Source: http://futur.upc.edu/179362
Timestamp: 2018-04-22 01:23:09+00:00

Document:
Garcia Senz, Domingo
DOMINGO.GARCIA UPC.EDU
0000-0001-5197-7100
Context. The optical light curve of Type Ia supernovae (SNIa) is powered by thermalized gamma-rays produced by the decay of 56Ni and 56Co, the main radioactive isotopes synthesized by the thermonuclear explosion of a C/O white dwarf. Aims. Gamma-rays escaping the ejecta can be used as a diagnostic tool for studying the characteristics of the explosion. In particular, it is expected that the analysis of the early gamma emission, near the maximum of the optical light curve, could provide information about the distribution of the radioactive elements in the debris. Methods. The gamma data obtained from SN2014J in M¿82 by the instruments on board INTEGRAL were analysed paying special attention to the effect that the detailed spectral response has on the measurements of the intensity of the lines. Results. The 158 keV emission of 56Ni has been detected in SN2014J at ~5s at low energy with both ISGRI and SPI around the maximum of the optical light curve. After correcting the spectral response of the detector, the fluxes in the lines suggest that, in addition to the bulk of radioactive elements buried in the central layers of the debris, there is a plume of 56Ni, with a significance of ~3s, moving at high velocity and receding from the observer. The mass of the plume is in the range of ~0.03-0.08 M¿. Conclusions. No SNIa explosion model has ever predicted the mass and geometrical distribution of 56Ni suggested here. According to its optical properties, SN2014J looks like a normal SNIa, so it is extremely important to discern whether it is also representative in the gamma-ray band.
Vol. 819, num. 2
DOI: 10.3847/0004-637X/819/2/132
La simulación mediante ordenador es una de las herramientas básicas de la Astrofísica moderna. Los procesos de gran escala temporal son imposibles de tratar con enfoques explícitos ya que estos se encuentran limitados, en su paso de tiempo máximo, por la restricción conocida como condición de Courant-Friedrichs-Lewy.Para utilizar los enfoques implícitos se genera un sistema de ecuaciones algebraicas acopladas, habitualmente resuelto con un esquema de Newton-Raphson y compuesto por todas las ecuaciones de cada uno de los puntos de resolución del modelo. El coste computacional de resolución aumenta sustancialmente con el número de incógnitas que han de determinarse a cada paso de tiempo. Las propiedades del siguiente paso de tiempo dependen de los valores de las variables desconocidas en dicho paso de tiempo y por tanto todas han de ser calculadas simultáneamente. La consecuencia es que todo el sistema de ecuaciones se ha de resolver conjuntamente realizando la inversión de una matriz dispersa enorme (la matriz es cuadrada y tiene un tamaño de n*v, siendo n el numero de partículas y v el número de variables independientes del sistema). Debido a esta restricción, la hidrodinámica implícita históricamente ha sido aplicada a sistemas en una sola dimensión.Para su implementación multidimensional sería interesante utilizar un enfoque lagrangiano como el suavizado de partículas hidrodinámicas denominado "Smooth Particle Hydrodynamics" ó SPH. La técnica se viene aplicando con éxito al campo de la astrofísica, la cosmología y diferentes problemas de la física de fluidos. El SPH integra las ecuaciones de la dinámica de fluidos en cada punto del formalismo lagrangiano (denominado partícula por tener una masa asociada) calculando velocidad, posición, densidad y presión como una interpolación de los valores de las partículas vecinas. Los métodos lagrangianos, a diferencia de los eulerianos, no necesitan de una malla regular que cubra la totalidad del espacio de integración, por tanto, la memoria y el tiempo de cálculo no se desperdician en la resolución de espacios vacíos. Los fluidos se descomponen en un conjunto de partículas donde podemos tratar numéricamente de forma más sencilla el movimiento en tres dimensiones derivado de las fuerzas de presión y auto-gravedad.El objetivo de esta tesis es detallar las principales características y la implementación de un nuevo código SPH, con un enfoque implícito, al que hemos denominado ISFAA (Implicit SPH for Astrophysical Applications). Este código amplia el trabajo previo de Knapp. C., 2000 e incluye el esquema físico más actual del SPH (basado en el principio variacional), viscosidad artificial, gravedad y conductividad térmica.Dado el enorme esfuerzo que supone construir y validar un nuevo código SPH, se pretende que en el futuro su utilidad se extienda al mayor número posible de escenarios. Con este fin se ha optado por un diseño modular que separe el tratamiento general del código de la implementación concreta de ecuaciones evolutivas básicas y de las propiedades del material (ecuación de estado, viscosidad artificial, etc.). Además, para la resolución del sistema de ecuaciones se utiliza la biblioteca de algoritmos paralelos PARDISO, que incorpora la librería Intel MKL y que en el futuro tendrá mejoras que impactarán positivamente en el código.Para comprobar la corrección del código y probar cada uno de los ingredientes físicos, se especifican una serie de test básicos (Explosión puntual, The wall heating shock, inestabilidades de Rayleigh-Taylor, caída libre, etc.) y una serie de test con gravedad (Toy Star, estabilización de una estrella de masa solar y una enana blanca).Por último se muestra la evolución de un sistema cuasiestático, en el que las velocidades no se encuentran explícitamente en el modelo. Este test está orientado a demostrar que el código implícito podría aplicarse con éxito en estas situaciones, consiguiendo simular el sistema en largos intervalos temporales.
