 5 Gyr. The destabilization is mainly due to terms of degree 6. This surprising result suggests an analogy to the Fermi-Pasta-Ulam-Tsingou problem, in which tangency to Toda Hamiltonian explains the very long time-scale of thermalization, which Fermi unsuccessfully looked for.},

note = {ADS Bibcode: 2022MNRAS.514.1342H},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{mogavero_origin_2022,

title = {The origin of chaos in the Solar System through computer algebra},

author = {Federico Mogavero and Jacques Laskar},

url = {https://ui.adsabs.harvard.edu/abs/2022A&A...662L...3M},

doi = {10.1051/0004-6361/202243327},

issn = {0004-6361},

year  = {2022},

date = {2022-06-01},

urldate = {2022-06-01},

journal = {Astronomy and Astrophysics},

volume = {662},

pages = {L3},

abstract = {The discovery of the chaotic motion of the planets in the Solar System dates back more than 30 years. Still, no analytical theory has satisfactorily addressed the origin of chaos so far. Implementing canonical perturbation theory in the computer algebra system TRIP, we systematically retrieve the secular resonances at work along the orbital solution of a forced long-term dynamics of the inner planets. We compare the time statistic of their half-widths to the ensemble distribution of the maximum Lyapunov exponent and establish dynamical sources of chaos in an unbiased way. New resonances are predicted by the theory and checked against direct integrations of the Solar System. The image of an entangled dynamics of the inner planets emerges.},

note = {ADS Bibcode: 2022A&A...662L...3M},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{SinnesaelLoi2022a,

title = {Cyclostratigraphy of the Middle to Upper Ordovician successions of the Armorican Massif (western France) using portable X-ray fluorescence},

author = {Matthias Sinnesael and Alfredo Loi and Marie-Pierre Dabard and Thijs R. A. Vandenbroucke and Philippe Claeys},

url = {https://gchron.copernicus.org/articles/4/251/2022/},

doi = {10.5194/gchron-4-251-2022},

issn = {2628-3719},

year  = {2022},

date = {2022-05-01},

urldate = {2022-12-03},

journal = {Geochronology},

volume = {4},

number = {1},

pages = {251--267},

abstract = {Abstract. To expand traditional cyclostratigraphic numerical 

methods beyond their common technical limitations and apply them to truly 

deep-time archives, we need to reflect on the development of new approaches 

to sedimentary archives that are not traditionally targeted for 

cyclostratigraphic analysis but that frequently occur in the impoverished 

deep-time record. Siliciclastic storm-dominated shelf environments are a 

good example of such records. Our case study focuses on the Middle to Upper 

Ordovician siliciclastic successions of the Armorican Massif (western 

France) that are well-studied examples in terms of sedimentology and sequence 

stratigraphy. In addition, these sections are protected geological heritage 

due to the extraordinary quality of the outcrops. We therefore tested the 

performance of non-destructive high-resolution (centimeter-scale) portable X-ray 

fluorescence and natural gamma-ray analyses on an outcrop to obtain major 

and trace element compositions. Despite the challenging outcrop conditions 

in the tidal beach zone, our geochemical analyses provide useful information 

regarding general lithology and several specific sedimentary features such 

as the detection of paleo-placers or the discrimination between different 

types of diagenetic concretions such as nodules. Secondly, these new 

high-resolution data are used to experiment with the application of commonly 

used numerical cyclostratigraphic techniques on this siliciclastic 

storm-dominated shelf environment, a non-traditional sedimentological 

setting for cyclostratigraphic analysis. In the parts of the section with a 

relatively homogeneous lithology, spectral power analyses and bandpass 

filtering hint towards a potential astronomical imprint of some sedimentary 

cycles, but this needs further confirmation in the absence of more robust 

independent age constraints.},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{FarhatLaskar2022a,

