<p>In short, not by much.</p>

<p>Out by us the Earth the gravitational acceleration towards the centre of the galaxy is $v^2/r = \frac{(2\times2\times 10^{20}\times \pi\  \mathrm{metres} / 230000000\  \mathrm{years})^2 }{ 2\times 10^{20} \mathrm{metres}}$, which is of the order of $10^{-10} ms^{-2}$ : in other words, it is very small. This is because spacetime is not highly curved except close to massive bodies.</p>

<p>This spacetime is approximately flat. It can be well approximated by Minkowski space. If you need to include in your model the distribution of mass in the galaxy, then Newtonian mechanics is sufficient, for example <a href="https://physics.stackexchange.com/questions/62637/the-potential-and-the-intensity-of-the-gravitational-field-in-the-axis-of-a-circ">https://physics.stackexchange.com/questions/62637/the-potential-and-the-intensity-of-the-gravitational-field-in-the-axis-of-a-circ</a></p>

<p>In the centre of the galaxy is a black hole, and it is in the neighbourhood of the black hole that GR really comes into play. Near the black hole, the Kerr solution of GR is a good model (the Kerr solution describes a symmetric uncharged spinning mass)</p>

<p>Now on the massive scale, a galaxy, or a cluster of galaxies can have a significant effect on light, given enough time, and enough distance. Light, travelling for many millions of years, past a galaxy, can have its path significantly bent by gravity. (The Schwartzchild solution is a first approximation to the shape of spacetime around a galaxy, though for a better approximation, numerical relativity can be used) This causes gravitational lensing. For light traveling inside a galaxy this is not a significant factor, There isn't time in a few years for light to be bent significantly by the general gravitational field of the galaxy. However light from a star passes close to another star, then there can be measurable bending. </p>

<p>The measurement of the bending of light of stars behind the sun during a solar eclipse was one of the first experimental confirmations of General Relativity (1919) <a href="https://www.wired.com/2009/05/dayintech_0529/" rel="nofollow noreferrer">https://www.wired.com/2009/05/dayintech_0529/</a> Note that even light that passes right over the Sun's surface would only be deflected by less that 2 arcseconds.</p>

CC BY-SA 3.0
2016-12-17T20:59:32.457Z
I would avoid using terms such as "approximately flat", because clearly gravity is significant just about any description of the galaxy, which means the curvature cannot be ignored. There is a sense in which the curvature is small, but justifying what it means for the curvature to be small over a region of spacetime can be quite involved, even if it seems intuitively obvious (Wald goes into detail about this).
John Davis
CC BY-SA 3.0
2016-12-17T08:25:26.640Z
2016-12-17T14:12:35.133Z
2017-04-13T12:40:15.377Z
James K
<p>Space is curved by mass (or more precisely by mass and momentum as described by the stress-energy tensor). The milky way system has a lot of mass and a lot of energy. In what ways is space-time curved within it?</p>

<p><a href="https://www.youtube.com/watch?v=-m3SddsTSAY" rel="nofollow noreferrer"><img src="https://i.sstatic.net/X441R.png"></a></p>

<astrophysics><space-time><general-relativity><dark-matter>
In what ways does the mass and energy of the milky way curve space time?
memex
# In what ways does the mass and energy of the milky way curve space time?

(Asked by: username_0 on 2016-12-14)

Space is curved by mass (or more precisely by mass and momentum as described by the stress-energy tensor). The milky way system has a lot of mass and a lot of energy. In what ways is space-time curved within it?

[![](https://i.sstatic.net/X441R.png)](https://www.youtube.com/watch?v=-m3SddsTSAY)

**Tags:** astrophysics, space-time, general-relativity, dark-matter


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## 1 answers

### Answer by username_1 on 2016-12-17. Score: 4

In short, not by much.

Out by us the Earth the gravitational acceleration towards the centre of the galaxy is $v^2/r = \frac{(2\times2\times 10^{20}\times \pi\ \mathrm{metres} / 230000000\ \mathrm{years})^2 }{ 2\times 10^{20} \mathrm{metres}}$, which is of the order of $10^{-10} ms^{-2}$ : in other words, it is very small. This is because spacetime is not highly curved except close to massive bodies.

This spacetime is approximately flat. It can be well approximated by Minkowski space. If you need to include in your model the distribution of mass in the galaxy, then Newtonian mechanics is sufficient, for example <https://physics.stackexchange.com/questions/62637/the-potential-and-the-intensity-of-the-gravitational-field-in-the-axis-of-a-circ>

In the centre of the galaxy is a black hole, and it is in the neighbourhood of the black hole that GR really comes into play. Near the black hole, the Kerr solution of GR is a good model (the Kerr solution describes a symmetric uncharged spinning mass)

Now on the massive scale, a galaxy, or a cluster of galaxies can have a significant effect on light, given enough time, and enough distance. Light, travelling for many millions of years, past a galaxy, can have its path significantly bent by gravity. (The Schwartzchild solution is a first approximation to the shape of spacetime around a galaxy, though for a better approximation, numerical relativity can be used) This causes gravitational lensing. For light traveling inside a galaxy this is not a significant factor, There isn't time in a few years for light to be bent significantly by the general gravitational field of the galaxy. However light from a star passes close to another star, then there can be measurable bending.

The measurement of the bending of light of stars behind the sun during a solar eclipse was one of the first experimental confirmations of General Relativity (1919) <https://www.wired.com/2009/05/dayintech_0529/> Note that even light that passes right over the Sun's surface would only be deflected by less that 2 arcseconds.

> **Comments:**
> **username_2**: I would avoid using terms such as "approximately flat", because clearly gravity is significant just about any description of the galaxy, which means the curvature cannot be ignored. There is a sense in which the curvature is small, but justifying what it means for the curvature to be small over a region of spacetime can be quite involved, even if it seems intuitively obvious (Wald goes into detail about this).  

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