# How to Calculate the Spin of Black Hole Sagittarius A*

This Insight takes a look at how it is possible to calculate the spin of Sagittarius A*, the supermassive black hole at the center of the Milky Way using some data and a few equations derived from Kerr metric. The following paper was used as a source-

Spin and mass of the nearest supermassive black hole by V I Dokuchaev
https://arxiv.org/abs/1306.2033

Extracts from the abstract-
‘Quasi-Periodic Oscillations (QPOs) of the hot plasma spots or clumps orbiting an accreting black hole contain information on the black hole mass and spin.

The promising observational signatures for the measurement of black hole mass and spin are the latitudinal oscillation frequency of the bright spots in the accretion ﬂow and the frequency of black hole event horizon rotation… Interpretation of the known QPO data by dint of a signal modulation from the hot spots in the accreting plasma reveals the Kerr metric rotation parameter, a=0.65 ± 0.05, and mass, M=(4.2 ± 0.2)10⁶ M$_⊙$, of the supermassive black hole in the Galactic center. At the same time, the observed 11.5 min QPO period is identiﬁed with a period of the black hole event horizon rotation, and, respectively, the 19 min period is identiﬁed with a latitudinal oscillation period of hot spots in the accretion ﬂow..’

I was interested that this paper calculated the quantity of spin for the black hole at the center of our galaxy, which is nearly 26,000 light-years from Earth, using a handful of observations and calculations (note, the mass is calculated from the orbits of nearby stars). While the equations themselves are fairly simple, it’s worth first taking a look at Kerr metric (which deals with the curvature of spacetime due to gravity and spin) from which they are derived-

One of the most common expressions for Kerr metric is-

\begin{align*} -c^{2} d\tau^{2} = ds^{2} = & -\left( 1 – \frac{2M r}{\rho^2} \right) c^{2} dt^{2} + \frac{\rho^2}{\Delta} dr^{2} + \rho^2\, d\theta^{2} \\ & + \left( r^{2} + a^{2} + \frac{2M r a^{2}}{ \rho^2} \sin^{2} \theta \right) \sin^{2} \theta \ d\phi^{2} – \frac{4M ra \sin^{2} \theta }{\rho^2} \, c \, dt \, d\phi \end{align*}

where $\rho^2=r^2+a^2 \cos^2 \theta$ and $\Delta=r^2 – 2Mr + a^2$. $\tau$ is proper (or local) time, s is spacetime and t is coordinate (or at infinity) time, M is the gravitational radius (a geometric unit for mass) where M=Gm/c² and a is the spin parameter (a geometric unit of spin) where a=J/mc.

This can also be written in a condensed form (and with c=1) as-

$$-d\tau^2=-\alpha dt^2+\frac{\rho^2}{\Delta}dr^2+\rho^2 d\theta^2+\varpi^2(d\phi-\omega dt)^2$$

where the angular velocity of the frame-dragging rate (ω) which is the rate that spacetime is dragged around the black hole as observed from infinity and the reduction factor (α) are given by-

$$\omega=\frac{2Mra}{\Sigma^2}\ \ \ \ \ \ \ \ \ \ \ \alpha=\sqrt{\Delta}\frac\rho\Sigma$$

Note, multiply ω by c for SI units of rad/s. The reduction factor (or lapse function) can be described as the redshift and time dilation at a specific r taking into account dilation due to gravity and frame-dragging (for instance, the frame-dragging rate as observed from infinity would be ω but the proper frame dragging rate locally would be ω/α). Other geometric functions are given by-

$$\Sigma^2=(r^2+a^2)^2-a^2\Delta \sin^2\theta\ \ \ \ \ \ \ \ \ \ \ \varpi=\frac\Sigma\rho\sin \theta$$

where ϖ is often referred to as the reduced circumference (or the proper coordinate radius that takes into account frame dragging).

The black holes event horizons (outer and inner) are given by-

$$r_{h\pm}=M\pm\sqrt{M^2-a^2}$$

where + defines the outer horizon and − defines the inner.