title = {Constraining the Earth's Dynamical Ellipticity From Ice Age Dynamics},

author = {Mohammad Farhat and Jacques Laskar and Gwenaël Boué},

url = {https://ui.adsabs.harvard.edu/abs/2022JGRB..12723323F},

doi = {10.1029/2021JB023323},

issn = {0148-0227},

year  = {2022},

date = {2022-05-01},

urldate = {2022-05-01},

journal = {Journal of Geophysical Research (Solid Earth)},

volume = {127},

pages = {e2021JB023323},

abstract = {The dynamical ellipticity of a planet expresses the departure of its mass distribution from spherical symmetry. It enters as a parameter in the description of a planet's precession and nutation, as well as other rotational normal modes. In the case of the Earth, uncertainties in this quantity's history produce an uncertainty in the solutions for the past evolution of the Earth-Moon system. Constraining this history has been a target of interdisciplinary efforts as it represents an astro-geodetic parameter whose variation is shaped by geophysical processes, and whose imprints can be found in the geological signal. We revisit the classical problem of its variation during ice ages, where glacial cycles exerted a varying surface loading that had altered the shape of the geoid. In the framework of glacial isostatic adjustment, and with the help of a recent paleoclimatic proxy of ice volume, we present the evolution of the dynamical ellipticity over the Cenozoic ice ages. We map out the problem in full generality identifying major sensitivities to surface loading and internal variations in parameter space. This constrained evolution is aimed to be used in future astronomical computations of the orbital and insolation quantities of the Earth.},

note = {ADS Bibcode: 2022JGRB..12723323F},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{farhat_constraining_2022,

title = {Constraining the Earth's Dynamical Ellipticity From Ice Age Dynamics},

author = {Mohammad Farhat and Jacques Laskar and Gwena"el. Boué},

url = {https://ui.adsabs.harvard.edu/abs/2022JGRB..12723323F},

doi = {10.1029/2021JB023323},

issn = {0148-0227},

year  = {2022},

date = {2022-05-01},

urldate = {2022-05-01},

journal = {Journal of Geophysical Research (Solid Earth)},

volume = {127},

pages = {e2021JB023323},

abstract = {The dynamical ellipticity of a planet expresses the departure of its mass distribution from spherical symmetry. It enters as a parameter in the description of a planet's precession and nutation, as well as other rotational normal modes. In the case of the Earth, uncertainties in this quantity's history produce an uncertainty in the solutions for the past evolution of the Earth-Moon system. Constraining this history has been a target of interdisciplinary efforts as it represents an astro-geodetic parameter whose variation is shaped by geophysical processes, and whose imprints can be found in the geological signal. We revisit the classical problem of its variation during ice ages, where glacial cycles exerted a varying surface loading that had altered the shape of the geoid. In the framework of glacial isostatic adjustment, and with the help of a recent paleoclimatic proxy of ice volume, we present the evolution of the dynamical ellipticity over the Cenozoic ice ages. We map out the problem in full generality identifying major sensitivities to surface loading and internal variations in parameter space. This constrained evolution is aimed to be used in future astronomical computations of the orbital and insolation quantities of the Earth.},

note = {ADS Bibcode: 2022JGRB..12723323F},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{BernusMinazzoli2022a,

title = {Constraining massless dilaton theory at Solar system scales with the planetary ephemeris INPOP},

author = {L. Bernus and O. Minazzoli and A. Fienga and A. Hees and M. Gastineau and J. Laskar and P. Deram and A. Di Ruscio},

url = {https://ui.adsabs.harvard.edu/abs/2022PhRvD.105d4057B},

doi = {10.1103/PhysRevD.105.044057},

issn = {1550-79980556-2821},

year  = {2022},

date = {2022-02-01},

urldate = {2022-12-01},

journal = {Physical Review D},

volume = {105},

pages = {044057},

abstract = {We expose the phenomenology of the massless dilaton theory in the Solar system for a nonuniversal quadratic coupling between the scalar field which represents the dilaton and the matter. Modified post-Newtonian equations of motion of an N -body system and the light time travel are derived from the action of the theory. We use the physical properties of the main planets of the Solar system to reduce the number of parameters to be tested to three in the linear coupling case. In the linear case, we have a universal coupling constant α0 and two coupling constants αT and αG related, respectively, to the telluric bodies and to the gaseous bodies. We then use the planetary ephemeris, INPOP19a, in order to constrain these constants. We succeeded to constrain the linear coupling scenario, and the constraints read α0=(1.01 $pm$23.7 )×10-5 , αT=(0.00 $pm$24.5 )×10-6 , αG=(-1.46 $pm$12.0 )×10-5 , at the 99.5% C.L.},

