Nevin N. Weinberg, Phil Arras, Joshua Burkart
A weakly nonlinear fluid wave propagating within a star can be unstable to three-wave interactions. The resonant parametric instability is a well-known form of three-wave interaction in which a primary wave of frequency \omega_a excites a pair of secondary waves of frequency \omega_b+\omega_c\simeq \omega_a. Here we consider a nonresonant form of three-wave interaction in which a low-frequency primary wave excites a high-frequency p-mode and a low-frequency g-mode such that \omega_b+\omega_c >> \omega_a. We show that a p-mode can couple so strongly to a g-mode of similar radial wavelength that this type of nonresonant interaction is unstable even if the primary wave amplitude is small. As an application, we analyze the stability of the tide in coalescing neutron star (NS) binaries to p-g mode coupling. We find that the equilibrium tide and dynamical tide are both p-g unstable at gravitational wave frequencies f_gw > 20 Hz and drive short wavelength p-g mode pairs to significant energies on very short timescales (much less than the orbital decay time due to gravitational radiation). Resonant parametric coupling to the tide is, by contrast, either stable or drives modes at a much smaller rate. We do not solve for the saturation of the p-g instability and therefore cannot say precisely how it influences NS binaries. However, we show that if even a single daughter mode saturates near its wave breaking amplitude, the p-g instability of the equilibrium tide: (i) induces significant orbital phase errors (\Delta\phi > 1 radian) that accumulate primarily at low frequencies (f_gw < 50 Hz) and (ii) heats the core to T~10^{10} K. Since there are >100 unstable daughters, \Delta\phi and T are potentially much larger than these values. Tides might therefore significantly influence the gravitational wave signal and electromagnetic emission at much larger orbital separations than previously thought.
View original:
http://arxiv.org/abs/1302.2292
No comments:
Post a Comment