Neutrino Emission as Diagnostics of Core-Collapse Supernovae

Müller, Bernhard

doi:10.1146/annurev-nucl-101918-023434

Cited by 74 publications

(42 citation statements)

References 178 publications

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“…The important problem of neutrino transport is treated in considerable depth by Mezzacappa (2005Mezzacappa ( , 2020 and is therefore not addressed in this review. A number of reviews address the potential of neutrinos (e.g., Kotake et al 2006;Müller 2019b) and gravitational waves (Ott 2009;Kotake 2013;Kalogera et al 2019) as diagnostics of the multi-dimensional dynamics in the supernova core.…”

Section: Scope and Structure Of This Reviewmentioning

confidence: 99%

“…Structure of the accretion flow At this stage, the PNS consists of an inner core of about 0:5 M (depending on the equation of state) with low entropy, which is surrounded by an extended mantle of about 1 M that was heated to entropies of about 6k b =nucleon as the shock propagated through the outer part of the collapsed iron core and most of the Si shell. The mantle extends out to the neutrinosphere at high subnuclear densities, where neutrinos on average undergo their last interaction before escape (for details see Kotake et al 2006;Janka 2017;Müller 2019b;Mezzacappa 2020). In the atmosphere immediately outside the neutrinosphere radius R m , the pressure P is dominated by non-relativistic baryons, and neutrino interactions are still frequent enough to act as ''thermostat'' and maintain a roughly isothermal stratification, resulting in an exponential density profile (Janka 2001):…”

Section: Structure Of the Accretion Flow And Runaway Conditions In Spmentioning

confidence: 99%

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Hydrodynamics of core-collapse supernovae and their progenitors

Müller¹

2020

Living Rev Comput Astrophys

161

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Multi-dimensional fluid flow plays a paramount role in the explosions of massive stars as core-collapse supernovae. In recent years, three-dimensional (3D) simulations of these phenomena have matured significantly. Considerable progress has been made towards identifying the ingredients for shock revival by the neutrino-driven mechanism, and successful explosions have already been obtained in a number of selfconsistent 3D models. These advances also bring new challenges, however. Prompted by a need for increased physical realism and meaningful model validation, supernova theory is now moving towards a more integrated view that connects multi-dimensional phenomena in the late convective burning stages prior to collapse, the explosion engine, and mixing instabilities in the supernova envelope. Here we review our current understanding of multi-D fluid flow in core-collapse supernovae and their progenitors. We start by outlining specific challenges faced by hydrodynamic simulations of core-collapse supernovae and of the late convective burning stages. We then discuss recent advances and open questions in theory and simulations.

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Section: Scope and Structure Of This Reviewmentioning

confidence: 99%

Section: Structure Of the Accretion Flow And Runaway Conditions In Spmentioning

confidence: 99%

Hydrodynamics of core-collapse supernovae and their progenitors

Müller¹

2020

Living Rev Comput Astrophys

161

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“…Furthermore, multidimensional models allow for departures from spherical symmetry, providing a more physically motivated scenario. We refer the reader to Müller (2019) for a discussion of potential ways to observationally decipher this explosion mechanism and to Müller (2020) for a review of the state-of-the-art simulations in this field.…”

Section: Assessment Of the Yieldsmentioning

confidence: 99%

The stochastic enrichment of Population II stars

Welsh

Cooke

Fumagalli

2020

Monthly Notices of the Royal Astronomical Society

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We investigate the intrinsic scatter in the chemical abundances of a sample of metal-poor ([Fe/H] <−2.5) Milky Way halo stars. We draw our sample from four historic surveys and focus our attention on the stellar Mg, Ca, Ni, and Fe abundances. Using these elements, we investigate the chemical enrichment of these metal-poor stars using a model of stochastic chemical enrichment. Assuming that these stars have been enriched by the first generation of massive metal-free stars, we consider the mass distribution of the enriching population alongside the stellar mixing and explosion energy of their supernovae. For our choice of stellar yields, our model suggests that the most metal-poor stars were enriched, on average, by $\hat{N}_{\star }=5^{+13}_{-3}~(1\sigma )$ Population III stars. This is comparable to the number of enriching stars inferred for the most metal-poor DLAs. Our analysis therefore suggests that some of the lowest mass structures at z ∼ 3 contain the chemical products from <13 (2σ) Population III enriched minihaloes. The inferred IMF is consistent with that of a Salpeter distribution and there is a preference towards ejecta from minimally mixed hypernovae. However, the estimated enrichment model is sensitive to small changes in the stellar sample. An offset of ∼0.1 dex in the [Mg/Ca] abundance is shown to be sensitive to the inferred number of enriching stars. We suggest that this method has the potential to constrain the multiplicity of the first generation of stars, but this will require: (1) a stellar sample whose systematic errors are well understood; and, (2) documented uncertainties associated with nucleosynthetic yields.

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“…Information of supernova mechanism from supernova neutrino detectors. The accumulation of predicted signals of supernova neutrinos will enable us to extract the information of supernovae from the detection of neutrino bursts in the future [349,350]. SK will detect ∼10,000 neutrino events from a supernovae in our Galaxy and provide valuable and unprecedentedly detailed information regarding the supernova mechanism.…”

Section: Light Curve Of Supernova Neutrinosmentioning

confidence: 99%

Gravitational wave physics and astronomy in the nascent era

Arimoto

Asada

Cherry

et al. 2021

Progress of Theoretical and Experimental Physics

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The detections of gravitational waves (GW) by LIGO/Virgo collaborations provide various possibilities to physics and astronomy. We are quite sure that GW observations will develop a lot both in precision and in number owing to the continuous works for the improvement of detectors, including the expectation to the newly joined detector, KAGRA, and the planned detector, LIGO-India. In this occasion, we review the fundamental outcomes and prospects of gravitational wave physics and astronomy. We survey the development focusing on representative sources of gravitational waves: binary black holes, binary neutron stars, and supernovae. We also summarize the role of gravitational wave observations as a probe of new physics.

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Neutrino Emission as Diagnostics of Core-Collapse Supernovae

Cited by 74 publications

References 178 publications

Hydrodynamics of core-collapse supernovae and their progenitors

Hydrodynamics of core-collapse supernovae and their progenitors

The stochastic enrichment of Population II stars

Gravitational wave physics and astronomy in the nascent era

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