# Item

ITEM ACTIONSEXPORT

Released

Journal Article

#### On the mass radiated by coalescing black-hole binaries

##### Locator

There are no locators available

##### Fulltext (public)

1206.3803

(Preprint), 479KB

APJ_758_1_63.pdf

(Any fulltext), 494KB

##### Supplementary Material (public)

There is no public supplementary material available

##### Citation

Barausse, E., Morozova, V., & Rezzolla, L. (2012). On the mass radiated by coalescing
black-hole binaries.* Astrophysical Journal,* *758*: 63.
doi:10.1088/0004-637X/758/1/63.

Cite as: http://hdl.handle.net/11858/00-001M-0000-000E-EEC9-9

##### Abstract

We derive an analytic phenomenological expression that predicts the final
mass of the black-hole remnant resulting from the merger of a generic binary
system of black holes on quasi-circular orbits. Besides recovering the correct
test-particle limit for extreme mass-ratio binaries, our formula reproduces
well the results of all the numerical-relativity simulations published so far,
both when applied at separations of a few gravitational radii, and when applied
at separations of tens of thousands of gravitational radii. These validations
make our formula a useful tool in a variety of contexts ranging from
gravitational-wave physics to cosmology. As representative examples, we first
illustrate how it can be used to decrease the phase error of the
effective-one-body waveforms during the ringdown phase. Second, we show that,
when combined with the recently computed self-force correction to the binding
energy of nonspinning black-hole binaries, it provides an estimate of the
energy emitted during the merger and ringdown. Finally, we use it to calculate
the energy radiated in gravitational waves by massive black-hole binaries as a
function of redshift, using different models for the seeds of the black-hole
population.