Computational simulation is one of the basic techniques of modern Astrophysics. The long-term time astrophysical processes cannot be treated with explicit approaches because that they are limited, in their maximum time step, by the restriction known as Courant-Friedrichs-Lewy Condition. In order to use implicit approaches a system of coupled algebraic equations needs to be solved. It is composed by all the equations of each one of the discrete points of the model and the usual solution comes through a Newton-Raphson scheme. The computational cost substantially increases with the number of unknowns of the model. In implicit schemes the properties of the current time step depends on the values of the unknown variables at that time step, so everything has to be calculated simultaneously. The consequence is that all equations should be jointly solved inverting of a huge sparse matrix (it is a squared n*v matrix, being n the number of particles and v the number of independent variables of the system). Due to this restriction, historically the implicit hydrodynamics had been only applied to one-dimensional systems. It would be very interesting to build an Implicit hydrocode taking advantage of the so called Smoothed Particle Hydrodynamics or SPH. This technique has been being applied successfully in astrophysics and cosmology and fluid physics. SPH integrates the dynamic fluid equations in each point of the Lagragian formalism (named particles because they have an associated mass) calculating speed, position, density and pressure as interpolations from neighbour particles. Unlike Eulerian methods the Lagragian approach does not need from a rectangular grid covering the integration domain. Therefore storage and computing time is not wasted in void regions. Fluids are decomposed in a set of particles where the numerical treatment of the three-dimensional movement derived from pressure and auto-gravity is easier. The goal of this thesis is to describe the main features and the implementation of a new SPH code which uses implicit approach, called ISFAA (Implicit SPH for Astrophysical Applications). This code enlarges the previous work from "An Implicit Smooth Particle hydrodynamic Code", Knapp C. (2000) and recent developments of the SPH scheme (based on the variation principle), artificial viscosity, gravity and thermal conductivity. Because of the huge effort which has to be invested to build and validate the new SPH code, it is pretended that in the future its use can be extended to a large number of scenarios. With this end a modular design has been implemented that allows to separate the code general treatment, the particular implementation of the basic evolutionary equations and the physical properties (equation of state, artificial viscosity, etc.). Furthermore, to find the solution of the equations' system, the library of parallel algorithms PARDISO, embodied in the library Intel MKL, has been used. Future improvements in these libraries will have a positive impact on the new code. To validate the code and check each one of the physical ingredients, a set of basic tests (point-like explosion, The wall heating shock, Rayleigh-Taylor instabilities, Free-Fall collapse, etc) were run and analyzed as well as several tests incorporating gravity (Toy Star, stability of a solar mass star and a White Dwarf). And finally, we show the evolution of a single quasi-static system. To handle with these scenarios we have built a slightly different implicit scheme, were velocities are not explicitly included in the equations of movement. The main aim of this tests is to demonstrate that an implicit quasi-hydrostatic scheme is able to work with time-steps many orders of magnitude large (10^4) than the characteristic current Courant time.
