MICRA2019 - Microphysics In Computational Relativistic Astrophysics

12 Aug 2019, 08:00 → 16 Aug 2019, 12:30 Europe/Berlin

Abbeanum-Ground floor-HS1 - Hörsaal 1 (Jena FSU)

 

Welcome to MICRA2019!

MICRA, which stands for Microphysics In Computational Relativistic Astrophysics, is a biennial workshop focused on improving, discussing, and addressing the microphysics needs of relativistic simulations of astrophysical systems, core-collapse supernovae, compact object mergers, and gamma-ray bursts by bringing together nuclear and neutrino theorists and astrophysicists and computational modelers. This year marks the 6th installment and the 10th anniversary of MICRA, and the first since the revolutionary gravitational wave event GW170817.

MICRA generally rotates back and forth between North America and Europe. This year MICRA2019 will be held at the TPI in Jena, Germany from August 12-16, 2019.  We are looking forward to an exciting workshop. The layout of MICRA2019 will be similar to previous MICRAs. We will have a few invited review talks and contributed talks of the major themes of the workshop with days generally focused on different microphysics and their impact on astrophysical systems. There will be ample time for discussion and break-out sessions in the afternoon. The days will focus on:

• The Nuclear Equation of State.  The nuclear equation of state is a staple of simulations of relativistic astrophysics.  The relationship between the density, temperature, and composition of the matter to the pressure sets the structure of neutron stars, protoneutron star, supermassive neutron stars, and hypermassive neutron stars.
• Neutrinos. Due the extreme densities and temperatures, the thermodynamics and dynamics of relativistic astrophysical systems are often driven by neutrino interactions, mainly emission, but also absorption.
• Nucleosynthesis. Massive stars, core-collapse supernovae and compact object mergers are the sites where many of the elements in nature are formed.  The sensitivity to the reaction rates, neutrino interactions, and the implications of GW170817 have brought nucleosynthesis in relativistic systems to the forefront of computational astrophysics.

At MICRA we are interested in both the theory of this microphysics and the practical details on implementation in computational simulations. We hope you will join us in the discussion! See you in Jena.

Invited Speakers

• CURTIS Sanjana (NC State U)
• KNELLER James (NC State U)
• LIEBENDOERFER Matthias (U of Basel)
• PEREGO Albino (U of Trento)
• RICHERS Sherwood (NC State U)
• ROSSWOG Stephan (Stockholm U)
• SCHNEIDER Andre (Stockholm U)
• TOLOS Laura (Goethe U)
• VARTANYAN David (Princeton U)
• VASSH Nicole (U of Notre Dame)

Scientific Organizing Committee

• BERNUZZI Sebastiano (Jena U)
• COUCH Sean M. (Michigan State U)
• FROHLICH Carla (NC State U)
• MOESTA Philipp (UC Berkley)
• O'CONNOR Evan (Stockholm U)

Local Organizing Committee

• ORTIZ Nestor (Jena U)
• ENDRIZZI Andrea (Jena U)
• NEDORA Vsevolod (Jena U)

MICRA2019_Jena.jpg

Monday 12 August

Logistics

08:00 Registration

1 Welcome & Intro

Neutrinos: Neutrinos I

All things Neutrinos, Neutrino Oscillations, transport, and interactions

2 Neutrinos in/from supernovae

The behavior of neutrinos in core-collapse supernovae is very different from their usual role as ephemeral larcenists. Neutrinos are the principle mechanism by which energy and lepton number are transported within the explosion, while core-collapse supernovae produce neutrinos in such prodigious quantities that the neutrino signal from a supernova in The Galaxy would allow us to directly observe the conditions at the center of the explosion and thus test our theories of how massive stars end their lives. In this talk I will present the current status of our understanding of neutrinos in supernovae emphasizing what has been recently learned, where the gaps in our understanding still exist, and what information we can hope to glean from a neutrino burst signal. In addition, I will discuss how new properties of neutrinos, such as interactions beyond the Standard Model or additional flavors of neutrinos, can be probed and tested in regimes of temperature and density not accessible here on Earth.

