Gravitational Waves from a Core g-Mode in Supernovae as Probes of the High-Density Equation of State

Jakobus, Pia; Müller, Bernhard; Heger, Alexander; Zha, Shuai; Powell, J.; Motornenko, Anton; Steinheimer, Jan; Stoecker, Horst

doi:10.48550/arxiv.2301.06515

Cited by 3 publications

(5 citation statements)

References 53 publications

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“…There is also evidence for some GW power in the "bumped" g-mode (that thereafter trends to lower frequencies), seen just after the mode repulsion in Figures 5 and 6, but most clearly in Figure 17 below. This is a qualitatively similar feature to that highlighted recently in [89]. Nevertheless, within ∼0.3 to ∼1.0 seconds (depending upon the progenitor) most power is clearly in the f-mode, where it persists thereafter.…”

Section: Avoided Crossing and Trapped G-modesupporting

confidence: 88%

“…Though we have endeavored here to provide a comprehensive look at the gravitational-wave signatures of core collapse, there remains much yet to understand. Topics unaddressed here are the nuclear equation-of-state dependencies, the role of rapid rotation, the possible signatures of strong magnetic fields [36,89](REF), and the results for other progenitor massive stars and from other stellar evolution codes. Importantly, the analysis of a detected GW signal would be significantly aided if done in concert with a corresponding analysis of the simultaneous neutrino signal.…”

Section: Discussionmentioning

confidence: 99%

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The Gravitational-Wave Signature of Core-Collapse Supernovae

Vartanyan¹,

Burrows²,

Coleman³

et al. 2023

Preprint

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We calculate the gravitational-wave (GW) signatures of detailed 3D core-collapse supernova simulations spanning a range of massive stars. Most of the simulations are carried out to times late enough to capture more than 95% of the total GW emission. We find that the f/g-mode and f-mode of proto-neutron star oscillations carry away most of the GW power. The f-mode frequency inexorably rises as the proto-neutron star (PNS) core shrinks. We demonstrate that the GW emission is excited mostly by accretion plumes onto the PNS that energize modal oscillations and also highfrequency ("haze") emission correlated with the phase of violent accretion. The duration of the major phase of emission varies with exploding progenitor and there is a strong correlation between the total GW energy radiated and the compactness of the progenitor. Moreover, the total GW emissions vary by as much as three orders of magnitude from star to star. For black-hole formation, the GW signal tapers off slowly and does not manifest the haze seen for the exploding models. For such failed models, we also witness the emergence of a spiral shock motion that modulates the GW emission at a frequency near ∼100 Hertz that slowly increases as the stalled shock sinks. We find significant angular anisotropy of both the high-and low-frequency (memory) GW emissions, though the latter have very little power.

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Section: Avoided Crossing and Trapped G-modesupporting

confidence: 88%

Section: Discussionmentioning

confidence: 99%

The Gravitational-Wave Signature of Core-Collapse Supernovae

Vartanyan¹,

Burrows²,

Coleman³

et al. 2023

Preprint

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“…One of the useful features in the proposed method is that we can apply it even in cases with no detection of GWs. This is a great advantage compared to other proposed GW-neutrino analysis, for instance GW spectrogram analysis [5][6][7][8][9][10][11][12][13][14][15][16][17], that commonly requires GW data with high S/N.…”

Section: Discussionmentioning

confidence: 99%

“…There are many previous theoretical studies to understand characteristic features of GWs and neutrino signals (see reviews, e.g., [1] for GWs and [2][3][4] for neutrinos and references therein). GW spectrogram analysis based on multi-dimensional (multi-D) simulations is one of major approaches to probe the interior physics of CCSNe [5][6][7][8][9]. This analysis can also be complemented by linear analysis (or asteroseismology) of the proto-neutron star (PNS) [10][11][12][13][14][15][16][17] or neutrino signal [18][19][20].…”