note = {ADS Bibcode: 2022PhRvD.105d4057B},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{FiengaBigot2022a,

title = {Evolution of INPOP planetary ephemerides and Bepi-Colombo simulations},

author = {A. Fienga and L. Bigot and D. Mary and P. Deram and A. Di Ruscio and L. Bernus and M. Gastineau and J. Laskar},

url = {https://ui.adsabs.harvard.edu/abs/2022IAUS..364...31F},

doi = {10.1017/S1743921321001277},

issn = {1743-9221},

year  = {2022},

date = {2022-01-01},

urldate = {2022-12-01},

journal = {IAU Symposium},

volume = {364},

pages = {31--51},

abstract = {We give here a detailed description of the latest INPOP planetary ephemerides INPOP20a. We test the sensitivity of the Sun oblateness determination obtained with INPOP to different models for the Sun core rotation. We also present new evaluations of possible GRT violations with the PPN parameters β, γ and ?. With a new method for selecting acceptable alternative ephemerides we provide conservative limits of about 7.16 × 10-5 and 7.49 × 10-5 for β-1 and γ-1 respectively using the present day planetary data samples. We also present simulations of Bepi-Colombo range tracking data and their impact on planetary ephemeris construction. We show that the use of future BC range observations should improve these estimates, in particular γ. Finally, interesting perspectives for the detection of the Sun core rotation seem to be reachable thanks to the BC mission and its accurate range measurements in the GRT frame.},

note = {ADS Bibcode: 2022IAUS..364...31F},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{HoangMogavero2021a,

title = {Chaotic diffusion of the fundamental frequencies in the Solar System},

author = {Nam H. Hoang and Federico Mogavero and Jacques Laskar},

url = {https://ui.adsabs.harvard.edu/abs/2021A%26A...654A.156H/abstract},

doi = {10.1051/0004-6361/202140989},

issn = {0004-6361},

year  = {2021},

date = {2021-10-01},

urldate = {2022-12-01},

journal = {Astronomy & Astrophysics, Volume 654, id.A156, textlessNUMPAGEStextgreater18textless/NUMPAGEStextgreater pp.},

volume = {654},

pages = {A156},

abstract = {The long-term variations in the orbit of the Earth govern the insolation on its surface and hence its climate. The use of the astronomical signal, whose imprint has been recovered in the geological records, has revolutionized the determination of the geological timescales. However, the orbital variations beyond 60 Myr cannot be reliably predicted because of the chaotic dynamics of the planetary orbits in the Solar System. Taking this dynamical uncertainty to account is necessary for a complete astronomical calibration of geological records. Our work addresses this problem with a statistical analysis of 120 000 orbital solutions of the secular model of the Solar System ranging from 500 Myr to 5 Gyr. We obtain the marginal probability density functions of the fundamental secular frequencies using kernel density estimation. The uncertainty of the density estimation is also obtained here in the form of confidence intervals determined by the moving block bootstrap method. The results of the secular model are shown to be in good agreement with those of the direct integrations of a comprehensive model of the Solar System. Application of our work is illustrated on two geological data sets: the Newark-Hartford records and the Libsack core. textlessP /textgreaterThe density estimation of the fundamental frequencies and their combinations are only available at the CDS via anonymous ftp to textlessA href="http://cdsarc.u-strasbg.fr"textgreatercdsarc.u-strasbg.frtextless/Atextgreater (ftp://130.79.128.5) or via textlessA href="http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/654/A156"textgreaterhttp://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/654/A156textless/Atextgreater},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{hoang_chaotic_2021,

