A model for gravitational wave emission from neutrino-driven core-collapse supernovae
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...Moreover, large-amplitude SASI motions were found to stir strong g-mode activity in the neutron star surface, which leads to gravitational-wave emission (Marek et al. 2009; Murphy et al. 2009)....
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...As a consequence, we had to replace an exponential factore−τeff , which was introduced in an ad hoc way by Murphy et al. (2009) and Nordhaus et al. (2010) to damp the neutrino source terms at high optical depthsτeff , by e−τeff/2.7 in order to reproduce the minimum luminosity found to yield…...
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...(4) and (5) is included in Nordhaus et al. (2010), but not in Murphy & Burrows (2008) and Murphy et al. (2009)....
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...…to ensure close similarity of our results to the 1D models studied by Nordhaus et al. (2010) and Murphy & Burrows (2008), we have to enhance the net cooling of the accreted matter by reducing the eff ctive opacityκeff by a factor of 2.7 compared to the value given in Murphy et al. (2009) and in Eq....
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...(6) The effective opacityκeff was derived by Janka (2001) and given in Murphy et al. (2009): κeff ≈ 1.5 · 10−7 · Xn,p ( ρ 1010 g cm−3 ) ( Tνe 4 MeV )2 cm−1, (7) whereXn,p = 12 ( Yn + Yp ) accounts for composition averaging....
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...In this phase, the GW emission transitions to higher frequencies, indicating that emission from deceleration of downflows at the steep density gradient at the edge of the protoneutron star (as first pointed out by Murphy et al. 2009) and convection in the protoneutron star play an increasing role....
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...A more detailed investigation of these features must be left to future work, since it would require multiple quadrupole integrals to isolate emission regions as done, e.g., by Murphy et al. (2009)....
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...…provide important insight into the role and relevance of multi-dimensional fluid instabilities, rotation, the structure of the protoneutron star, and the nuclear EOS (Dimmelmeier et al. 2008; Marek et al. 2009; Yakunin et al. 2010; Murphy et al. 2009; Röver et al. 2009; Ott 2009; Kotake 2011)....
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...Our typical |h| are also quantitatively consistent with the findings of the simpler 3D simulations of Scheidegger et al. (2010) and Kotake et al. (2009, 2011), but are a factor of a few smaller than predictions from 2D simulations (e.g., Marek et al. 2009; Yakunin et al. 2010; Murphy et al. 2009)....
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...…prompt convection with frequencies around ∼100 − 200Hz, a subsequent almost quiescent phase, followed by higher-frequency (400 − 1000Hz) emission, whose amplitudes are dominated by the deceleration of undershooting convective plumes at the edge of the protoneutron star (cf. Murphy et al. 2009)....
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References
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"A model for gravitational wave emis..." refers background in this paper
...Although core structure follows a general trend with the progenitor’s ZAMS mass, the correlation is known to be somewhat chaotic (Woosley et al. 2002)....
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942 citations
"A model for gravitational wave emis..." refers background in this paper
...However, the rotation rates necessary for GWs with sizeable amplitudes are likely to obtain in only ∼1% of the massive star population (Heger et al. 2005; Hirschi et al. 2004; Woosley & Heger 2006; Ott et al. 2006b)....
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844 citations
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"A model for gravitational wave emis..." refers background in this paper
...(5) Note that these approximations for heating and cooling by neutrinos (Bethe & Wilson 1985; Janka 2001) depend upon local quantities and predefined parameters....
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...More than two decades ago, Wilson (1985) and Bethe & Wilson (1985) suggested that a fraction of the neutrinos being emitt d from depth (.100 km) would be recaptured in the gain region (&100 km), reviving the stalled shock into explosion....
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839 citations