Speaker: Jim Kneller (NC State University)

MICRA 2019.pdf

09:30 Discussion

09:45 Morning Coffee

Neutrinos: Neutrinos II

All things Neutrinos, Neutrino Oscillations, transport, and interactions

3 Neutrino Quantum Kinetics in Compact Objects

Neutrinos play a critical role of transporting energy and changing the lepton density within core-collapse supernovae (CCSNe) and neutron star mergers. The possibility of flavor or angular instabilities in the neutrino distributions have the potential to revolutionize our understanding of the CCSN explosion mechanism and neutrino signals. However, understanding these effects will require yet-undeveloped technology to simulate the neutrino quantum kinetic equations (QKEs). I will present a method for extending existing neutrino interaction rates long used in CCSN/merger simulations to full QKE source terms for use in numerical calculations. To demonstrate the effects of a complete set of neutrino interaction physics, I will show the results of simulations of the full isotropic QKEs in conditions relevant to CCSNe and neutron star mergers. I will demonstrate that in isotropic calculations, electron scattering, nucleon-nucleon bremsstrahlung processes, and four-neutrino processes dominate flavor decoherence in the protoneutron star (PNS), absorption dominates near the shock, and all of the considered processes except elastic nucleon scattering are relevant in the decoupling region. Finally, I will present an effective decoherence opacity that at most energies predicts decoherence rates to within a factor of 10 in our model PNS and within 20% outside of the PNS.

Speaker: Sherwood Richers (University of California, Berkeley)

10:45 Discussion

4 General Relativistic Multidimensional Flux-Limited Diffusion Scheme for Neutrino Transport

We present the new code NADA-FLD to solve multi-dimensional neutrino-hydrodynamics in full general relativity (GR) in spherical polar coordinates. The neutrino transport assumes the flux-limited diffusion (FLD) approximation and evolves the neutrino energy densities measured in the frame comoving with the fluid. Operator splitting is used to avoid multi-dimensional coupling of grid cells in implicit integration steps involving matrix inversions. Terms describing lateral diffusion and advection are integrated explicitly with the Allen-Cheng or the Runge-Kutta-Legendre method, which remain stable even in the optically thin regime. We discuss several toy-model problems in one and two dimensions to test the basic functionality and individual components of the transport scheme. We also perform fully dynamic core-collapse supernova (CCSN) simulations in spherical symmetry. For a Newtonian model we find good agreement with the M1 code ALCAR, and for a GR model we reproduce the main effects of GR in CCSNe already found by previous works.

Speaker: Mr Ninoy Rahman (Max Planck for Astrophysics)

Ninoy_Rahman_MICRA_2019.pdf

11:20 Discussion

5 The Effects of Neutrino Oscillations on Core-Collapse Supernova Explosions

At the present time even the most sophisticated, multi-dimensional simulations of core-collapse supernovae do not (self-consistently) include neutrino flavor transformation. This physics is missing despite the importance of neutrinos in the core-collapse explosion paradigm. Because of this dependence, any flavor transformation that occurs in the region between the proto-neutron star and the shock could result in major effects upon the dynamics of the explosion.

We present the first hydrodynamic core-collapse supernova simulation which simultaneously includes flavor transformation of the free-streaming neutrinos in the neutrino transport. These oscillation calculations are dynamically updated and evolve self-consistently alongside the hydrodynamics. Using a $M=15\;{\rm M_{\odot}}$ progenitor, we find that while the oscillations can have an effect on the hydrodynamics, flavor transformation alone does not lead to a successful explosion of this progenitor.

Speaker: Charles Stapleford (North Carolina State University)

11:50 Discussion

12:00 Lunch

Neutrinos: Neutrinos III

All things Neutrinos, Neutrino Oscillations, transport, and interactions

6 Nucleon-nucleon bremsstrahlung in core-collapse supernova simultations

Neutrinos are the main vector of energy transport in the revival process of a stalled supernova shock. The treatment of their interactions with the medium is therefore an important part of our simulations. One of those interactions is the nucleon-nucleon bremsstrahlung which will create or annihilate a neutrino/anti-neutrino pair. In this talk, I will present the results for a finer treatment of this process in the GR1D supernova evolution code. I will talk about simulations from two different progenitors, one of which producing a successful explosion. Those simulations showed that the way of treating nucleon-nucleon bremsstrahlung and electron-positron pair production can have a significant impact on the shock evolution as well as on the neutrino luminosities.