title = {Chaotic diffusion of the fundamental frequencies in the Solar System},

author = {Nam H. Hoang and Federico Mogavero and Jacques Laskar},

url = {https://ui.adsabs.harvard.edu/abs/2021A&A...654A.156H},

doi = {10.1051/0004-6361/202140989},

issn = {0004-6361},

year  = {2021},

date = {2021-10-01},

urldate = {2021-10-01},

journal = {Astronomy and Astrophysics},

volume = {654},

pages = {A156},

abstract = {The long-term variations in the orbit of the Earth govern the insolation on its surface and hence its climate. The use of the astronomical signal, whose imprint has been recovered in the geological records, has revolutionized the determination of the geological timescales. However, the orbital variations beyond 60 Myr cannot be reliably predicted because of the chaotic dynamics of the planetary orbits in the Solar System. Taking this dynamical uncertainty to account is necessary for a complete astronomical calibration of geological records. Our work addresses this problem with a statistical analysis of 120 000 orbital solutions of the secular model of the Solar System ranging from 500 Myr to 5 Gyr. We obtain the marginal probability density functions of the fundamental secular frequencies using kernel density estimation. The uncertainty of the density estimation is also obtained here in the form of confidence intervals determined by the moving block bootstrap method. The results of the secular model are shown to be in good agreement with those of the direct integrations of a comprehensive model of the Solar System. Application of our work is illustrated on two geological data sets: the Newark-Hartford records and the Libsack core. The density estimation of the fundamental frequencies and their combinations are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/654/A156},

note = {ADS Bibcode: 2021A&A...654A.156H},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{boulila_potential_2021,

title = {Potential encoding of coupling between Milankovitch forcing and Earth's interior processes in the Phanerozoic eustatic sea-level record},

author = {Slah Boulila and Bilal U. Haq and Nathan Hara and R. Dietmar Müller and Bruno Galbrun and Guillaume Charbonnier},

url = {https://ui.adsabs.harvard.edu/abs/2021ESRv..22003727B},

doi = {10.1016/j.earscirev.2021.103727},

issn = {0012-8252},

year  = {2021},

date = {2021-09-01},

urldate = {2021-09-01},

journal = {Earth Science Reviews},

volume = {220},

pages = {103727},

abstract = {The driving mechanisms of Earth's climate system at a multi-Myr timescale have received considerable attention since the 1980's as they are deemed to control large-amplitude climatic variations that result in severe biogeochemical disruptions, major sea-level variations, and the evolution of Earth's land- and seascapes through geological time. The commonly accepted mechanism for these changes derives from the evolution of Earth's coupled plate-mantle system. Connection between Earth's interior and external climate drivers, e.g., Milankovitch insolation forcing, has not been investigated at multi-Myr timescale, because tectonics and astronomical influences at these longer timescales have long been thought as independent pacemakers in the evolution of the Earth system. Here we have analyzed time-series from multiple geological datasets and found common periodicities of 10 and 35 Myr. Additionally, we have highlighted the modulation in amplitude of the 10 Myr cycle band by the 35 Myr cyclicity in sedimentary sea-level data. We then demonstrate the same physical amplitude modulation relationship between these two cyclicities in astronomical (Milankovitch) variations, and establish correlation between Milankovitch and sea-level variations at these two frequency bands. The 10 and 35 Myr cycles are prominent in the geological records, suggesting either unresolved fundamental Milankovitch periodicities, or reflecting a sedimentary energy-transfer process from higher to lower Milankovitch frequencies, as argued here via amplitude modulation analysis in both astronomical and sea-level data. Finally, we find a coherent correlation, at the 35 Myr cycle band, between Milankovitch, sea-level and geodynamic (plate subduction rate) variations, hinting at a coupling between Earth's interior and surface processes via Milankovitch paced climate. Thus, our findings point to a coupling between Milankovitch and Earth's internal forcings, at 10 to 10s of Myr. The most likely scenario that could link insolation-driven climate change to Earth's interior processes is Earth's interior feedbacks to astro-climatically driven mass changes on Earth's surface. We suggest that Earth's interior processes may drive large-amplitude sea-level changes, especially during greenhouse periods, by resonating to astro-climatically driven Earth's surface perturbations.},

