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

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 p...

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Vydáno v:	The European physical journal. C, Particles and fields Ročník 79; číslo 8; s. 1 - 12
Hlavní autoři:	Iorio, Lorenzo, Rieutord, Michel, Rozelot, Jean-Pierre, de Souza, Armando Domiciano
Médium:	Journal Article
Jazyk:	angličtina
Vydáno:	Berlin/Heidelberg Springer Berlin Heidelberg 01.08.2019 Springer Springer Nature B.V Springer Verlag (Germany) SpringerOpen
Témata:	Analysis Angular momentum Astronomy Astrophysics Astrophysics and Cosmology Binary stars Dipoles Electric waves Electromagnetic radiation Electromagnetic waves Elementary Particles Ellipticity General Relativity and Quantum Cosmology Gravitational fields Gravity Hadrons Heavy Ions Main sequence stars Measurement Science and Instrumentation Millisecond pulsars Nuclear Energy Nuclear Physics Orbits Physics Physics and Astronomy Quadrupoles Quantum Field Theories Quantum Field Theory Regular Article - Theoretical Physics Stellar rotation String Theory Time lag Wave propagation
ISSN:	1434-6044, 1434-6052
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Popis
Shrnutí:	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 p 2 / R e 2 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 Δ δ τ of the Rømer-like, orbital component of the pulsar’s time delay δ τ induced over 10 years by the pN gravitoelectric mass monopole Schwarzschild , G M c - 2 , quadrupole G M R e 2 J 2 c - 2 , gravitomagnetic spin dipole Lense - Thirring , G S c - 2 and octupole G S R e 2 ε 2 c - 2 accelerations along with the Newtonian quadrupolar G M R e 2 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 days, 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 G M c - 2 , ≲ 10 - 40 ms G M R e 2 J 2 c - 2 , ≲ 0.5 - 6 ms G S c - 2 , ≲ 5 - 20 μ s G S R e 2 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 ( G M c - 2 , G M J 2 c - 2 , and, perhaps, G S c - 2 as well) key features of the distorted gravitational fields of the fast rotating stars hosted by them.
Bibliografie:	ObjectType-Article-1 SourceType-Scholarly Journals-1 ObjectType-Feature-2 content type line 14
ISSN:	1434-6044 1434-6052
DOI:	10.1140/epjc/s10052-019-7194-5