Issue |
A&A
Volume 514, May 2010
|
|
---|---|---|
Article Number | A51 | |
Number of page(s) | 23 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361/200913220 | |
Published online | 18 May 2010 |
The influence of model parameters on the prediction of gravitational wave signals from stellar core collapse
Department of Physics, University of Basel, Klingelbergstrasse
82, 4056 Basel, Switzerland e-mail: simon.scheidegger@unibas.ch
Received:
31
August
2009
Accepted:
18
January
2010
We present a gravitational wave (GW) analysis of an
extensive series of three-dimensional
magnetohydrodynamical core-collapse simulations.
Our 25 models are based on a 15 progenitor
stemming from (i) stellar evolution calculations;
(ii) a spherically symmetric effective general
relativistic potential, either the Lattimer-Swesty (with three possible
compressibilities) or the Shen equation of state for hot, dense
matter; and (iii) a neutrino parametrisation
scheme that is accurate until about 5 ms postbounce.
For three representative models, we also included
long-term neutrino physics by means of a
leakage scheme, which is based on partial implementation
of the isotropic diffusion source approximation (IDSA).
We systematically investigated the effects of the equation of state,
the initial rotation rate, and both the toroidal
and the poloidal magnetic fields
on the GW signature. We stress the importance of including of postbounce neutrino physics, since it quantitatively alters the GW signature.
Slowly rotating models, or those that do not rotate
at all, show GW
emission caused by prompt and proto-neutron star (PNS) convection.
Moreover, the signal stemming from prompt convection
allows for the distinction between
the two different nuclear equations of state
indirectly by different properties of the fluid instabilities.
For simulations with moderate or even fast rotation rates,
we only find the axisymmetric type I wave signature at core bounce.
In line with recent results, we could confirm that
the maximum GW amplitude scales roughly linearly with the
ratio of rotational to gravitational energy at core bounce below
a threshold value of about 10%.
We point out that models set up with an initial
central angular velocity of 2π rad s-1 or faster
show nonaxisymmetric narrow-band GW radiation
during the
postbounce phase. This emission process is
caused by a low T/|W| dynamical instability.
Apart from these two points, we show that it is
generally very difficult to discern
the effects of the individual features of the input physics in
a GW signal from a rotating core-collapse supernova
that can be attributed unambiguously to a specific model.
Weak magnetic fields do not notably influence the dynamical
evolution of the core and thus the GW emission.
However, for strong initial poloidal magnetic fields (≳1012 G),
the combined action of flux-freezing and field winding
leads to conditions where the ratio of magnetic field pressure to
matter pressure reaches about unity
which leads to the onset of a jet-like supernova explosion.
The collimated bipolar out-stream of matter is then reflected
in the emission of a type IV GW signal.
In contradiction to axisymmetric simulations,
we find evidence that nonaxisymmetric fluid
modes can counteract or even suppress jet formation for models with strong
initial toroidal magnetic fields.
The results of models with continued neutrino emission
show that including of the deleptonisation
during the postbounce phase is an indispensable issue for the
quantitative prediction of GWs
from core-collapse supernovae,
because it can alter the GW amplitude up to a factor of 10
compared to a pure hydrodynamical treatment.
Our collapse simulations
indicate that corresponding events in our Galaxy would be detectable either
by LIGO, if the source is rotating, or at least by the advanced LIGO detector,
if it is not or only slowly rotating.
Key words: gravitational waves / supernovae: general / hydrodynamics / neutrinos / stars: rotation / stars: neutron
© ESO, 2010
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