La simulación mediante ordenador es una de las herramientas básicas de la Astrofísica moderna. Los procesos de gran escala temporal son imposibles de tratar con enfoques explícitos ya que estos se encuentran limitados, en su paso de tiempo máximo, por la restricción conocida como condición de Courant-Friedrichs-Lewy. Para utilizar los enfoques implícitos se genera un sistema de ecuaciones algebraicas acopladas, habitualmente resuelto con un esquema de Newton-Raphson y compuesto por todas las ecuaciones de cada uno de los puntos de resolución del modelo. El coste computacional de resolución aumenta sustancialmente con el número de incógnitas que han de determinarse a cada paso de tiempo. Las propiedades del siguiente paso de tiempo dependen de los valores de las variables desconocidas en dicho paso de tiempo y por tanto todas han de ser calculadas simultáneamente. La consecuencia es que todo el sistema de ecuaciones se ha de resolver conjuntamente realizando la inversión de una matriz dispersa enorme (la matriz es cuadrada y tiene un tamaño de n*v, siendo n el numero de partículas y v el número de variables independientes del sistema). Debido a esta restricción, la hidrodinámica implícita históricamente ha sido aplicada a sistemas en una sola dimensión. Para su implementación multidimensional sería interesante utilizar un enfoque lagrangiano como el suavizado de partículas hidrodinámicas denominado "Smooth Particle Hydrodynamics" ó SPH. La técnica se viene aplicando con éxito al campo de la astrofísica, la cosmología y diferentes problemas de la física de fluidos. El SPH integra las ecuaciones de la dinámica de fluidos en cada punto del formalismo lagrangiano (denominado partícula por tener una masa asociada) calculando velocidad, posición, densidad y presión como una interpolación de los valores de las partículas vecinas. Los métodos lagrangianos, a diferencia de los eulerianos, no necesitan de una malla regular que cubra la totalidad del espacio de integración, por tanto, la memoria y el tiempo de cálculo no se desperdician en la resolución de espacios vacíos. Los fluidos se descomponen en un conjunto de partículas donde podemos tratar numéricamente de forma más sencilla el movimiento en tres dimensiones derivado de las fuerzas de presión y auto-gravedad. El objetivo de esta tesis es detallar las principales características y la implementación de un nuevo código SPH, con un enfoque implícito, al que hemos denominado ISFAA (Implicit SPH for Astrophysical Applications). Este código amplia el trabajo previo de Knapp. C., 2000 e incluye el esquema físico más actual del SPH (basado en el principio variacional), viscosidad artificial, gravedad y conductividad térmica. Dado el enorme esfuerzo que supone construir y validar un nuevo código SPH, se pretende que en el futuro su utilidad se extienda al mayor número posible de escenarios. Con este fin se ha optado por un diseño modular que separe el tratamiento general del código de la implementación concreta de ecuaciones evolutivas básicas y de las propiedades del material (ecuación de estado, viscosidad artificial, etc.). Además, para la resolución del sistema de ecuaciones se utiliza la biblioteca de algoritmos paralelos PARDISO, que incorpora la librería Intel MKL y que en el futuro tendrá mejoras que impactarán positivamente en el código. Para comprobar la corrección del código y probar cada uno de los ingredientes físicos, se especifican una serie de test básicos (Explosión puntual, The wall heating shock, inestabilidades de Rayleigh-Taylor, caída libre, etc.) y una serie de test con gravedad (Toy Star, estabilización de una estrella de masa solar y una enana blanca). Por último se muestra la evolución de un sistema cuasiestático, en el que las velocidades no se encuentran explícitamente en el modelo. Este test está orientado a demostrar que el código implícito podría aplicarse con éxito en estas situaciones, consiguiendo simular el sistema en largos intervalos temporales.
Comunicación a la Unión Astronómica Internacional del descubrimiento de la supernova del tipo Ia SN2014J
High resolution-simulations of the head-on collisions of white dwarfs
Garcia, D.; Cabezon, R.; Arcones, A.; Relaño, A.; Thielemann, F.K.
Vol. 436, num. 4, p. 3413-3429
DOI: 10.1093/mnras/stt1821
Escartín, J.A.; Garcia, D.; Cabezón, R.M.
p. 874-879
We describe and check a novel formulation of Smoothed Particle Hydrodynamics (SPH) based on an Integral Approach to the Derivatives, called IAD0, that can be applied to simulate astrophysical systems. The method relies in a tensor approach to calculating gradients, which is more accurate than the standard procedure (STD), due to its better renormalization properties. The proposed scheme fully conserves momentum and energy in isentropic ows, and is less susceptible to the pairing instability. The resulting algorithm is veried using two tests: a two-dimensional simulation of the Kelvin-Helmholtz instability and the three-dimensional simulation of the merging of two polytropes. The analysis of these test cases suggests that the method is able to improve the results of the standard technique with only a moderate computational overload.
ISFAA, prospects for an implicit Smoothed Particle Hydrodynamics
Escartín, J.A.; Garcia, D.
