15 years of high precision astrometry in the Galactic Center

Gillessen, S.; Genzel, R.; Eisenhauer, F.; Ott, Thomas; Trippe, Sascha; Martins, F.

doi:10.1017/s1743921308019820

Cited by 2 publications

(1 citation statement)

References 8 publications

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“…Then, all the multipole moments of its external spacetime are functions of just M • and J • . For other studies involving the S stars and various consequences of the gravitomagnetic field of Sgr A * , see Jaroszynski (1998), Levin & Beloborodov (2003), Kraniotis (2007), Gillessen et al (2008), Will (2008) In this paper, the perspectives of measuring the gravitomagnetic spin-induced orbital precessions of S4716 are investigated. As far as the gravitoelectric (GE), Schwarzschild-like perinigricon precession is concerned, it was recently measured with the S2 star to a 15% accuracy level (Gravity Collaboration et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Is It Possible to Measure the Lense–Thirring Orbital Shifts of the Short-period S Star S4716 Orbiting Sgr A*?

Iorio

2023

ApJ

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The maximal values of the general relativistic Lense–Thirring (LT) orbital shifts ΔI LT, ΔΩLT, and Δω LT of the inclination I, the longitude of the ascending node Ω, and the perinigricon ω, respectively, of the recently discovered star S4716, which has the shortest orbital period P b = 4.02 yr of all the S stars that orbit the supermassive black hole (SMBH) in Sgr A*, are of the order of ≃5–16 arcseconds per revolution ″ rev − 1 . Given the current error σ ω = 0.°02 in determining ω, which is the most accurate orbital parameter of S4716 among all those affected by the SMBH's gravitomagnetic field through its angular momentum J •, about 48 yr would be needed to reduce σ ω to ≃10% of the cumulative LT perinigricon shift over the same time span. Measuring ΔI LT and ΔΩLT to the same level of accuracy would take much longer. Instead, after just 16 yr, a percent measurement of the larger gravitoelectric (GE) Schwarzschild-like perinigricon shift Δω GE, which depends only on the SMBH's mass M •, would be possible. On the other hand, the uncertainties in the physical and orbital parameters entering Δω GE would cause a huge systematic bias of Δω LT itself. The SMBH's quadrupole mass moment Q 2 • induces orbital shifts as little as ≃0.01–0.05″ rev−1.

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Section: Introductionmentioning

confidence: 99%

Is It Possible to Measure the Lense–Thirring Orbital Shifts of the Short-period S Star S4716 Orbiting Sgr A*?

Iorio

2023

ApJ

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Evolution of eccentric stellar discs around supermassive black holes: the complex disc disruption dynamics and the milliparsec stars

Rantala,

Naab

2023

Monthly Notices of the Royal Astronomical Society

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We study the 10 Myr evolution of parsec-scale stellar disks with initial masses of Mdisk = 1.0–7.5 × 104 M⊙ and eccentricities einit = 0.1–0.9 around supermassive black holes (SMBHs). Our disk models are embedded in a spherical background potential and have top-heavy single and binary star initial mass functions (IMF) with slopes of 0.25–1.7. The systems are evolved with the N-body code BIFROST including post-Newtonian (PN) equations of motion and simplified stellar evolution. All disks are unstable and evolve on Myr timescales towards similar eccentricity distributions peaking at e⋆ ∼ 0.3–0.4. Models with high einit also develop a very eccentric (e⋆ ≳ 0.9) stellar population. For higher disk masses Mdisk ≳ 3 × 104 M⊙, the disk disruption dynamics is more complex than the standard secular eccentric disk instability with opposite precession directions at different disk radii - a precession direction instability. We present an analytical model describing this behavior. A milliparsec population of N ∼ 10–100 stars forms around the SMBH in all models. For low einit stars migrate inward while for einit ≳ 0.6 stars are captured by the Hills mechanism. Without PN, after 6 Myr the captured stars have a sub-thermal eccentricity distribution. We show that including PN effects prevents this thermalization by suppressing resonant relaxation effects and cannot be ignored. The number of tidally disrupted stars is similar or larger than the number of milliparsec stars. None of the simulated models can simultaneously reproduce the kinematic and stellar population properties of the Milky Way center clockwise disk and the S-cluster.

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15 years of high precision astrometry in the Galactic Center

Cited by 2 publications

References 8 publications

Is It Possible to Measure the Lense–Thirring Orbital Shifts of the Short-period S Star S4716 Orbiting Sgr A*?

Is It Possible to Measure the Lense–Thirring Orbital Shifts of the Short-period S Star S4716 Orbiting Sgr A*?

Evolution of eccentric stellar discs around supermassive black holes: the complex disc disruption dynamics and the milliparsec stars

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