Speaker: Aurore Betranhandy (Stockholm University)

14:20 Discussion

Neutrinos: Discussion Prep for the Week

All things Neutrinos, Neutrino Oscillations, transport, and interactions

15:00 Afternoon Coffee

Neutrinos: Neutrino Discussion/Breakout

All things Neutrinos, Neutrino Oscillations, transport, and interactions

Tuesday 13 August

Core-Collapse Supernovae: Core-Collapse Supernova I

Modeling, observations, and theory of Core-collapse

7 Simulations of Core-Collapse Supernovae

Simulations of Core-Collapse Supernovae rely on four important ingredients: An efficient and reasonably accurate implementation of equation of state and reaction rates, a spatially and temporally well-resolved evolution of shock-roof magneto-hydrodynamics, a multidimensional parallel implementation of neutrino transport approximations with a well-defined pinch of relativistic effects and conservation laws, and an ever-growing toolbox for the analysis of output data. I will discuss the performance of the Isotropic Diffusion Source Approximation (IDSA) in 3D supernova models and compare the results of our code "Elephant" with other 3D supernova codes. Remarks on the future and availability of Elephant are also given.

Speaker: Matthias Liebendoerfer (University of Basel)

09:30 Discussion

09:45 Morning Coffee

Core-Collapse Supernovae: Core-Collapse Supernova II

Modeling, observations, and theory of Core-collapse

8 Towards 3D Simulations of Theoretical CCSNe Populations

Using Fornax, we have provided a broad suite of almost a dozen high-fidelity 3D simulations of core-collapse supernovae, spanning 9 $-$ 60 M$_{\odot}$ in progenitor mass. Such a plethora of simulations, many through one second postbounce, allows us to probe the detailed dependence of explosion outcome on progenitor profile, grid resolution, and neutrino microphysics as well as study emergent neutrino and gravitational wave signatures. Building on communal efforts, we are now poised to transition from individual case studies to population studies of CCSNe phenomenology in 3D.

Speaker: Mr David Vartanyan (Princeton)

10:45 Discussion

9 Fully relativistic CCSN simulations of 20Msun star with magnetic field

We will report fully relativistic CCSN simulations of 20Msun progenitor star with M1 neutrino transport. To explore the role of magnetic field, particularly in the explosion dynamics and in the explosive nucleosynthesis, we calculated several models w/ and w/o rotation and magnetic field. Regarding the dynamics, we found a bipolar outflow in strongly magnetized model, while oblate like explosion is seen in non-magnetized rotating model. The ejecta in the magnetorotational explosion (MRE) model show relatively higher entropy and Ye compared to the previous studies with rather more simplified neutrino treatments. Because of the 3D effects, the MRE is not a collimated jet-like explosion and the abundance pattern reaches only up to the second peak. This is consistent with previous study. In this talk, we will also discuss their multi-messenger aspects including neutrino and GW signals.

Speaker: Takami Kuroda (Institut für Kernphysik, Technische Universität Darmstadt)

11:20 Discussion

10 Multi-dimensional core-collapse supernova simulations with the Boltzmann-radiation-hydrodynamics code

In this talk, I would like to report the recent results of the multi-dimensional core-collapse simulations with the Boltzmann-radiation-hydrodynamics code, which solves the Boltzmann equations for neutrino transport directly. The neutrino transport is an important ingredient of the core-collapse supernova (CCSN) simulations since the neutrino heating plays a crucial role in the explosion mechanism. Indeed, the fact that the CCSN does not explode under the spherical symmetry is concluded by the Boltzmann-radiation-hydrodynamics simulations. Among recent multi-dimensional CCSN simulations, only our Boltzmann-radiation-hydrodynamics code solves the neutrino transport in a direct manner.

We simulate the collapse of non-rotating and rotating cores of the progenitor with $11.2\,M_\odot$ with Furusawa-Shen and Lattimer-Swesty equations of state under the axisymmetry. We pay particular attention to the neutrino distribution in phase space, which is accessible only by the Boltzmann solver. Especially, we compare the Eddington tensors calculated both from the raw data and from the M1-closure approximation. We find that the difference in the Eddington factors reaches $\sim20\%$ in our simulation. This is due to the different dependence of the Eddington and flux factors on the angular profile of the neutrino distribution function, and hence modification to the closure relation is needed.