A two-dimensional axisymmetric implementation of the smoothed particle hydrodynamics (SPH) technique, called for short AxisSPH, has been described in this thesis, along with a number of basic tests and realistic applications. The main goal of this work was to fill a gap on a topic which has been scarcely addressed in the published literature concerning SPH. Although the application of AxisSPH to the simulation of real problems is restricted to those systems which display the appropriate symmetry there are, however, many interesting examples of physical systems which evolve following the axisymmetric premise. These examples belong to a variety of scientific and technological areas such as, for example, astrophysics, laboratory astrophysics or inertial confinement fusion. Additionally AxisSPH can be also useful in convergence studies of the standard 3D-SPH technique because the higher resolution achieved in 2D can be used to benchmark the three-dimensional codes. The main improvements implemented in AxisSPH with respect existing axisymmetric SPH formulations are summarized as follows: 1) We have derived simple analytical expressions for correction factors which largely improves the calculation of density and velocity in the vicinity of the z-axis. These expressions and their derivatives were given as a function of an adimensional parameter and do not increase the computational load of the scheme. 2) We have obtained the appropriate expression of the fluid Euler equations containing the new correction functions and their derivatives. Far enough from the singular axis, the scheme reduces to the standard formulation discussed by Brookshaw (2003). 3) A novel expression for the heat conduction term, which has to be added to the energy equation was devised and checked. This new term improves the description of the heat flux for those particles located at the axis neighborhoods. 4) Until now axisymmetric SPH hydrocodes handle artificial viscosity using a crude approach because it was treated as a simple restriction of the standard 3D Cartesian viscosity to 2D. Here we propose to calculate the viscous pressure as a combination of two terms, the first one is the (standard) Cartesian part and the second is the axis-converging part of the viscosity respectively. As expected this last term is of special relevance to simulate implosions. 5) We have developed an original method to incorporate gravity into AxisSPH. First the direct ring to ring force was found as a function of the Euclidean distance between the 2D particles. In second place the gravitational force on a given particle was obtained by summing the contributions of all N particles. We have also developed a more efficient scheme to obtain the gravitational force calculating the potential of the ring, instead the force because it involves lesser algebraic operations. The scheme has been checked using a large number of tests cases. These tests range from very specific oriented to check a particular algorithm or a piece of physics, to rather complex ones intended to analyze the behavior of the scheme in potential real applications (ICF, jets, astrophysics). At least in one case, the head on collision of a pair of white dwarfs, the result of the simulations carried out using AxisSPH brings new, unpublished, scientific material.
En esta tesis se ha desarrollado un código, que hemos llamado AxisSPH, en dos dimensiones axisimétrico a partir de la técnica conocida como SPH (“smooothed particle hydrodynamics”). AxisSPH ha sido validado después de realizar una serie de tests básicos y algunas simulaciones de situaciones reales. El objetivo principal de este trabajo ha sido llenar, en parte, el vacío existente al respecto en la literatura sobre SPH. Aunque sólo se puede aplicar AxisSPH en problemas reales que presenten la apropiada simetría, existen muchos ejemplos interesantes de sistemas físicos que presentan la simetría axial demandada. Existen ejemplos en campos de aplicación tanto científica como tecnológica, por ejemplo en astrofísica, en el llamado laboratorio de astrofísica o en fusión por confinamiento inercial (ICF). Otra interesante aplicación de AxisSPH puede ser su utilización en estudios de convergencia con otros códigos 3D-SPH debido a su mayor resolución, al tratarse de un código 2D. Las mejoras implementadas en el código AxisSPH en comparación con otros códigos axisimétricos SPH existentes se pueden resumir en los siguientes puntos: 1) Hemos deducido expresiones analíticas simples para unos factores de corrección que mejoran el cálculo de la densidad y la velocidad en las proximidades del eje z. Dichas expresiones y sus derivadas dependen de un parámetro adimensional que no incrementa mucho el peso computacional del esquema propuesto. 2) Hemos obtenido las expresiones adecuadas de las ecuaciones de Euler que contienen estas nuevas funciones correctoras y sus derivadas. Lejos del eje de singularidad estas ecuaciones se transforman en las de la formulación estándar propuesta por Brookshaw (2003). 3) Una expresión novedosa del término de conducción, que debe de añadirse a la ecuación de la energía, se ha propuesto y validado. Este nuevo término mejora la evolución del flujo de calor de las partículas situadas en las proximidades del eje z. 4) Hasta el momento los códigos hidrodinámicos SPH axisimétricos existentes trabajaban con una aproximación poco elaborada de la viscosidad artificial ya que consistían en una restricción a dos dimensiones de la viscosidad estándar 3D. En este trabajo proponemos el cálculo de la presión debida a la viscosidad como combinación de dos términos, el primero reflejo de la parte cartesiana y la segunda da cuenta de la parte relacionada con la convergencia en el eje. Como era de esperar este último término es de relevante importancia en la simulación de implosiones. 5) Hemos desarrollado un método original para incorporar el cálculo de la gravedad en el código AxisSPH. En primer lugar la fuerza directa de anillo a anillo y en segundo lugar la fuerza de la gravedad que sufre una determinada partícula a partir de la contribución del resto de las N partículas existentes. También hemos desarrollado un esquema más eficiente para calcular la gravedad a partir del cálculo del potencial del anillo en lugar del cálculo directo de la fuerza ya que implica un menor número de operaciones algebraicas. El método ha sido verificado con un gran número de test numéricos. Desde los más específicos orientados a comprobar la validez de un algoritmo particular o la capacidad para simular un fenómeno físico en particular, hasta simulaciones bastante más complejas, con la intención de validar la capacidad de simular aplicaciones potencialmente más reales (ICF, jets, astrofísica). Así, en al menos un caso, en la colisión frontal de dos enanas blancas, los resultados de la simulación utilizando AxisSPH pueden aportar material científico publicable.