note = {ADS Bibcode: 2021ESRv..22003727B},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{FiengaDeram2021a,

title = {INPOP21a planetary ephemerides},

author = {A. Fienga and P. Deram and A. Di Ruscio and V. Viswanathan and J. I. B. Camargo and L. Bernus and M. Gastineau and J. Laskar},

url = {https://ui.adsabs.harvard.edu/abs/2021NSTIM.110.....F},

year  = {2021},

date = {2021-06-01},

urldate = {2022-12-01},

journal = {Notes Scientifiques et Techniques de l'Institut de Mecanique Celeste},

volume = {110},

abstract = {The major points of improvement of INPOP21a relative to INPOP19a are i) the addition of 2 years of Mars Express data and 1 year of Juno normal points, ii) the use of new Uranus ground-based optical observations reduced with the Gaia DR3, iii) the modification of the dynamical modeling for the Kuiper belt object perturbations, and iv) the first determination of the Sun oblateness including the Lense-Thirring effect.},

note = {ADS Bibcode: 2021NSTIM.110.....F},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{WangLi2021a,

title = {Sedimentary noise modeling of lake-level change in the late Triassic Newark Basin of North America},

author = {Meng Wang and Mingsong Li and David B. Kemp and Slah Boulila and James G. Ogg},

year  = {2021},

date = {2021-01-01},

journal = {Global and Planetary Change},

pages = {103706},

note = {Publisher: Elsevier},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{MogaveroLaskar2021a,

title = {Long-term dynamics of the inner planets in the Solar System},

author = {Federico Mogavero and Jacques Laskar},

year  = {2021},

date = {2021-01-01},

journal = {Astronomy & Astrophysics},

volume = {655},

pages = {A1},

note = {Publisher: EDP Sciences},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{BoulilaHaq2021a,

title = {Potential encoding of coupling between Milankovitch forcing and Earth's interior processes in the Phanerozoic eustatic sea-level record},

author = {Slah Boulila and Bilal U. Haq and Nathan Hara and R. Dietmar Müller and Bruno Galbrun and Guillaume Charbonnier},

year  = {2021},

date = {2021-01-01},

journal = {Earth-Science Reviews},

volume = {220},

pages = {103727},

note = {Publisher: Elsevier},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{BoulilaDupont-Nivet2021a,

title = {Age and driving mechanisms of the Eocene-Oligocene Transition from astronomical tuning of a lacustrine record (Rennes Basin, France)},

author = {Slah Boulila and Guillaume Dupont-Nivet and Bruno Galbrun and Hugues Bauer and Jean-Jacques Ch^ateauneuf},

year  = {2021},

date = {2021-01-01},

journal = {Climate of the Past Discussions},

pages = {1--27},

note = {Publisher: Copernicus GmbH},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{Di-RuscioFienga2020a,

title = {New constraints on the Kuiper belt mass and P9 location from INPOP19a planetary ephemerides},

author = {Andrea Di Ruscio and Agnes Fienga and Léo Bernus and Pierre Deram and Daniele Durante and Luciano Iess and Jacques Laskar and Mickaël Gastineau},