Speaker: Akira Harada (ICRR)

MICRA2019AkiraHarada.pdf

11:50 Discussion

12:00 Lunch

Core-Collapse Supernovae: Core-Collapse Supernova III

Modeling, observations, and theory of Core-collapse

11 The Impact of GR Hydrodynamics in CCSN Simulations

Numerical simulations of core collapse supernovae (CCSNe) must balance numerical accuracy with computational cost in order to produce numerous, high-fidelity simulations. The FLASH code architecture leverages advanced neutrino treatments and a general relativistic effective potential (GREP) to efficiently simulate CCSNe. These explosive, high energy events are prolific sources of gravitational waves (GWs) and would be detectable with current age GW detectors, in the case of a Galactic event. While the GREP has the advantage of speed, it has been shown to misrepresent certain aspects of the GW signal from CCSNe. Here will be a review of current GW studies using FLASH and an outline to integrate GR hydrodynamics into its framework.

Speaker: Michael Pajkos (Michigan State University)

MICRA_Pajkos.pdf

14:20 Discussion

12 A pulsar-runaway-pair from a nearby supernova about 1.8 Myr ago that ejected 60-Fe found on Earth

The detection of 1.5-3.2 Myr 60-Fe on Earth indicates recent nearby core-collapse supernovae.
For supernovae in multiple stars, the primary stars become neutron stars, while former
companions can get unbound (runaway stars). By tracing back the space motion of runaway
and neutron stars to the nearest young (about 16 Myr) association of massive stars
(Scorpius-Centaurus-Lupus), we found kinematic evidence that a certain runaway star
and a certain radio pulsar were released by a supernova in a binary about 1.8 Myr ago
at about 107 pc distance; association age and flight time determine the progenitor mass
(16-18 M_sun), which can constrain supernova nucleosynthesis yields and 60-Fe uptake on Earth.
Our scenario links 60-Fe found on Earth to an individual supernova in a binary.

Speaker: Prof. Ralph Neuhaeuser (AIU U Jena)

14:50 Discussion

15:00 Afternoon Coffee

Core-Collapse Supernovae: Core-Collapse Supernova IV

Modeling, observations, and theory of Core-collapse

13 Challenge to Black Hole Models and Supernova explosion driven by Magnetic

1) A unusually strong radial magnetic field detected near our Galactic Center (2013) is consistent with the prediction from our model of supermassive object with magnetic monopoles (MM) ( Peng and Chou 2001). The important implications of the unusually strong radial magnetic field near the GC are: a) A strong evidence of the existence of MM; b) The black hole model of the suppermassive object at the GC is unphysical (Peng et al., 2016; 2017).
2) I shall also give query on the black hole models for other quasars and active galactic nuclei.The key dilemma of the black hole model is the question on the BH mass at the center of AGNs.
The dilemma will disappear in our model of Supper-massive Stars with MM.
3) Taking the RC effect (nucleons may decay catalyzed by MM) as an energy source, we have proposed an unified model for various supernova explosion (Peng et al. 2017). In our model, the remnant of the collapsed core of supernova is still a neutron star rather than a black hole no matter how huge of the supernova mass. That means, black holes with stellar mass are impossible to be formed through supernova explosion.
4) We may explain the physical reason of the Hot Big Bang of the Universe with the similar mechanism of supernova explosion by using the RC effect as an energy source. That is , the primordial Black hole of the whole Universe is no physical

Speaker: Prof. Qiuhe Peng (Nanjing University)

15:50 Discussion

Core-Collapse Supernovae: Breakout/Debrief

Modeling, observations, and theory of Core-collapse

Wednesday 14 August

Equation of State: Equation of State I

14 The Hadronic Equation of State for Neutron Stars

The equation of state (EoS) of dense hadronic matter is of crucial importance for the description of the static and dynamical properties of neutron stars. In this talk I will review the current status of the hadronic EoS for neutron stars, from the point of both ab-initio many-body approaches and phenomenological models. The theoretical predictions for the hadronic EoS will be compared to the data coming from both nuclear physics experiments and astrophysical observations, providing insights for future research.

Speaker: Dr Laura Tolos (Institute for Theoretical Physics, Goethe University )

09:30 Discussion

09:45 Morning Coffee

Equation of State: Equation of State II

15 Equation of State Effects in the Core Collapse of Massive Stars

Uncertainties in our knowledge of the properties of dense matter near and above nuclear saturation density are among the main sources of variations in multi-messenger signatures predicted for the core collapse of massive stars and the properties of the resulting remnants. In this talk, I discuss how variations in the equation of state of dense matter affect the core collapse of massive stars. By simulating the core collapse of many different progenitors using a wide range of equations of state we conclude that temperature effects are among the largest sort of uncertainty in the dynamics of the core collapse, the emitted neutrino signal, and the compact object formed.