Section: Introductionmentioning

confidence: 99%

Supernova neutrino signals based on long-term axisymmetric simulations

Nagakura

Burrows

Vartanyan

2021

Monthly Notices of the Royal Astronomical Society

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We study theoretical neutrino signals from core-collapse supernova (CCSN) computed using axisymmetric CCSN simulations that cover the post-bounce phase up to ∼4 s. We provide basic quantities of the neutrino signals such as event rates, energy spectra, and cumulative number of events at some terrestrial neutrino detectors, and then discuss some new features in the late phase that emerge in our models. Contrary to popular belief, neutrino emissions in the late phase are not always steady, but rather have temporal fluctuations, the vigor of which hinges on the CCSN model and neutrino flavor. We find that such temporal variations are not primarily driven by proto-neutron star (PNS) convection, but by fallback accretion in exploding models. We assess the detectability of these temporal variations, and find that IceCube is the most promising detector with which to resolve them. We also update fitting formulae first proposed in our previous paper for which the total neutrino energy (TONE) emitted at the CCSN source is estimated from the cumulative number of events in each detector. This will be a powerful technique with which to analyse real observations, particularly for low-statistics data.

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“…Many studies have sought to understand the hydrodynamic source of GWs and detection prospects of these signals using two-and three-dimensional models of core collapse (Marek et al 2009;Murphy et al 2009;Müller et al 2013;Yakunin et al 2015;Kuroda et al 2016;Nakamura et al 2016;Andresen et al 2017;Powell & Müller 2019;Radice et al 2019;Mezzacappa et al 2020;Vartanyan & Burrows 2020;Andresen et al 2021;Takiwaki et al 2021;Bugli et al 2023;Mezzacappa et al 2023;Vartanyan et al 2023). In pursuit of core-collapse GW phenomenology, some recent work has found that the frequency structure of GWs produced by the collapse of astrophysically rare progenitors may depend on the equation of state (EOS); for example, Richers et al (2017) with rotating models of core collapse, and Jakobus et al (2023) with two high-mass (35 M e and 85 M e ), zero-metallicity progenitors. However, due to the extreme computational cost of multidimensional models, it is not yet possible to fully explore the observational consequences of core-collapse GWs across a landscape of stellar progenitor properties, nuclear EOS configurations, and other relevant (astro)physics.…”

Section: Introductionmentioning

confidence: 99%

Gravitational Wave Eigenfrequencies from Neutrino-driven Core-collapse Supernovae

Wolfe,

Fröhlich,

Miller

et al. 2023

ApJ

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Core-collapse supernovae (CCSNe) are predicted to produce gravitational waves (GWs) that may be detectable by Advanced LIGO/Virgo. These GW signals carry information from the heart of these cataclysmic events, where matter reaches nuclear densities. Recent studies have shown that it may be possible to infer the properties of the proto-neutron star (PNS) via GWs generated by hydrodynamic perturbations of the PNS. However, we lack a comprehensive understanding of how these relationships may change with the properties of CCSNe. In this work, we build a self-consistent suite of over 1000 exploding CCSNe from a grid of progenitor masses and metallicities combined with six different nuclear equations of state (EOS). Performing a linear perturbation analysis on each model, we compute the resonant GW frequencies of the PNS, and we motivate a time-agnostic method for identifying characteristic frequencies of the dominant GW emission. From this, we identify two characteristic frequencies, of the early- and late-time signal, that measure the surface gravity of the cold remnant neutron star, and simultaneously constrain the hot nuclear EOS. However, we find that the details of the CCSN model, such as the treatment of gravity or the neutrino transport, and whether it explodes, noticeably change the magnitude and evolution of the PNS eigenfrequencies.

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Gravitational Waves from a Core g-Mode in Supernovae as Probes of the High-Density Equation of State

Cited by 3 publications

References 53 publications

The Gravitational-Wave Signature of Core-Collapse Supernovae

The Gravitational-Wave Signature of Core-Collapse Supernovae

Supernova neutrino signals based on long-term axisymmetric simulations

Gravitational Wave Eigenfrequencies from Neutrino-driven Core-collapse Supernovae

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