White dwarf dynamical interactions. Enrique García-Berro. Jornades de Recerca, Departament de Física

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1 White dwarf dynamical interactions Enrique García-Berro Jornades de Recerca, Departament de Física

2 CONTENTS 1. Introduction 2. Smoothed Particle Hydrodynamics 3. White dwarf mergers 4. White dwarf collisions

3 CONTENTS 1. Introduction 2. Smoothed Particle Hydrodynamics 3. White dwarf mergers 4. White dwarf collisions

4 CONTENTS 1. Introduction 1. Introduction 1.1 White dwarfs 1.2 Type Ia supernovae 1.3 White dwarf interactions

1. INTRODUCTION 1.1 White dwarfs o White dwarfs are the remnants of the evolution of the vast majority of normal stars. o They are the most frequent (>90%) fossil stars within the stellar graveyard.

5 1. INTRODUCTION 1.1 White dwarfs o White dwarfs are the remnants of the evolution of the vast majority of normal stars. o They are the most frequent (>90%) fossil stars within the stellar graveyard. o After main sequence stars exhaust hydrogen in their cores, they become red giants. o After red giants burn helium, converting it into carbon and oxygen, they eject the hydrogen-rich outer layers form a planetary nebula and become white dwarfs.

6 1. INTRODUCTION 1.1 White dwarfs o White dwarfs are compact objects, supported by the pressure of degenerate electrons. o The basic theory of white dwarf structure was developed by Chandrasekhar & Fowler (Nobel Prize, 1983), independently. o The basic idea is actually very simple: since the pressure of degenerate electrons does not depend on the temperature they simply cool down at constant radius. o Moreover, we now understand very well their mechanical and thermal properties. o One important issue: the mass-radius relationship.

7 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear supernovae. o They are among the most energetic events in the universe. o They all have nearly the same luminosity, making them excellent distance indicators. o Actually, they can be considered, to a good approximation standard candles (the light curve can be calibrated). o This allowed the discovery of the accelerated expansion of the universe (Nobel Prize 2011, to Perlmutter, Schmidt & Riess).

8 1. INTRODUCTION 1.2 Type Ia supernovae o We know the physical mechanism powering the outburst: the explosion of a carbon-oxygen white dwarf in a binary system, with a mass close to the Chandrasekhar limit. o However, the nature of the stellar systems which give rise to SNe Ia remains a long-standing mystery. o There are several possible scenarios: Single degenerate (SD): WD + RG Core degenerate (CD): WD + core of an AGB star Double degenerate (DD): WD + WD in a binary system White dwarf collisions (WDC): WD + WD.

9 1. INTRODUCTION 1.2 Type Ia supernovae o We know the physical mechanism powering the outburst: the explosion of a carbon-oxygen white dwarf in a binary system, with a mass close to the Chandrasekhar limit. o However, the nature of the stellar systems which give rise to SNe Ia remains a long-standing mystery. o There are several possible scenarios: Single degenerate (SD): WD + RG Core degenerate (CD): WD + core of an AGB star Double degenerate (DD): WD + WD in a binary system White dwarf collisions (WDC): WD + WD.

10 1. INTRODUCTION 1.2 Type Ia supernovae o We know the physical mechanism powering the outburst: the explosion of a carbon-oxygen white dwarf in a binary system, with a mass close to the Chandrasekhar limit. o However, the nature of the stellar systems which give rise to SNe Ia remains a long-standing mystery. o There are several possible scenarios: Single degenerate (SD): WD + RG Core degenerate (CD): WD + core of an AGB star Double degenerate (DD): WD + WD in a binary system White dwarf collisions (WDC): WD + WD.

$1. INTRODUCTION 1.3 White dwarf interactions o A large fraction of stars belong to binary systems or, more generally, to multiple systems.$

11 1. INTRODUCTION 1.3 White dwarf interactions o A large fraction of stars belong to binary systems or, more generally, to multiple systems. o A substantial number of these binary systems are so close that at a given time of their life a mass transfer episode will occur. o Moreover, in dense stellar systems, like globular clusters or nuclei of galaxies, single stars pass very close each other.

has received considerable interest in the last 30 years, for multiple reasons.