Speaker: André da Silva Schneider (Stockholm University)

10:45 Discussion

16 Neutrino emission and equation of state in core collapse supernovae

I would like to report the recent progress on microphysics and supernova neutrinos utilizing our numerical simulations based on Boltzmann equation. As recent progress of core-collapse supernova simulations is rapid toward the first principle type calculations, remaining uncertainties of the microphysics are becoming important.

We have been developing the data table of equation of state (EOS) based on the nuclear many body theories both in non-relativistic and relativistic approaches including detailed information of mixture of nuclei (Togashi, Furusawa 2017, 2019). Revision of Shen EOS table is on going with improvement of isovector interactions for neutron matter, keeping good properties of nuclei and nuclear matter with TM1 (Hu, Sumiyoshi et al., 2019). Our group is running 2D core-collapse supernovae by neutrino-radiation hydrodynamics with 6D Boltzmann solver using some of these microphysics and I would like to touch upon their effects.

I would like to also report the prediction of neutrino detection at Superkamiokande based on supernova neutrino database and a series of simulations. Long term behavior of event number of neutrino detection over 100 sec is studied by proto-neutron cooling simulations to determine the last event and burst duration. We propose the backward time plot to extract the properties of proto-neutron star (Suwa et al. 2019). 1D simulations with Boltzmann equation have been also applied to predictions of diffuse supernova neutrino background in order to assess the fraction of black hole formation from massive stars (Horiuchi et al. 2018).

Speaker: Kosuke Sumiyoshi (National Institute of Technology, Numazu College)

1908_MICRA.pdf

11:20 Discussion

17 Core-collapse supernovae and equation of state effects*

Core-collapse supernovae (CCSN) are cosmic laboratories for physics at the extremes and numerical simulations are essential to help us understand the underlying mechanisms in these events. A key ingredient in simulations is the equation of state (EOS), which determines the contraction behavior of the proto-neutron star (PNS) and thus impacts neutrino energies and explosion dynamics. However, the EOS for hot and dense matter is still not fully understood and CCSN simulations rely on EOS models that differ in their underlying theory and nuclear matter properties.

We present the first systematic study on the impact of different nuclear matter properties of the EOS in CCSN simulations. This allows us to examine possible reasons for differences in commonly used EOS in simulations. We find that the contraction behavior of the PNS is mainly governed by the effective mass, which impacts the shock propagation.

*Supported by the Deutsche Forschungsgemeinschaft through SFB 1245 (Projektnummer 279384907) and the European Research Council Grant No. 677912 EUROPIUM.

Speaker: Hannah Yasin

11:50 Discussion

12:00 Lunch

Equation of State: Equation of State III

18 A unified quark-hadron equation of state

The aim of our work is to develop a unified equation of state (EoS) for nuclear and quark matter for a wide range in temperature, baryon density and iso-spin asymmetry, which will make it applicable for heavy-ion collisions as well as for the astrophysics of neutron stars, neutron-star mergers and supernova explosions.
As a first step, we use improved EoS for the hadronic and quark matter phases and join them via Maxwell construction. To go beyond this simple Ansatz, we are developing a consistent cluster expansion for quark matter, based on the Phi- derivable formalism [1]. In hadronic phase this reproduces the generalized Beth-Uhlenbeck formalism by Roepke et.al. [2]. To this end, we work with a relativistic density functional approach for the self energies in a quasi particle picture [3], which gives us the possibility to start with a reasonable physical basis and apply improvements to fit certain constraints from lattice QCD and neutron star measurements.

[1] N. U. F. Bastian, D. Blaschke, T. Fischer and G. Röpke, Universe 4, 67 (2018).
[2] G. Röpke, N.-U. Bastian, D. Blaschke, T. Klähn, S. Typel and H. H. Wolter, Nucl. Phys. A 897, 70 (2013).
[3] M. A. R. Kaltenborn, N. U. F. Bastian and D. B. Blaschke, Phys. Rev. D 96, 056024 (2017).