Angular velocity of the event horizons (as observed from infinity)-

$$\Omega_{h\pm}=\frac{a}{r_{h\pm}+a^2}$$

where again, + defines the outer and − defines the inner horizon. Angular velocity (in its most simple form) required for a stable equatorial orbit at a specific r is given by-

$$\Omega_{\phi\pm}=\frac{\pm\sqrt{M}}{r^{3/2}\pm a\sqrt{M}}$$

Here, + defines a prograde orbit (with the frame-dragging) and − the retrograde orbit (against the frame-dragging). Allowing for resonance (the rate at which an object in orbit bobs up and down in latitude due to the highly curved spacetime), the angular velocity with latitudinal oscillation of a near-circular orbit at a specific r is given by-

$$\Omega_{\theta \pm}=\Omega_{\phi \pm}\sqrt{1\mp4a_*x^{3/2}+3a_*^2x^{-2}}$$

where $a_*=a/M$ and $x=r/M$

This angular velocity describes the latitudinal oscillation of the hot spot or clump of plasma in the thin accretion disk (Note, Ωθ grows slightly less than ΩΦ the closer r is to the black hole, the orbit velocity is probably the same but due to slight movements in latitude, the angular velocity for Ωθ is less than ΩΦ which is a mathematical exact equatorial orbit, see fig. 6 in the paper). It is assumed that the brightest hot spots in the accretion ﬂow are located near the inner edge of the accretion disk, corresponding to the radius of the marginally stable circular orbit given by-

$$r_{ms\pm}\ =\ M\left(3+Z_2 \mp \sqrt{(3-Z_1)(3+Z_1+2Z_2)}\right)$$

where

$$Z_1=1+\left(1-x^2\right)^{1/3}\left(\left(1+x\right)^{1/3}+\left(1-x\right)^{1/3}\right)$$

and

$$Z_2=\sqrt{3x^2+Z_1^2}$$

The marginally stable orbit is at 6M for a static black hole and reduces the greater the spin is, down to M for a hypothetical maximal black hole where a=M, hence the spin parameter can be deduced from where the marginally stable orbit resides.

Based on Quasi-Periodic Oscillations (QPOs) of ~11.5 minutes at the event horizon (Th) and ~19 minutes at the marginally stable orbit (Tθ), the following would apply (considering only the outer event horizon and the prograde orbit respectively)-

$$T_h=\frac{2\pi}{\Omega_h}\approx 11.5 \text{mins}$$

$$T_\theta=\frac{2\pi}{\Omega_\theta}\approx 19 \text{mins}$$

where rms would be used to calculate Ωθ. In both cases, the spin parameter is calculated to be a/M≈0.65 in order to match the orbit periods (T), as per fig. 8 in the paper. (Note, the equation for T is based on circumference/velocity where circ=2πϖ and v=Ωϖ where ϖ replaces what would normally be r).

While there are other signals for QPO’s around the black hole, these are the most significant when calculating the spin, the shortest stable orbit period in x-rays indicating the MSCO (inner edge of the accretion disk), and the shortest period in near-infrared which indicates matter falling into the black hole (note, the matter falling locally would be instantaneous but due to the deep gravity well, the matter would appear to make a few orbits of the event horizon in near-infrared before shifting deeper into radio waves). The results also correspond with the estimate of a≃0 − 0.6, from the millimeter VLBI observations of Sgr A*.

Other useful calculations from Kerr metric-

The proper velocity required for a stable orbit in the equatorial plane (where + defines a prograde orbit and − the retrograde orbit)-

$$v_{s\pm}=\frac{r^2+a^2\mp 2a\sqrt{Mr}}{\sqrt{\Delta} \left[a\pm r\sqrt{r/M}\right]}$$

which is equivalent to-

$$v_{s\pm}=(\Omega_{\phi \pm}-\omega)\frac{\varpi}{\alpha}$$

Ergoregion boundaries (where + defines the outer and − defines the inner boundary, the inner residing within the inner horizon)-

$$r_{e\pm}=M\pm\sqrt{M^2-a^2\cos^2\theta}$$

Photon sphere (or more accurately, the photon circle in the equatorial plane, where + defines the prograde and − defines the retrograde orbit), 3M for a static black hole-

$$r_{ph\pm}=2M\left[1+\cos\left(\frac{2}{3}\cos^{-1}\mp \frac{|a|}{M}\right)\right]$$

Marginally bound circular orbit (where orbits are unstable), 4M for a static black hole-

$$r_{mb\pm}=\left(\sqrt{M}+\sqrt{M\mp a}\right)^2=2M\mp a+2\sqrt{M(M\mp a)}$$

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3 replies
1. Buzz Bloom says:

I am interested in the topic, but unfortunately I could not read the equations. Is there someway for me to get the equations' text translated into something readable?

I see that the equations became readable when I clicked on the tutorial icon in this thread.

It was unreadable in the Insight text.

2. mfb says:

I'm curious if the Event Horizon Telescope will have sufficient time resolution to contribute to this directly – or do they have to take a long-term average to see anything? A resolved observation of the accretion disk and its surroundings should help to check these models.

3. PF_Help_Bot says:

Thanks for the thread! This is an automated courtesy bump. Sorry you aren't generating responses at the moment. Do you have any further information, come to any new conclusions or is it possible to reword the post? The more details the better.