Garcia, D.; Badenes, C.; Serichol, N.
Vol. 745, num. 1, p. 1-14
DOI: 10.1088/0004-637X/745/1/75
In this paper, we report on the bulk features of the hole carved by the companion star in the material ejected during a Type Ia supernova (SN Ia) explosion. In particular we are interested in the long-term evolution of the hole as well as in its fingerprint in the geometry of the supernova remnant (SNR) after several centuries of evolution, which is a hot topic in current SN Ia studies. We use an axisymmetric smoothed particle hydrodynamics code to characterize the geometric properties of the SNR resulting from the interaction of this ejected material with the ambient medium.Our aim is to use SNR observations to constrain the single degenerate scenario for SN Ia progenitors. Our simulations show that the hole will remain open during centuries, although its partial or total closure at later times due to hydrodynamic instabilities is not excluded. Close to the edge of the hole, the Rayleigh–Taylor instability grows faster, leading to plumes that approach the edge of the forward shock.We also discuss other geometrical properties of the simulations, like the evolution of the contact discontinuity.
Garcia-berro, E.; Diaz-Aguilo, M.; Renedo, I.; Sala, G.; Escartin, J.; Loren, P.; Garcia, D.; Torres, S.; Camacho, J.; Longland, R.L.
ISFAA, prospects for an implicit SPH
Escartín, A.; Garcia, D.; Cabezón, R.
International Spheric Workshop
The method known as Smoothed Particle Hydrodynamics (SPH) is an important tool in modern numerical Astrophysics. It has been extensively used to simulate a large number of systems ranging from planets to clusters of galaxies. Nevertheless current applications of the method are restricted to dynamical situations because of the limitations in the time-step imposed by the Courant condition. Here we describe the main features of a new implicit SPH code which is able to handle with several thousand particles and, therefore, it can be used to simulate slowly evolving systems.
Hydrodynamical simulations of DNS systems: gravitational emission and equation of state
Observational evidences point to a common explosion mechanism of Type Ia supernovae based on a delayed detonation of a white dwarf (WD). Although several scenarios have been proposed and explored by means of one, two, and three-dimensional simulations, the key point still is the understanding of the conditions under which a stable detonation can form in a destabilized WD. One of the possibilities that have been invoked is that an inefficient deflagration leads to the pulsation of a Chandrasekhar-mass WD, followed by formation of an accretion shock around a carbon-oxygen rich core. The accretion shock confines the core and transforms kinetic energy from the collapsing halo into thermal energy of the core, until an inward moving detonation is formed. This chain of events has been termed Pulsating Reverse Detonation (PRD). In this work we explore the robustness of the detonation ignition for different PRD models characterized by the amount of mass burned during the deflagration phase, Mdefl. The evolution of the WD up to the formation of the accretion shock has been followed with a three-dimensional hydrodynamical code with nuclear reactions turned off. We found that detonation conditions are achieved for a wide range of Mdefl. However, if the nuclear energy released during the deflagration phase is close to the WD binding energy (~0.46 × 1051 erg ¿ Mdefl ~ 0.30 M¿) the accretion shock cannot heat and confine the core efficiently and detonation conditions are not robustly achieved.
Observational evidences point to a common explosion mechanism of Type Ia supernovae based on a delayed detonation of a white dwarf (WD). However, all attempts to ¿nd a convincing ignition mechanism based on a delayed detonation in a destabilized, expanding, white dwarf have been elusive so far. One of the possibilities that has been invoked is that an inef¿cient de¿agration leads to pulsation of a Chandrasekhar-mass WD, followed by formation of an accretion shock that con¿nes a carbon–oxygen rich core, while transforming the kinetic energy of the collapsing halo into thermal energy of the core, until an inward moving detonation is formed. This chain of events has been termed Pulsating Reverse Detonation (PRD). In this work, we present three-dimensional numerical simulations of PRD models from the time of detonation initiation up to homologous expansion. Different models characterized by the amount of mass burned during the de¿agration phase, Mde¿, give explosions spanning a range of kinetic energies, K ~ (1.0–1.2)×1051 erg, and 56Ni masses, M(56Ni) ~ 0.6–0.8 M , which are compatible with what is expected for typical Type Ia supernovae. Spectra and light curves of angle-averaged spherically symmetric versions of the PRD models are discussed. Type Ia supernova spectra pose the most stringent requirements on PRD models.
