White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E....
Transcript of White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E....
![Page 1: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/1.jpg)
White dwarf dynamical interactions
Enrique García-Berro
Jornades de Recerca, Departament de Física
![Page 2: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/2.jpg)
White dwarf dynamical interactions – E. García-Berro
1. Introduction 2. Smoothed Particle Hydrodynamics 3. White dwarf mergers 4. White dwarf collisions
CONTENTS
![Page 3: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/3.jpg)
White dwarf dynamical interactions – E. García-Berro
1. Introduction 2. Smoothed Particle Hydrodynamics 3. White dwarf mergers 4. White dwarf collisions
CONTENTS
![Page 4: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/4.jpg)
White dwarf dynamical interactions – E. García-Berro
CONTENTS 1. Introduction
1. Introduction 1.1 White dwarfs 1.2 Type Ia supernovae 1.3 White dwarf interactions
![Page 5: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/5.jpg)
White dwarf dynamical interactions – E. García-Berro
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.
![Page 6: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/6.jpg)
White dwarf dynamical interactions – E. García-Berro
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.
![Page 7: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/7.jpg)
White dwarf dynamical interactions – E. García-Berro
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).
![Page 8: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/8.jpg)
White dwarf dynamical interactions – E. García-Berro
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.
![Page 9: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/9.jpg)
White dwarf dynamical interactions – E. García-Berro
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.
![Page 10: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/10.jpg)
White dwarf dynamical interactions – E. García-Berro
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.
![Page 11: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/11.jpg)
White dwarf dynamical interactions – E. García-Berro
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.
![Page 12: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/12.jpg)
White dwarf dynamical interactions – E. García-Berro
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.
![Page 13: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/13.jpg)
White dwarf dynamical interactions – E. García-Berro
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
![Page 14: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/14.jpg)
White dwarf dynamical interactions – E. García-Berro
1. Introduction 2. Smoothed Particle Hydrodynamics 3. White dwarf mergers 4. White dwarf collisions
CONTENTS
![Page 15: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/15.jpg)
White dwarf dynamical interactions – E. García-Berro
CONTENTS 2. Smoothed particle hydrodynamics
2. Smoothed particle hydrodynamics 2.1 Generalities 2.2 Numerical setup 2.3 Input physics
![Page 16: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/16.jpg)
White dwarf dynamical interactions – E. García-Berro
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.
![Page 17: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/17.jpg)
White dwarf dynamical interactions – E. García-Berro
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.
![Page 18: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/18.jpg)
White dwarf dynamical interactions – E. García-Berro
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.
![Page 19: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/19.jpg)
White dwarf dynamical interactions – E. García-Berro
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).
![Page 20: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/20.jpg)
White dwarf dynamical interactions – E. García-Berro
1. Introduction 2. Smoothed Particle Hydrodynamics 3. White dwarf mergers 4. White dwarf collisions
CONTENTS
![Page 21: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/21.jpg)
White dwarf dynamical interactions – E. García-Berro
3. WHITE DWARF MERGERS
![Page 22: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/22.jpg)
White dwarf dynamical interactions – E. García-Berro
3. WHITE DWARF MERGERS
![Page 23: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/23.jpg)
White dwarf dynamical interactions – E. García-Berro
1. Introduction 2. Smoothed Particle Hydrodynamics 3. White dwarf mergers 4. White dwarf collisions
CONTENTS
![Page 24: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/24.jpg)
White dwarf dynamical interactions – E. García-Berro
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
![Page 25: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/25.jpg)
White dwarf dynamical interactions – E. García-Berro
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.
![Page 26: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/26.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.1 Initial conditions
![Page 27: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/27.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.2 Outcomes
Eccentric orbit, 0.8 M + 1.0 M
![Page 28: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/28.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.2 Outcomes
Lateral collision: single remnant
![Page 29: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/29.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.2 Outcomes
Direct collision: disruption of one star
![Page 30: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/30.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.2 Outcomes
Direct collision: disruption of both stars
![Page 31: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/31.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.2 Outcomes
Direct collision: disruption of one star
![Page 32: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/32.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.2 Outcomes
Direct collision: disruption of both stars
![Page 33: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/33.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.2 Outcomes
![Page 34: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/34.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.3 Characteristics of the interactions
![Page 35: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/35.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.3 Characteristics of the interactions
o The peak temperatures reached in the interactions are typically 109 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 56Ni is produced, which may explain some underluminous transients.
![Page 36: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/36.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.4 Observational signatures
o Gravitational wave emission in the slow-motion, weak-field, 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 56Ni and 56Co 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).
![Page 37: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/37.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.4.1 Gravitational waves
Eccentric orbits
![Page 38: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/38.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.4.1 Gravitational waves
Lateral collisions
![Page 39: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/39.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.4.2 Light curves
![Page 40: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/40.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.4.3 Thermal neutrinos
![Page 41: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/41.jpg)
White dwarf dynamical interactions – E. García-Berro
4. WHITE DWARF COLLISIONS 4.4.4 Fallback luminosities
![Page 42: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/42.jpg)
White dwarf dynamical interactions – E. García-Berro
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.
![Page 43: White dwarf dynamical interactions Enrique García- …...White dwarf dynamical interactions – E. García-Berro 1. INTRODUCTION 1.2 Type Ia supernovae o Also known as thermonuclear](https://reader033.fdocuments.us/reader033/viewer/2022041705/5e447440c8d38909997e4e0b/html5/thumbnails/43.jpg)
White dwarf dynamical interactions
Enrique García-Berro
Jornades de Recerca, Departament de Física