Speaker: Niels-Uwe Bastian (University of Wroclaw)

201905_Jena_pub.pdf

14:20 Discussion

19 Optimal neutron-star mass ranges to constrain the equation of state of nuclear matter with electromagnetic and gravitational-wave observations

Exploiting a very large library of physically plausible equations of state (EOSs) containing more than $10^7$ members and yielding more than $10^9$ stellar models, we conduct a survey of the impact that a neutron-star radius measurement via electromagnetic observations can have on the EOS of nuclear matter. Such measurements are soon to be expected from the ongoing NICER mission and will complement the constraints on the EOS from gravitational-wave detections. Thanks to the large statistical range of our EOS library, we can obtain a first quantitative estimate of the commonly made assumption that the high-density part of the EOS is best constrained when measuring the radius of the most massive, albeit rare, neutron stars with masses $M > 2.1 M$?. At the same time, we find that radius measurements of neutron stars with masses $M \sim 1.7 − 1.85 M$? can provide the strongest constraints on the low-density part of the EOS. Finally, we quantify how radius measurements by future missions can further improve our understanding of the EOS of matter at nuclear densities.

Speaker: Lukas Weih (Goethe University, Frankfurt)

14:50 Discussion

15:00 Afternoon Coffee

Equation of State: Breakout/Debrief

Thursday 15 August

Mergers: Mergers I

20 From merger to electromagnetic emission

The recent GW+EM detection of a neutron star merger has underlined the multitude of physical processes that are needed for a reliable prediction of multi-messenger signals. In the talk I will discuss the various processes that lead from the merger to the electromagnetic emission. Particular attention will be payed to topics where our understanding is incomplete and more progress is needed.

Speaker: Prof. Stephan Rosswog (Stockholm University)

09:30 Discussion

09:45 Morning Coffee

Mergers: Mergers II

21 Modelling on neutron star mergers: status and open issues

A robust and quantitative understanding of neutron star mergers requires detailed numerical simulations. The latter must include all the relevant physics, resolve the necessary lenght scales, and cover all the important temporal phases. The key role of all fundamental interactions makes this task extremely challenging. In this talk, I will briefly summarize the present status of the field and highlight our present understanding. Despite the many insights achieved in the last years, many open issues remain, including the properties of hot nuclear matter and the relevance of weak interaction. The exploration and the solution of these open questions are essential to interpret past and future multimessenger detections from neutron star mergers.

Speaker: Dr Albino Perego (University of Trento)

10:45 Discussion

22 Neutrinos in Binary Neutron Star Mergers

I will present results of general relativistic hydrodynamic (GRHD) simulations of binary neutron star (BNS) mergers with a hybrid leakage-transport scheme for the neutrino treatment. I will discuss the matter dynamics and show the thermodynamic conditions of the fluid in the region where the three evolved neutrino species decouple from matter. Finally, I will give an overview of the state-of-the-art for neutrino evolution in GRHD.

Speaker: Andrea Endrizzi (TPI - University of Jena)

11:20 Discussion

23 Black hole simulations with the FO-CCZ4 formulation of the Einstein equations and ADER discontinuous Galerkin schemes

We present FO-CCZ4, a strongly hyperbolic first-order formulation of the Einstein
equations based on the conformal and covariant Z4 system with constraint-violation damping. This formulation combines the advantages of a conformal and traceless formulation, with the suppression of constraint violations given by the damping terms, but being first order in time and space, it is particularly suited for a discontinuous Galerkin (DG) implementation. The strongly hyperbolic first-order formulation has been obtained by making careful use of first and second-order ordering constraints. A proof of strong hyperbolicity is given for a selected choice of standard gauges via an analytical computation of the entire eigenstructure of the FO-CCZ4 system. A key feature of our formulation is that the first-order CCZ4 system decouples into a set of pure ordinary differential equations and a reduced hyperbolic system of partial differential equations that contains only linearly degenerate fields. We implement FO-CCZ4 in a high-order path-conservative (ADER)-DG scheme with adaptive mesh refinement and local time-stepping, supplemented with a third-order ADER-WENO subcell finite-volume limiter in order to deal with singularities arising with black holes. We validate the correctness of the formulation through a series of standard tests in vacuum, performed in one, two and three spatial dimensions, and also present preliminary results on the evolution of binary black-hole systems. To the best of our knowledge, these are the first successful three-dimensional simulations of moving punctures carried out with high-order DG schemes using a first-order formulation of the Einstein equations. Supported by European Research Council Grant No. 677912 EUROPIUM

