The post-Newtonian gravitomagnetic spin-octupole moment of an oblate rotating body and its effects on an orbiting test particle; are they measurable in the Solar system?

Iorio, Lorenzo

doi:10.1093/mnras/stz304

Cited by 12 publications

(14 citation statements)

References 33 publications

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“…are the components of the particle's velocity v along the radial direction and the primary's spin respectively. The averaged rates of change of the semimajor axis a, the eccentricity e, the inclination I, the longitude of the ascending node Ω and the argument of pericenter ω induced by Equations ( 1) to (2) were analytically calculated for a general orientation of Ŝ in space by Iorio (2015Iorio ( , 2019; previous derivations of the gravitoelectric mass quadrupole effects in the particular case of an equatorial coordinate system with its reference z axis aligned with Ŝ can be found in Soffel et al (1987); Soffel (1989); Brumberg (1991); .…”

Section: Introductionmentioning

confidence: 99%

“…In this paper, we will preliminarily explore the perspectives of measuring, for the first time, some consequences of Equations ( 1) to (2) by suitably designing a dedicated drag-free satellite-based mission around the Earth encompassing a highly eccentric geocentric orbit exploiting the frozen perigee configuration; we provisionally name it as HERO (Highly Eccentric Relativity Orbiter). For some embryonal thoughts about the possibility of using an Earth's spacecraft to measure the pN gravitoelectric effects proportional to GJ 2 /c 2 , see Iorio (2013Iorio ( , 2015; for deeper investigations concerning a possible probe around Jupiter to measure them and the pN gravitomagnetic signature proportional to GS ε 2 /c 2 , see Iorio (2013Iorio ( , 2019. About the propagation of the electromagnetic waves in the deformed spacetime of an oblate body and the perspectives of measuring the resulting deflection due to Jupiter with astrometric techniques, see, e.g., Crosta & Mignard (2006); Kopeikin & Makarov (2007); Le Poncin-Lafitte & Teyssandier (2008); Abbas, Bucciarelli & Lattanzi (2019), and references therein.…”

Section: Introductionmentioning

confidence: 99%

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A HERO for General Relativity

Iorio

2019

Universe

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HERO (Highly Eccentric Relativity Orbiter) is a space-based mission concept aimed to perform several tests of post-Newtonian gravity around the Earth with a preferably drag-free spacecraft moving along a highly elliptical path fixed in its plane undergoing a relatively fast secular precession. We considered two possible scenarios: a fast, 4-hr orbit with high perigee height of 1, 047 km, and a slow, 21-hr path with a low perigee height of 642 km. HERO may detect, for the first time, the post-Newtonian orbital effects induced by the mass quadrupole moment J 2 of the Earth which, among other things, affects the semimajor axis a via a secular trend of ≃ 4 − 12 cm yr −1 , depending on the orbital configuration. Recently, the secular decay of the semimajor axis of the passive satellite LARES was measured with an error as little as 0.7 cm yr −1 . Also the post-Newtonian spin dipole (Lense-Thirring) and mass monopole (Schwarzschild) effects could be tested to a high accuracy depending on the level of compensation of the non-gravitational perturbations, not treated here. Moreover, the large eccentricity of the orbit would allow to constrain several long-range modified models of gravity and to accurately measure the gravitational red-shift as well. Each of the six Keplerian orbital elements could be individually monitored to extract the GJ 2 /c 2 signature, or they could be suitably combined in order to disentangle the post-Newtonian effect(s) of interest from the competing mismodeled Newtonian secular precessions induced by the zonal harmonic multipoles J ℓ of the geopotential. In the latter case, the systematic uncertainty due to the current formal errors σ J ℓ of a recent global Earth's gravity field model are better than 1% for all the post-Newtonian effects considered, with a peak of ≃ 10 −7 for the Schwarzschild-like shifts. Instead, the gravitomagnetic spin octupole precessions are too small to be detectable.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

A HERO for General Relativity

Iorio

2019

Universe

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“…Nevertheless, some indication of irregular, non-periodic behavior in the contribution of the relativistic corrections may be disclosed in this period of time, and in the case of resonant orbits, chaotic motion in certain configurations may arise. In connection with the mission proposal in this paper, we should notice that Iorio has also proposed a Jovian probe to test the post-Newtonian gravitomagnetic spin octupole of Jupiter [37]. However, our focus is on the classical resonant trajectories and their modification by general relativistic corrections to the equations of motion instead of the gravity field of Jupiter in itself.…”

Section: Introductionmentioning

confidence: 99%

Monitoring Jovian Orbital Resonances of a Spacecraft: Classical and Relativistic Effects

Acedo¹

2019

Universe

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Orbital resonances continue to be one of the most difficult problems in celestial mechanics. They have been studied in connection with the so-called Kirkwood gaps in the asteroid belt for many years. On the other hand, resonant trans-Neptunian objects are also an active area of research in Solar System dynamics, as are the recently discovered resonances in extrasolar planetary systems. A careful monitoring of the trajectories of these objects is hindered by the small size of asteroids or the large distances of the trans-Neptunian bodies. In this paper, we propose a mission concept, called CHRONOS (after the greek god of time), in which a spacecraft could be sent to with the initial condition of resonance with Jupiter in order to study the future evolution of its trajectory. We show that radio monitoring of these trajectories could allow for a better understanding of the initial stages of the evolution of resonant trajectories and the associated relativistic effects.