url = {https://ui.adsabs.harvard.edu/abs/2020EPSC...14..804D},

doi = {10.5194/epsc2020-804},

year  = {2020},

date = {2020-09-01},

urldate = {2020-09-01},

pages = {EPSC2020--804},

abstract = {The accuracy achieved by modern deep space radio tracking systems has dramatically increased the precision of planetary ephemerides in the last decade. This improvement is particularly beneficial to the study of the trans-Neptunian solar system, still a relatively unknown region (Prialnik et al. 2020).The Kuiper belt has a pivotal role in our understanding of the outer solar system, and a better constrain of its mass inferred by its gravity perturbations on the planets can help to explain the observed clustering of Kuiper belt objects (KBO), and the potential presence of a ninth planet beyond the orbit of Neptune, P9 (Batygin et al. 2019).We thus provide a new estimate of the cumulative mass of KBOs located in the 2:1 and 3:2 mean motion resonances with Neptune deduced from INPOP19a. INPOP19a is the last version of INPOP planetary ephemeris, which, among the numerous updates (Fienga et al. 2019), benefits from the addition of the new normal points obtained with the gravity experiment of the Juno mission and the new normal points deduced from Cassini radio tracking data. The latter, in particular, play a decisive role for constraining the mass of the Kuiper belt, thanks to the enhanced accuracy registered in the analysis of navigation and gravity data (Di Ruscio et al. 2020; Durante et al. 2019) and the extended time-frame covered with the inclusion of the Grand Finale measurements (Iess et al. 2019).We modeled the Kuiper belt by including in INPOP dynamical model three circular, not inclined rings located at 39.4, 44.0, and 47.5 AU, to which we attributed one-sixth, two-thirds, and one-sixth of the total mass, respectively, using the same approach adopted by Pitjeva & Pitjev (2018). In addition, we included the orbits of nine KBOs, beside Pluto, whose masses are independently constrained by observations of their satellites dynamics.Solving for the mass of the Kuiper belt together with the orbits of the eight planets of the solar system, Pluto, and the Moon, plus the mass of 343 asteroids of the main belt, we fitted the entire INPOP dataset (Fienga et al. 2019) and estimated a total mass for the rings of KBOs of (0.061 $pm$ 0.001)M⊕.We also provide new constraints on the location of P9 by analyzing the potential gravity perturbation on planetary ephemerides, specifically on the orbit of Saturn. We used two statistical criteria to identify the possible regions compatible with INPOP19a: i) based on the propagated covariance matrix, and ii) on the χ2 likelihood of P9-perturbed postfit residuals (Fienga et al. 2020). We show that, according to INPOP19a, there is no clear evidence for the existence of P9, but we identified two zones for which its existence is compatible with the accuracy of INPOP planetary ephemerides (see Fig. 1).Fig. 1. The plots show the two compatible zones we identified for the potential location of P9 with a mass of 5 M⊕ at a distance of 600 AU. The x and y axes report the angular position in Right Ascension (RA) and Declination (Dec) of the planet in the International Celestial Reference Frame. The colorbar indicates the χ2 Likelihood computed for each P9-perturbed solution. References:Batygin, K., Adams, F. C., Brown, M. E., and Becker, J. C. 2019, "The Planet Nine Hypothesis", Physics Reports, 805Di Ruscio, A., Fienga, A., Durante, D., Iess, L., Laskar, J., and Gastineau, M. 2020, "Analysis of Cassini radio tracking data for the construction of INPOP19a: A new estimate of the Kuiper belt mass", A&A, Forthcoming articleDurante, D., Hemingway, D. J., Racioppa, P., Iess, L., and Stevenson, D. J. 2019, "Titan's gravity field and interior structure after Cassini", Icarus, 326, 123Fienga, A., Deram, P., Viswanathan, V., Di Ruscio, A., Bernus, L., Durante, D., Gastineau, M., and Laskar, J. 2019, "INPOP19a planetary ephemerides", NSTIM, 109Fienga, A., Di Ruscio, A., Bernus, L. Deram, P., Durante, D., Laskar, J., and Iess, L. 2020, "New constraints on the location of P9 obtained with the INPOP19a planetary ephemeris", A&A, Forthcoming articleIess, L., Militzer, B., Kaspi, Y., et al. 2019, "Measurement and implications of Saturn"s gravity field and ring mass", Science, 364Pitjeva, E. V. & Pitjev, N. P. 2018, "Mass of the Kuiper belt", Celest. Mech. Dyn. Astron, 130, 57Prialnik, D., Barucci, M., and Young, L. 2020, "The Trans-Neptunian Solar System", Elsevier},

note = {Conference Name: European Planetary Science Congress ADS Bibcode: 2020EPSC...14..804D},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{BernusMinazzoli2020a,

title = {Constraint on the Yukawa suppression of the Newtonian potential from the planetary ephemeris INPOP19a},

