<p>When I first read about this (supernovae causing gravitational waves) that was the same thought I had. But I read up about it and found that no supernovae explosion is perfectly spherically symmetric and so therefore the center of mass/energy will move with the explosion, causing a short burst of gravitational waves as the retarded gravitational potential catches up with the new center of mass.</p>

<p>Below is an example of what these signals would look like if detected by LIGO. They don't produce that increasing frequency signal you mentioned, instead its simply a short sharp change in the strain momentarily (note the timescale along the bottom too, the recent black hole merger event lasted about 0.2s).</p>

<p><a href="https://i.sstatic.net/axrK5.jpg" rel="nofollow noreferrer"><img src="https://i.sstatic.net/axrK5.jpg" alt="enter image description here"></a></p>

CC BY-SA 3.0
2016-03-02T23:42:12.767Z
Where'd you get, or how'd you produce, that image?
zibadawa timmy
CC BY-SA 3.0
2016-03-03T10:33:46.733Z
@zibadawatimmy Here: http://www.ligo.org/science/GW-Burst.php
Dean
CC BY-SA 3.0
2016-03-02T13:54:20.887Z
2016-03-02T13:54:20.887Z
Dean
<p>The key here is that to produce gravitational waves, the supernova explosion must not have perfect spherical symmetry. Technically, what you need is an "accelerating" gravitational quadrupole moment.</p>

<p>It is quite unlikely that supernovae explosions will be symmetric. Asymmetries can be produced by binary companions, magnetic fields, rotation...</p>

<p>The characteristics of a "burst" source of gravitational waves will be quite unlike the signature of coalescing binary black holes. The magnitude of the signal is expected to follow the collapsing core of the star and reach a peak at something called the "core bounce", where the equation of state of the gas "stiffens" and a shock wave propagates outwards. The signal is thus likely to gradually increase in amplitude for some tens of milli-seconds, followed by an abrupt spike at the bounce, followed by a "ring-down" as the core (a proto-neutron star) settles down towards a spherically symmetric configuration over the course of a further 10 milli-seconds or so.</p>

<p>The frequencies of the waves will have a broad range governed by the characteristic frequency implied by $(G\rho)^{1/2}$, which is the inverse of the freefall timescale, where $\rho$ is the density at the time when the GWs are emitted. For a typical core collapse, the densities could range from $10^{14}$ to a few $10^{17}$ kg/m$^3$ over the course of the event, producing GW frequencies of tens to thousands of Hz - exactly in the range at which aLIGO is sensitive.</p>

<p>Because GWs pass through the envelope of the star unimpeded then the GW signature of a supernova probes the very heart of a supernova explosion and should be seen some hours before the visible signature is apparent. On the other hand any neutrino emission from a core collapse supernova should be detected at a very similar time to the GW waves. Any delay here could fix the currently poorly known neutrino mass.</p>

CC BY-SA 3.0
2016-03-02T15:50:22.807Z
Stars spin, on a spin axis. That makes it very hard for them to have perfect spherical symmetry.
Wayfaring Stranger
CC BY-SA 3.0
2016-03-02T16:48:17.777Z
@WayfaringStranger That's what I've said.
ProfRob
CC BY-SA 3.0
2016-03-02T18:13:42.507Z
Rob, sure, I just thought the condensed version would look nice down here.
Wayfaring Stranger
CC BY-SA 3.0
2016-03-02T14:01:08.640Z
2016-03-02T14:01:08.640Z
ProfRob
<p>With the recent results of LIGO, I read a lot how limited the detection capabilities where and how one could only expect to measure the most extreme events like black hole mergers and supernovae.</p>

<p>I get the black hole mergers, since here we see an ever higher frequency gravitational interference of two large bodies. But how can a supernova cause a gravitational wave? All the mass is still there, it is just thrown out  isn't it? So from far away shouldn't the mass still be concentrated on a relatively small place and thus the gravity from the recently exploded star should remain unchanged, right?</p>

<gravity>
How can a supernova cause a gravitational wave?
choeger
# How can a supernova cause a gravitational wave?

(Asked by: username_0 on 2016-03-01)

With the recent results of LIGO, I read a lot how limited the detection capabilities where and how one could only expect to measure the most extreme events like black hole mergers and supernovae.

I get the black hole mergers, since here we see an ever higher frequency gravitational interference of two large bodies. But how can a supernova cause a gravitational wave? All the mass is still there, it is just thrown out isn't it? So from far away shouldn't the mass still be concentrated on a relatively small place and thus the gravity from the recently exploded star should remain unchanged, right?

**Tags:** gravity


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## 2 answers

### Answer by username_3 on 2016-03-02. Score: 10 | Accepted answer

The key here is that to produce gravitational waves, the supernova explosion must not have perfect spherical symmetry. Technically, what you need is an "accelerating" gravitational quadrupole moment.

It is quite unlikely that supernovae explosions will be symmetric. Asymmetries can be produced by binary companions, magnetic fields, rotation...

The characteristics of a "burst" source of gravitational waves will be quite unlike the signature of coalescing binary black holes. The magnitude of the signal is expected to follow the collapsing core of the star and reach a peak at something called the "core bounce", where the equation of state of the gas "stiffens" and a shock wave propagates outwards. The signal is thus likely to gradually increase in amplitude for some tens of milli-seconds, followed by an abrupt spike at the bounce, followed by a "ring-down" as the core (a proto-neutron star) settles down towards a spherically symmetric configuration over the course of a further 10 milli-seconds or so.

The frequencies of the waves will have a broad range governed by the characteristic frequency implied by $(G\rho)^{1/2}$, which is the inverse of the freefall timescale, where $\rho$ is the density at the time when the GWs are emitted. For a typical core collapse, the densities could range from $10^{14}$ to a few $10^{17}$ kg/m$^3$ over the course of the event, producing GW frequencies of tens to thousands of Hz - exactly in the range at which aLIGO is sensitive.

Because GWs pass through the envelope of the star unimpeded then the GW signature of a supernova probes the very heart of a supernova explosion and should be seen some hours before the visible signature is apparent. On the other hand any neutrino emission from a core collapse supernova should be detected at a very similar time to the GW waves. Any delay here could fix the currently poorly known neutrino mass.

> **Comments:**
> **username_4**: Stars spin, on a spin axis. That makes it very hard for them to have perfect spherical symmetry.  
> **username_3**: @username_4 That's what I've said.  
> **username_4**: Rob, sure, I just thought the condensed version would look nice down here.  

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### Answer by username_1 on 2016-03-02. Score: 3

When I first read about this (supernovae causing gravitational waves) that was the same thought I had. But I read up about it and found that no supernovae explosion is perfectly spherically symmetric and so therefore the center of mass/energy will move with the explosion, causing a short burst of gravitational waves as the retarded gravitational potential catches up with the new center of mass.

Below is an example of what these signals would look like if detected by LIGO. They don't produce that increasing frequency signal you mentioned, instead its simply a short sharp change in the strain momentarily (note the timescale along the bottom too, the recent black hole merger event lasted about 0.2s).

[![enter image description here](https://i.sstatic.net/axrK5.jpg)](https://i.sstatic.net/axrK5.jpg)

> **Comments:**
> **username_2**: Where'd you get, or how'd you produce, that image?  
> **username_1**: @username_2 Here: http://www.ligo.org/science/GW-Burst.php  

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