Observational evidences point to a common explosion mechanism of Type Ia supernovae based on a delayed detonation of a white dwarf (WD). However, all attempts to ﬁnd a convincing ignition mechanism based on a delayed detonation in a destabilized, expanding, white dwarf have been elusive so far. One of the possibilities that has been invoked is that an inefﬁcient deﬂagration leads to pulsation of a Chandrasekhar-mass WD, followed by formation of an accretion shock that conﬁnes a carbon–oxygen rich core, while transforming the kinetic energy of the collapsing halo into thermal energy of the core, until an inward moving detonation is formed. This chain of events has been termed Pulsating Reverse Detonation (PRD). In this work, we present three-dimensional numerical simulations of PRD models from the time of detonation initiation up to homologous expansion. Different models characterized by the amount of mass burned during the deﬂagration phase, Mdeﬂ, give explosions spanning a range of kinetic energies, K ∼ (1.0–1.2)×1051 erg, and 56Ni masses, M(56Ni) ∼ 0.6–0.8 M , which are compatible with what is expected for typical Type Ia supernovae. Spectra and light curves of angle-averaged spherically symmetric versions of the PRD models are discussed. Type Ia supernova spectra pose the most stringent requirements on PRD models.
The axisymmetric form of the hydrodynamic equations within the smoothed particle hydrodynamics (SPH) formalism is presented and checked using idealized scenarios taken from astrophysics (free fall collapse, implosion and further pulsation of a Sun-like star), gas dynamics (wall heating problem, collision of two streams of gas) and inertial confinement fusion (ablative implosion of a small capsule). New material concerning the standard SPH formalism is given. That includes the numerical handling of those mass points which move close to the singularity axis, more accurate expressions for the artificial viscosity and the heat conduction term and an easy way to incorporate self-gravity in the simulations. The algorithm developed to compute gravity does not rely in any sort of grid, leading to a numerical scheme totally compatible with the Lagrangian nature of the SPH equations.
A displayer of stellar hydrodynamics processes
Escartin, J.; Garcia, D.
Data de presentació: 2008-07-08
Deflagration models poorly explain the observed diversity of SNIa. Current multidimensional simulations of SNIa predict a significant amount of, so far unobserved, carbon and oxygen moving at low velocities. It has been proposed that these drawbacks can be resolved if there is a sudden jump to a detonation (delayed detonation), but these kinds of models have been explored mainly in one dimension. Here we present new three-dimensional delayed detonation models in which the deflagraton-to-detonation transition (DDT) takes place in conditions like those favored by one-dimensional models. Methods. We have used a smoothed-particle-hydrodynamics code adapted to follow all the dynamical phases of the explosion, with algorithms devised to handle subsonic as well as supersonic combustion fronts. The starting point was a centrally ignited C–O white dwarf of 1.38 M. When the average density on the flame surface reached ~2-3 × 107 g cm-3 a detonation was launched. Results. The detonation wave processed more than 0.3 M of carbon and oxygen, emptying the central regions of the ejecta of unburned fuel and raising its kinetic energy close to the fiducial 1051 erg expected from a healthy type Ia supernova. The final amount of 56Ni synthesized also was in the correct range. However, the mass of carbon and oxygen ejected is still too high. Conclusions. The three-dimensional delayed detonation models explored here show an improvement over pure deflagration models, but they still fail to coincide with basic observational constraints. However, there are many aspects of the model that are still poorly known (geometry of flame ignition, mechanism of DDT, properties of detonation waves traversing a mixture of fuel and ashes). Therefore, it will be worth pursuing its exploration to see if a good SNIa model based on the three-dimensional delayed detonation scenario can be obtained.