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“…In its weak-field and slow-motion approximation, general relativity predicts that, in addition to the time-honored post-Newtonian (pN) gravitoelectric and gravitomagnetic precessions induced by the mass M (Schwarzschild) and the spin angular momentum S (Lense-Thirring) of the central body acting as source of the gravitational field, other pN gravitoelectric and gravitomagnetic orbital effects related to its oblateness arise as well (Soffel 1989;Soffel et al 1987;Heimberger, Soffel & Ruder 1990;Brumberg 1991;Will 2014;Panhans & Soffel 2014;Iorio 2015;Meichsner & Soffel 2015;Soffel & Frutos 2016;Frutos-Alfaro & Soffel 2018;Schanner & Soffel 2018). So far, they have never been put to the test in any astronomical and astrophysical scenarios, despite some recent preliminary investigations pertaining the planet Jupiter in our solar system (Iorio 2013(Iorio , 2019; for some embryonic thoughts about an Earth-spacecraft scenario, see Iorio (2013Iorio ( , 2015. To the pN level, the oblateness of astronomical bodies modifies also the propagation of the electromagnetic waves in their deformed spacetime.…”

Section: Introductionmentioning

confidence: 99%

“…An analysis of the analytical expressions of the pN gravitoelectric and gravitomagnetic orbital precessions due to the asphericity of the primary (Iorio 2015(Iorio , 2019 shows that the key ingredients needed to enhance their magnitude are a strongly distorted central body, and a highly eccentric and close orbit of the moving particle.…”

Section: Introductionmentioning

confidence: 99%

Classical and general relativistic post-Keplerian effects in binary pulsars hosting fast rotating main sequence stars

et al. 2019

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We consider a binary system composed of a pulsar and a massive, fast rotating, highly distorted main sequence star of mass M, spin angular momentum S, dimensionless mass quadrupole moment J 2 , equatorial and polar radii R e , R p , flattening ν (R e −R p )/R e , and ellipticity ε 1 − R 2 p /R 2 e as a potential scenario to dynamically put to the test certain post-Keplerian effects of both Newtonian and post-Newtonian nature. We numerically produce time series of the perturbations ∆ (δτ) of the Rømerlike, orbital component of the pulsar's time delay δτ induced over 10 years by the pN gravitoelectric mass monopole Schwarzschild, GMc −2 , quadrupole GMR 2 e J 2 c −2 , gravitomagnetic spin dipole Lense-Thirring, GS c −2 and octupole GS R 2 e ε 2 c −2 accelerations along with the Newtonian quadrupolar GMR 2 e J 2 one. We do not deal with the various propagation time delays due to the travelling electromagnetic waves. It turns out that, for a Be-type star with M = 15 M , R e = 5.96 R , ν = 0.203, S = 3.41×10 45 J s, J 2 = 1.92×10 −3 orbited by a pulsar with an orbital period P b 40−70 d, the classical oblateness-driven effects are at the 4 − 150 s level, while the pN shifts are of the order of 1.5 − 20 s GMc −2 , 10 − 40 ms GMR 2 e J 2 c −2 , 0.5 − 6 ms GS c −2 , 5 − 20 µs GS R 2 e ε 2 c −2 , depending on their orbital configuration. The root-mean-square (rms) timing residuals σ τ of almost all the existing non-recycled, non-millisecond pulsars orbiting massive, fast rotating main sequence stars are ms. Thus, such kind of binaries have the potential to become interesting laboratories to measure, or, at least, constrain, some Newtonian and post-Newtonian (GMc −2 , GMJ 2 c −2 , and, perhaps, GS c −2 as well) key features of the distorted gravitational fields of the fast rotating stars hosted by them.

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The post-Newtonian gravitomagnetic spin-octupole moment of an oblate rotating body and its effects on an orbiting test particle; are they measurable in the Solar system?

Cited by 12 publications

References 33 publications

A HERO for General Relativity

A HERO for General Relativity

Monitoring Jovian Orbital Resonances of a Spacecraft: Classical and Relativistic Effects

Classical and general relativistic post-Keplerian effects in binary pulsars hosting fast rotating main sequence stars

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