12 1. INTRODUCTION 1.3 White dwarf interactions o The study of the interactions between two white dwarfs has received considerable interest in the last 30 years, for multiple reasons. o The effort of producing SNe Ia in white dwarf interactions has been only partially successful, and only under certain circumstances a powerful detonation ensues.

13 1. INTRODUCTION 1.3 White dwarf interactions o Even if dynamical interactions fail in producing a supernova outburst, they can still be responsible of some other interesting phenomena: R Corona Borealis stars High-field magnetic white dwarfs Anomalous X-Ray pulsars Powerful sources of gravitational waves

14 CONTENTS 1. Introduction 2. Smoothed Particle Hydrodynamics 3. White dwarf mergers 4. White dwarf collisions

15 CONTENTS 2. Smoothed particle hydrodynamics 2. Smoothed particle hydrodynamics 2.1 Generalities 2.2 Numerical setup 2.3 Input physics

2. SMOOTHED PARTICLE HYDRODYNAMICS 2.1 Generalities o SPH is an approximate method to solve the equations of fluid dynamics. o The fluid elements are replaced by particles of finite size.

16 2. SMOOTHED PARTICLE HYDRODYNAMICS 2.1 Generalities o SPH is an approximate method to solve the equations of fluid dynamics. o The fluid elements are replaced by particles of finite size. o Mathematicians would think about these particles as interpolation points on a moving grid. o Physicist think about them as regular particles, moving under the action of normal forces.

2. SMOOTHED PARTICLE HYDRODYNAMICS 2.1 Generalities o Interesting features: Advection is treated in a very natural way. Hence, transport phenomena occur naturally.

17 2. SMOOTHED PARTICLE HYDRODYNAMICS 2.1 Generalities o Interesting features: Advection is treated in a very natural way. Hence, transport phenomena occur naturally. When two different phases occur, the interfaces move freely. We do not have a fixed grid. Resolution is dependent on both space and time, without rezoning. Complex physics can be easily introduced. Kernel estimation can be used to interpolate anywhere at any time.

2. SMOOTHED PARTICLE HYDRODYNAMICS 2.2 Numerical setup o Cubic spline (Monaghan & Lattanzio 1985). o Octree (Barnes & Hut 1986). o Smoothing lengths: iteration method (Price & Monaghan 2007).

18 2. SMOOTHED PARTICLE HYDRODYNAMICS 2.2 Numerical setup o Cubic spline (Monaghan & Lattanzio 1985). o Octree (Barnes & Hut 1986). o Smoothing lengths: iteration method (Price & Monaghan 2007). o Artificial viscosity based on Riemann solvers (Monaghan 1997), variable viscosity parameters of Morris & Monaghan (1997) and switch of Balsara (1995). o Predictor-corrector numerical scheme with variable timestep (Serna et al., 1996). o Time steps are the same for all particles. o Message Passage Interface (MPI) libraries.

2. SMOOTHED PARTICLE HYDRODYNAMICS 2.3 Input physics o Simultaneous evolution of the energy and temperature. o Helmholtz EOS (Timmes & Swesty 2000).

19 2. SMOOTHED PARTICLE HYDRODYNAMICS 2.3 Input physics o Simultaneous evolution of the energy and temperature. o Helmholtz EOS (Timmes & Swesty 2000). o Nuclear network: 14 nuclei: He, C, O, Ne, Mg, Si, S, Ar, Ca, Ti, Cr, Fe, Ni, Zn. Reactions: captures of α particles, associated back reactions, fusion of two C nuclei, reaction between C and O and between two O nuclei. REACLIB database (Cyburt et al. 2010). o Neutrino emissivity (Itoh et al. 1997).