Aims. Deflagration models poorly explain the observed diversity of SNIa. Current multidimensional simulations of SNIa predict a significant amount of, so far unobserved, carbon and oxygen moving at low velocities. It has been proposed that these drawbacks can be resolved if there is a sudden jump to a detonation (delayed detonation), but these kinds of models have been explored mainly in one dimension. Here we present new three-dimensional delayed detonation models in which the deflagraton-to-detonation transition (DDT) takes place in conditions like those favored by one-dimensional models. Methods. We have used a smoothed-particle-hydrodynamics code adapted to follow all the dynamical phases of the explosion, with algorithms devised to handle subsonic as well as supersonic combustion fronts. The starting point was a centrally ignited C–O white dwarf of 1.38 M . When the average density on the flame surface reached ∼2−3 × 107 g cm−3 a detonation was launched. Results. The detonation wave processed more than 0.3 M of carbon and oxygen, emptying the central regions of the ejecta of unburned fuel and raising its kinetic energy close to the fiducial 1051 erg expected from a healthy type Ia supernova. The final amount of 56Ni synthesized also was in the correct range. However, the mass of carbon and oxygen ejected is still too high. Conclusions. The three-dimensional delayed detonation models explored here show an improvement over pure deflagration models, but they still fail to coincide with basic observational constraints. However, there are many aspects of the model that are still poorly known (geometry of flame ignition, mechanism of DDT, properties of detonation waves traversing a mixture of fuel and ashes). Therefore, it will be worth pursuing its exploration to see if a good SNIa model based on the three-dimensional delayed detonation scenario can be obtained.
We calculate detailed non-LTE synthetic spectra of a pulsating reverse detonation (PRD) model, a novel explosion mechanism for Type Ia supernovae. While the hydro models are calculated in three dimensions, the spectra use an angle-averaged hydro model and thus some of the three-dimensional (3D) details are lost, but the overall average should be a good representation of the average observed spectra. We study the model at three epochs: maximum light, 7 days prior to maximum light, and 5 days after maximum light. At maximum the defining Si II feature is prominent, but there is also a prominent C II feature, not usually observed in normal SNe Ia near maximum. We compare to the early spectrum of SN 2006D, which did show a prominent C II feature, but the fit to the observations is not compelling. Finally, we compare to the postmaximum UV+optical spectrum of SN 1992A. With the broad spectral coverage it is clear that the iron-peak elements on the outside of the model push too much flux to the red and thus the particular PRD realizations studied would be intrinsically far redder than observed SNe Ia. We briefly discuss variations that could improve future PRD models.
The merging of white dwarf and neutron star systems: gravitational radiation
Garcia, D.; Garcia-berro, E.; Pedemonte, A.; Loren-Aguilar, P.; Isern, J.; Lobo, J.
Vol. 66, num. 1, p. 1-10
Ajuts per a equipament i infraestructura destinats a la recerca: SAI i sis ordinadors
Garcia, D.; Bravo, E.; Cabezón, R.; Woosley, S.
Vol. 660, num. 1, p. 509-515
DOI: 10.1086/513177
The physical structure of a nuclear flame is a basic ingredient of the theory of Type Ia supernovae (SNe Ia). Assuming an exponential density reduction with several characteristic times, we have followed the evolution of a planar nuclear flame in an expanding background from an initial density of 6.6 × 107 g cm-3 down to 2 × 106 g cm-3. The total amount of synthesized intermediate-mass elements (IMEs), from silicon to calcium, was monitored during the calculation. We have used the computed mass fractions, XIME, of these elements to estimate the total amount of IMEs synthesized during the deflagration of a massive white dwarf. Using XIME and adopting the usual hypothesis that the relevant flame speed is actually the turbulent speed on the integral length scale, we have built a simple geometrical approach to model the region where IMEs are thought to be produced. It turns out that a healthy production of IMEs involves the combination of not-too-short expansion times, tc = 0.2 s, and high turbulent intensities. According to our results, it could be difficult to produce much more than 0.2 M¿ of intermediate-mass elements within the standard deflagrative paradigm. The calculations also suggest that the mass of the IMEs scales with the mass of the Fe-peak elements, making it difficult to reconcile energetic explosions with low ejected nickel masses, as in the well-observed supernova SN 1991bg or in SN 1998de. Thus, a large production of Si-peak elements, especially in combination with a low or moderate production of iron, could be better addressed either by the delayed detonation route in standard Chandrasekhar-mass models or, perhaps, by the off-center helium detonation in the sub-Chandrasekhar-mass scenario.
The physical structure of a nuclear flame is a basic ingredient of the theory of Type Ia supernovae (SNe Ia). Assuming an exponential density reduction with several characteristic times, we have followed the evolution of a planar nuclear flame in an expanding background from an initial density of 6.6 × 107 g cm-3 down to 2 × 106 g cm-3. The total amount of synthesized intermediate-mass elements (IMEs), from silicon to calcium, was monitored during the calculation. We have used the computed mass fractions, XIME, of these elements to estimate the total amount of IMEs synthesized during the deflagration of a massive white dwarf. Using XIME and adopting the usual hypothesis that the relevant flame speed is actually the turbulent speed on the integral length scale, we have built a simple geometrical approach to model the region where IMEs are thought to be produced. It turns out that a healthy production of IMEs involves the combination of not-too-short expansion times, τc ≥ 0.2 s, and high turbulent intensities. According to our results, it could be difficult to produce much more than 0.2 M☉ of intermediate-mass elements within the standard deflagrative paradigm. The calculations also suggest that the mass of the IMEs scales with the mass of the Fe-peak elements, making it difficult to reconcile energetic explosions with low ejected nickel masses, as in the well-observed supernova SN 1991bg or in SN 1998de. Thus, a large production of Si-peak elements, especially in combination with a low or moderate production of iron, could be better addressed either by the delayed detonation route in standard Chandrasekhar-mass models or, perhaps, by the off-center helium detonation in the sub-Chandrasekhar-mass scenario.