Speaker: Federico Maria Guercilena (Institut für Kernphysik, Technische Universität Darmstadt)

talk_guercilena.pdf

11:50 Discussion

12:00 Lunch

Mergers: Mergers III

24 Signatures of first order phase transitions and of spins in neutron star mergers

With the detection of GW170817 we have observed the first multi messenger signal from two merging neutron stars.
This signal carried a multitude of information about the underlying equation of state (EOS) of nuclear matter, which so far is not known for densities above nuclear saturation. In particular it is not known if exotic states or even a phase transition to quark matter can occur at densities so extreme that they can’t be probed by any current experiment.
In this talk we will show how the information carried in the gravitational wave signal of GW170817 can be used to constrain the EOS at densities above saturation and what we can learn about the possible existence of phase transitions. We will also comment on how we can use future gravitational wave detections in order to set limits on the existence of neutron stars having a quark matter core.
Finally, we will discuss the detectability of a hadron-quark phase transition taking place in a neutron star merger event. Starting from a fully consistent description of matter having a first-order phase transition to quark matter at finite temperatures, we will demonstrate what imprint a hadron-quark phase transition would leave on the gravitational-wave signal. We will conclude by showing that a hot and dense core of quark matter is formed in such a simulation and will also briefly comment on how this is related to the phase diagram of quantum chromodynamics.

Additionally, we will report on recent results of neutron star mergers with spin and show how part of the mass ejection in a neutron star merger can be suppressed when the neutron stars have spins $\simeq 0.28$.

Speaker: Elias Most

14:20 Discussion

25 Numerical relativity informed models of the electromagnetic counterpart of neutron star mergers

Neutron star merger is a unique cosmic laboratory to investigate general relativity in a strong field regime and fundamental physics, including dense matter and heavy-elements-nucleosynthesis.

Our work focuses on the electromagnetic counterpart of the gravitational wave source GW170817. We study the merger dynamics and light curves employing the state of the art numerical, general relativistic simulations with microphysics.

We find that cases with long-lived remnants exhibit a quasi-steady outflow, powered by the interaction between the remnant and the surrounding disk. The outflow has distinct from well known dynamical ejecta properties and larger mass. Including it into the numerical-relativity informed kilonova models, we show that this component is imporntnat for understanding the early blue component of AT2017gfo.

Speaker: Vsevolod Nedora (Theoretisch-Physikalisches Institut)

14:50 Discussion

15:00 Afternoon Coffee

Mergers: Mergers IV

26 A multi-dimensional implementation of the Advanced Spectral neutrino Leakage scheme

Merging neutron stars are both gravitational wave and electromagnetic transient sources, as confirmed by the detection of the GW170817 event. The gravitational wave emission was indeed followed by emission all across the electromagnetic spectrum, including an optical and infrared signal known as macronova. This signal is powered by the radioactive decay of freshly synthesized r-process elements.
The early blue component requires ejecta with electron fractions $Y_e > 0.25$. Such large values in a neutron rich environment like the one coming from a neutron star merger point to a re-processing of a fraction of the ejecta by weak interactions.
In this talk I will present a multi-dimensional implementation of the Advanced Spectral neutrino Leakage applicable to binary neutron star mergers. The main goal is modeling the neutrino absorption in the semi-transparent regime, which can drive winds from the merger and raise the $Y_e$. This ejection channel is thought to be behind the observed blue macronova component. Preliminary numerical tests of the scheme are presented in the form of snapshot calculations and compared against a two-moment scheme approach.

Speaker: Mr Davide Gizzi (Stockholm University)

15:50 Discussion

Mergers: Breakout/Debrief

Friday 16 August

Nucleosynthesis: Nucleosynthesis I

27 r-process nucleosynthesis in compact object mergers

Thirty years after both the light and neutrino emission was observed from SN1987A, the neutron star merger event GW170817 demonstrated the power of new tools in multi-messenger astronomy. Since LIGO/VIRGO gravitational wave detection enables identification and pointed electromagnetic follow-up of merger events, new insights into these rare and interesting systems can be gained. The observations of the GW170817 electromagnetic counterpart suggested the production of heavy elements via the rapid neutron capture process (r process) due to the light curve compatibility with the presence of high opacity elements such as the lanthanides. However lanthanide production in r-process nucleosynthesis is subject to large uncertainties from nuclear physics and astrophysics unknowns. For instance the rare-earth abundance peak, a feature of enhanced lanthanide production at A~164 seen in the solar r-process residuals, is not robustly produced in r-process calculations when nuclear physics inputs are varied. Nuclear and astrophysics uncertainties also make it difficult to know if merger events are responsible for populating the heaviest observed nuclei, the actinides. An r process which reaches the actinides is also likely to host fission, which is largely experimentally uncharted for neutron-rich nuclei, further compounding the difficulty in predicting the nucleosynthetic outcome in merger events. Here we will review what can be gleaned regarding heavy element production from this merger event with an emphasis on how nuclear physics unknowns can affect such conclusions. We will discuss a potential direct signature of actinide production in merger environments as well as the potential for future experimental and theoretical efforts to refine our knowledge of fission in the r process. The question of where nature primarily produces the heavy elements can only be answered through such collaborative efforts between experiment, theory, and observation.