author = {L. Bernus and O. Minazzoli and A. Fienga and M. Gastineau and J. Laskar and P. Deram and A. Di Ruscio},

url = {https://ui.adsabs.harvard.edu/abs/2020PhRvD.102b1501B},

doi = {10.1103/PhysRevD.102.021501},

issn = {1550-79980556-2821},

year  = {2020},

date = {2020-07-01},

urldate = {2022-12-01},

journal = {Physical Review D},

volume = {102},

pages = {021501},

abstract = {We use the latest solution of the ephemeris INPOP (19a) in order to improve our previous constraint on the existence of a Yukawa suppression to the Newtonian potential, generically associated to a graviton's mass. Unlike the ephemeris INPOP17a, several residuals are found to degrade significantly at roughly the same amplitudes of the Compton wavelength λg. As a consequence, we introduce a novel statistical criterion in order to derive the constraint with INPOP19a. After checking that it leads to a constraint consistent with our previous result when applied on INPOP17b, we apply the method to the new solution INPOP19a. We show that the residuals of Mars orbiters, Cassini, Messenger, and Juno, degrade significantly when λg≤3.43 ×1013 km with a 99.7% confidence level---corresponding to a graviton mass bigger than 3.62 ×10-23 eV /c2. This is a stronger constraint on the Compton wavelength than the one obtained from the first gravitational-wave transient catalog by the LIGO-Virgo Collaboration in the radiative regime, since our 90% C.L. limit reads λgtextgreater3.93 ×1013 km (mgtextless3.16 ×10-23 eV /c2 ).},

note = {ADS Bibcode: 2020PhRvD.102b1501B},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{2020A&A...640A...7D,

title = {Analysis of Cassini radio tracking data for the construction of INPOP19a: A new estimate of the Kuiper belt mass},

author = {A {Di Ruscio} and A {Fienga} and D {Durante} and L {Iess} and J {Laskar} and M {Gastineau}},

doi = {10.1051/0004-6361/202037920},

year  = {2020},

date = {2020-01-01},

urldate = {2020-01-01},

pages = {A7},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{HilgenZeeden2020a,

title = {Paleoclimate records reveal elusive∼ 200-kyr eccentricity cycle for the first time},

author = {Frits Hilgen and Christian Zeeden and Jacques Laskar},

year  = {2020},

date = {2020-01-01},

journal = {Global and Planetary Change},

volume = {194},

pages = {103296},

note = {Publisher: Elsevier},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{GalbrunBoulila2020a,

title = {" Short" or" long" Rhaetian? Astronomical calibration of Austrian key sections},

author = {Bruno Galbrun and Slah Boulila and Leopold Krystyn and Sylvain Richoz and Silvia Gardin and Annachiara Bartolini and Martin Maslo},

year  = {2020},

date = {2020-01-01},

journal = {Global and Planetary Change},

volume = {192},

pages = {103253},

note = {Publisher: Elsevier},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{BoulilaCharbonnier2020a,

title = {Unraveling short-and long-term carbon cycle variations during the Oceanic Anoxic Event 2 from the Paris Basin Chalk},

author = {Slah Boulila and Guillaume Charbonnier and Jorge E. Spangenberg and Silvia Gardin and Bruno Galbrun and Justine Briard and Laurence Le Callonnec},

year  = {2020},

date = {2020-01-01},

journal = {Global and Planetary Change},

volume = {186},

pages = {103126},

note = {Publisher: Elsevier},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{BoulilaBrange2020a,

title = {Astronomical pacing of Late Cretaceous third-and second-order sea-level sequences in the Foz do Amazonas Basin},

author = {Slah Boulila and Célia Brange and Alberto Machado Cruz and Jacques Laskar and Christian Gorini and Tadeu Dos Reis and Cleverson Guizan Silva},

year  = {2020},

date = {2020-01-01},

journal = {Marine and Petroleum Geology},

volume = {117},

pages = {104382},

note = {Publisher: Elsevier},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{FiengaDeram2019a,