Velarde, P.; González, M.; Oliva, E.; Kasperczuk, A.; Pisarczyk, T.; Ullschmied, J.; Stehlé, C.; Rus, B.; Garcia, D.; Bravo, E.; Relaño, A.
5th International conference on inertial fusion sciences and applications : September 9-14, 2007 : Kobe, Japan
Hernanz, M.; Dominguez, I.; Garcia-berro, E.; Garcia, D.; Barstow, M.; Bravo, E.; Gonzalez-Riestra, R.; Isern, J.; Jose, J.; Torres, S.
Velarde, P.; Garcia, D.; Bravo, E.; Ogando, F.; Relaño, A.; Oliva, E.
Vol. 13, num. 092901, p. 1-10
The evolution of supernova remnants (SNRs) represents a useful and natural laboratory for gasdynamics studies. In this paper the results of several hydrodynamical simulations of the propagation and early phases of interaction of two SNRs embedded in a homogeneous interstellar environment are shown. In particular, the hydrodynamic evolution and collision of twin SNRs during their self-similar stage has been simulated using a two-dimensional Lagrangian hydrocode. In addition, the results of a detailed simulation that attempts to set the adequate conditions to reproduce the same phenomenon through laser ablation of two plastic plugs at the laboratory scale are presented. These results indicate that both large-scale and small-scale simulations display several common features that can be used to design an experiment aimed to validate the hydrodynamical codes. Of particular interest are the structures found around the juncture of the two colliding shells produced by the interaction of the remnants.
Single point off-center helium ignitions as origin of some type la supernovae
Data de presentació: 2006-06-28
Velarde, P.; Garcia, D.; Bravo, E.; Ogando, F.; Relaño, A.; González, E.; Lachaise, M.; Oliva, E.
Vol. 133, p. 1035-1037
The stagnation phase of an ICF capsule simulated with an axisymmetrical smoothed-particle hydrodynamics code
29th European Conference on Laser Interaction with Matter
Data de presentació: 2006-05-12
Vol. 642, num. 2, p. L157-L160
We describe a mechanism by which a failed deflagration of a Chandrasekhar-mass carbon-oxygen white dwarf can turn into a successful thermonuclear supernova explosion, without invoking an ad hoc high-density deflagration-detonation transition. Following a pulsating phase, an accretion shock develops above a core of 1 M_sun composed of carbon and oxygen, inducing a converging detonation. A three-dimensional simulation of the explosion produced a kinetic energy of 1.05E51 ergs and 0.70 M_sun of 56Ni, ejecting scarcely 0.01 M_sun of C-O moving at low velocities. The mechanism works under quite general conditions and is flexible enough to account for the diversity of normal Type Ia supernovae. In given conditions the detonation might not occur, which would reflect in peculiar signatures in the gamma and UV-wavelengths.
Forcada, R.; Garcia, D.; Jose, J.
Astrophysics and space science 3
New astronomy reviews 1
Universo (Barcelona) 1
Bravo Guil, Eduardo 61
Garcia-berro Montilla, Enrique 22
José Pont, Jordi 21
Cabezón Gómez, Rubén Martín 16
Hernanz Carbó, Margarita 10
Isern Vilaboy, Jordi 9
Escartin Vigo, Jose Antonio 8
Parikh, Anuj Ramesh 8
Sala Cladellas, Gloria 8
Serichol Augue, Nuria 7
Isern Vilaboy, Jorge 6
Relaño, A 6
Badenes Montoliu, Carles 5
Domínguez Aguilera, Inmaculada 5
Gutierrez Cabello, Jorge Luis 5
Cabezon Gomez, Ruben Martin 4
Campos Costa Marreiros Figueira, Joana 4
GAA - Grup d'Astronomia i Astrofísica 124
GRPFM - Grup de Recerca en Propietats Físiques dels Materials 61
GREENER - Grup de recerca d´estudis energètics i de les radiacions 2
Departament de Física i Enginyeria Nuclear 120
Facultat d'Informàtica de Barcelona (FIB) 102

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