Speaker: Nicole Vassh

09:30 Discussion

09:45 Morning Coffee

Nucleosynthesis: Nucleosynthesis II

28 Nucleosynthesis in core-collapse supernovae

Core-collapse supernovae (CCSNe) are one of the most important sites of element synthesis in the universe and drive the chemical evolution of galaxies. A major goal of CCSN nucleosynthesis studies is to determine how nucleosynthesis outcomes depend on progenitor properties (e.g. mass and metallicity) and the explosion details. Traditional calculations do not account for neutrino-matter interactions, thus omitting key microphysics relevant for both the explosion and the explosive nucleosynthesis. In this talk, I will review our current understanding of nucleosynthesis in core-collapse supernovae. I will also present nucleosynthesis yields for progenitors of different masses and metallicities exploded using PUSH. The PUSH method is based on the neutrino-driven mechanism and follows the evolution of the proto-neutron star as well as the electron fraction of the ejecta. This allows a more accurate treatment of nucleosynthesis in the innermost stellar layers. I will focus especially on the synthesis of iron group elements, which are produced in these innermost layers and are therefore quite sensitive to the explosion details. I will contrast our results with more traditional calculations. Finally, I will compare our predicted yields to observationally derived values for supernovae and metal-poor stars. This complete set of isotopic yields provides an essential input for modeling galactic chemical evolution.

Speaker: Sanjana Curtis

10:45 Discussion

29 Influence of astrophysical and nuclear physics uncertainties on the nucleosynthesis in core-collapse supernova neutrino-driven winds

Neutrino-driven winds emerging after a successful core-collapse
supernovae can produce the lighter heavy elements between Fe and Ag depending on the
properties of the ejecta.
However, despite the fast progress in supernovae simulations in the last
decades, there are still large uncertainties in the astrophysical
conditions.
We rely on a steady-state neutrino-driven wind model to
systematically study the influence of astrophysical uncertainties on
the nucleosynthesis evolution in neutrino-driven ejecta.
Furthermore, uncertainties in the nuclear physic input to the
nucleosynthesis calculation impact the abundance patterns.
In order to identify key reactions, we perform sensitivity studies based on a
Monte Carlo approach for a variety of astrophysical conditions in neutron- and
proton-rich ejecta.

Supported by the European Research Council Grant No. 677912 EUROPIUM
and the Deutsche Forschungsgemeinschaft through SFB 1245 (Projektnummer
279384907).

Speaker: Maximilian Jacobi (TU-Darmstadt)

11:20 Discussion

30 Inhomogeneous Galactic Chemical Evolution of r-process Elements

The origin of the heaviest elements is still a matter of debate. For the rapid neutron
capture process (“r-process”), multiple sites have been proposed, e.g., neutron star
mergers and (sub-classes) of supernovae. R-process elements have been measured in
metal-poor halo stars. Galactic archaeology studies show that the r-process abundances
among these stars vary by over two orders of magnitude. On the other hand, abundances
in stars in the Galactic disk do not differ greatly. This leads to two major open questions:
1. What is the reason for such a huge abundance scatter of r-process elements in
the early Galaxy?
2. While the large scatter at low metallicities might point to a rare production site,
why is there barely any scatter at Solar metallicities?
We use the high resolution ((20 pc)^3 /cell) inhomogeneous Galactic chemical evolution
tool “ICE” to study the role of the contributing sources of r-process elements. Our main
findings are that additionally to neutron star mergers, a second, early acting site is
necessary. We assume “magnetorotationally driven supernovae” can act as this additional
and earlier r-process site and conclude that our simulations with an adequate combination
of these two sites successfully reproduce the observed r-process elemental abundances in
the Galactic halo. Finally, we discuss the potential role of neutron star-black hole mergers
as alternative earlier r-process site.

Speaker: Benjamin Wehmeyer (Konkoly Observatory & Univ. of Hertfordshire)

11:50 Discussion

Logistics: Wrap-up