title = {INPOP19a planetary ephemerides},

author = {A. Fienga and P. Deram and V. Viswanathan and A. Di Ruscio and L. Bernus and D. Durante and M. Gastineau and J. Laskar},

url = {https://ui.adsabs.harvard.edu/abs/2019NSTIM.109.....F},

year  = {2019},

date = {2019-12-01},

urldate = {2022-12-01},

journal = {Notes Scientifiques et Techniques de l'Institut de Mecanique Celeste},

volume = {109},

abstract = {INPOP19a is the new ephemerides for the orbits of the 8 planets of the solar system, the moon, Pluto as well as 14000 asteroids. It is fitted over about 155000 planetary observations including 9 positions of Jupiter deduced from the Juno mission, an extension of the Cassini data sample from 2014 to 2017 for the Saturn orbit and of the MEX data from 2016.4 to 2017.4 for the Mars orbit. The asteroid orbits were fitted on the almost 2 millions of observations obtained by the GAIA mission and delivered with the DR2. The INPOP dynamical modeling was also modified in comparison to the previous version, INPOP17a. A ring modeling the accelerations induced by Trans-Neptunian objects as well as the 9 most massive TNOs have been added in order to improve the fit to the Saturn observations. A new estimation of the TNO ring mass has been produced. Finally, a new Bayesian procedure for the computation of the masses of 343 main-belt asteroids has been applied and leads to an important improvement in the accuracy of the Mars orbit and of its extrapolation capabilities.},

note = {ADS Bibcode: 2019NSTIM.109.....F},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{BernusMinazzoli2019a,

title = {Constraining the Mass of the Graviton with the Planetary Ephemeris INPOP},

author = {L. Bernus and O. Minazzoli and A. Fienga and M. Gastineau and J. Laskar and P. Deram},

url = {https://ui.adsabs.harvard.edu/abs/2019PhRvL.123p1103B},

doi = {10.1103/PhysRevLett.123.161103},

issn = {0031-9007},

year  = {2019},

date = {2019-10-01},

urldate = {2022-12-01},

journal = {Physical Review Letters},

volume = {123},

pages = {161103},

abstract = {We use the planetary ephemeris INPOP17b to constrain the existence of a Yukawa suppression to the Newtonian potential, generically associated with the graviton's mass. We also give an interpretation of this result for a specific case of fifth force framework. We find that the residuals for the Cassini spacecraft significantly (90% C.L.) degrade for Compton wavelengths of the graviton smaller than 1.83 ×1013 km , which correspond to a graviton mass bigger than 6.76 ×10-23 eV /c2. This limit is comparable in magnitude to the one obtained by the LIGO-Virgo Collaboration in the radiative regime. We also use this specific example to defend that constraints on alternative theories of gravity obtained from postfit residuals may be generically overestimated.},

note = {ADS Bibcode: 2019PhRvL.123p1103B},

keywords = {},

pubstate = {published},

tppubtype = {article}

}

@article{RambauxViswanathan2019a,

title = {Dynamical model of lunar core and observational constraint from Lunar Laser Ranging},

author = {Nicolas Rambaux and Vishnu Viswanathan and Agnes Fienga and Jacques Laskar and Mickael Gastineau},

url = {https://ui.adsabs.harvard.edu/abs/2019EPSC...13.1607R},

year  = {2019},

date = {2019-09-01},

urldate = {2022-12-01},

volume = {2019},

pages = {EPSC--DPS2019--1607},

abstract = {Our Moon is one of the most studied objects in the Solar system; we benefit from chemical, geophysical, and geodetical observations achieved by multiple Earth ground based telescopes and in situ missions such as GRAIL and Apollo. However, its deep interior properties remains a puzzle because the lunar core is very small implying small signature in the observational data set. This paper focuses on the description of a new lunar core rotational model included in INPOP and used to provide a determination of the radius and geometry of the lunar core-mantle boundary (CMB) from the LLR observations.},

note = {Conference Name: EPSC-DPS Joint Meeting 2019 ADS Bibcode: 2019EPSC...13.1607R},

keywords = {},

pubstate = {published},

tppubtype = {article}

}