20 CONTENTS 1. Introduction 2. Smoothed Particle Hydrodynamics 3. White dwarf mergers 4. White dwarf collisions

21 3. WHITE DWARF MERGERS

22 3. WHITE DWARF MERGERS

23 CONTENTS 1. Introduction 2. Smoothed Particle Hydrodynamics 3. White dwarf mergers 4. White dwarf collisions

24 CONTENTS 4.White dwarf collisions 4. White dwarf collisions 4.1 Initial conditions 4.2 Outcomes 4.3 Characteristics of the interactions 4.4 Observational signatures

25 4. WHITE DWARF COLLISIONS 4.1 Initial conditions o We consider five white dwarfs with masses 0.4, 0.6, 0.8 and 1.0 M, with the appropriate composition (He, CO and ONe). o The initial trajectories are elliptical, corresponding to a post-capture scenario.

26 4. WHITE DWARF COLLISIONS 4.1 Initial conditions

27 4. WHITE DWARF COLLISIONS 4.2 Outcomes Eccentric orbit, 0.8 M M

28 4. WHITE DWARF COLLISIONS 4.2 Outcomes Lateral collision: single remnant

29 4. WHITE DWARF COLLISIONS 4.2 Outcomes Direct collision: disruption of one star

30 4. WHITE DWARF COLLISIONS 4.2 Outcomes Direct collision: disruption of both stars

31 4. WHITE DWARF COLLISIONS 4.2 Outcomes Direct collision: disruption of one star

32 4. WHITE DWARF COLLISIONS 4.2 Outcomes Direct collision: disruption of both stars

33 4. WHITE DWARF COLLISIONS 4.2 Outcomes

34 4. WHITE DWARF COLLISIONS 4.3 Characteristics of the interactions

4. WHITE DWARF COLLISIONS 4.3 Characteristics of the interactions o The peak temperatures reached in the interactions are typically 10 9 K, driving extensive nucleosynthesis in the shocked regions.

35 4. WHITE DWARF COLLISIONS 4.3 Characteristics of the interactions o The peak temperatures reached in the interactions are typically 10 9 K, driving extensive nucleosynthesis in the shocked regions. o Two interactions result in a powerful detonation, producing a SNIa outburst. o Some other simulations result in bound remnants with masses close to the Chandrasekhar limit. o A wide range of masses of 56 Ni is produced, which may explain some underluminous transients.

4. WHITE DWARF COLLISIONS 4.4 Observational signatures o Gravitational wave emission in the slow-motion, weakfield, quadrupole approximation (Misner et al. 1973).

36 4. WHITE DWARF COLLISIONS 4.4 Observational signatures o Gravitational wave emission in the slow-motion, weakfield, quadrupole approximation (Misner et al. 1973). o Late-time bolometric light curve, using a Monte Carlo code which solves the transport of photons, and the injection of energy by γ-rays produced by the 56 Ni and 56 Co decays (Kushnir et al. 2013). o Thermal neutrino emission, using the rates of Itoh et al. (1997). o Fallback accretion X-ray luminosity (Rosswog 2007).

37 4. WHITE DWARF COLLISIONS Gravitational waves Eccentric orbits

38 4. WHITE DWARF COLLISIONS Gravitational waves Lateral collisions

39 4. WHITE DWARF COLLISIONS Light curves

40 4. WHITE DWARF COLLISIONS Thermal neutrinos

41 4. WHITE DWARF COLLISIONS Fallback luminosities

high-energy observations, and data from the future space borne

42 4. WHITE DWARF COLLISIONS 4.4 Observational signatures o A combination of optical and high-energy observations, and data from the future space borne gravitational wave detectors would provide in valuable insight on the conditions under which these interactions occur.

43 White dwarf dynamical interactions Enrique García-Berro Jornades de Recerca, Departament de Física

White dwarf collisions: a new pathway to type Ia supernovae. Enrique García-Berro & Pablo Lorén-Aguilar

White dwarf collisions: a new pathway to type Ia supernovae Enrique García-Berro & Pablo Lorén-Aguilar Supernovae, hypernovae and binary driven hypernovae An Adriatic Workshop Pescara 2016 CONTENTS 1.