Axisymmetric smoothed particle hydrodynamics with self-gravity

Garcı́a-Senz, Domingo; Relaño, A.; Cabezón, Rubén M.; Bravo, Eduardo

doi:10.1111/j.1365-2966.2008.14058.x

Cited by 21 publications

(35 citation statements)

References 21 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We carried out the simulations with the axisymmetric SPH hydrocode AxisSPH, described in García-Senz et al (2008), which incorporates a new algorithm to solve the contribution of gravity in the axisymmetric SPH paradigm. The scheme calculates gravity by computing the direct interaction between any pair of particles, each of them approximated as a toroidal distribution of mass.…”

Section: Hydrodynamic Methods and Initial Settingmentioning

confidence: 99%

“…Simulations were carried out using an axisymmetric smoothed particle hydrodynamics (SPH) code developed recently, García-Senz et al (2008). Because it was not possible to simulate the evolution over the large dynamic range in time between the collision and the fully developed SNR phase (minutes to thousands of years), we divided the process in three stages.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

IS THERE A HIDDEN HOLE IN TYPE Ia SUPERNOVA REMNANTS?

Garcı́a-Senz

Badenes

Serichol³

2011

ApJ

Self Cite

View full text Add to dashboard Cite

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.

show abstract

Section: Hydrodynamic Methods and Initial Settingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

IS THERE A HIDDEN HOLE IN TYPE Ia SUPERNOVA REMNANTS?

Garcı́a-Senz

Badenes

Serichol³

2011

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…The hydrocode AxisSPH is a two-dimensional SPH code written in axisymmetric geometry which incorporates several improvements over existing versions of these hydrodynamic codes (García-Senz et al 2009). Its main advantage relies in the more accurate treatment of particles moving close to the symmetry z-axis which is a singular line.…”

Section: Appendix A: Main Features Of Axissphmentioning

confidence: 99%

High-resolution simulations of the head-on collision of white dwarfs

Garcı́a-Senz

Cabezón

Arcones

et al. 2013

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

The direct impact of white dwarfs has been suggested as a plausible channel for type Ia supernovae. In spite of their (a priori) rareness, in highly populated globular clusters and in galactic centers, where the amount of white dwarfs is considerable, the rate of violent collisions between two of them might be non-negligible. Even more, there are indications that binary white dwarf systems orbited by a third stellar-mass body have an important chance to induce a clean head-on collision. Therefore, this scenario represents a source of contamination for the supernova light-curves sample that it is used as standard candles in cosmology, and it deserves further investigation. Some groups have conducted numerical simulations of this scenario, but their results show several differences. In this paper we address some of the possible sources of these differences, presenting the results of high resolution hydrodynamical simulations jointly with a detailed nuclear post-processing of the nuclear abundances, to check the viability of white dwarf collisions to produce significant amounts of 56 Ni. To that purpose, we use a 2D-axial symmetric smoothed particle hydrodynamic code to obtain a resolution considerably higher than in previous studies. In this work, we also study how the initial mass and nuclear composition affect the results. The gravitational wave emission is also calculated, as this is a unique signature of this kind of events. All calculated models produce a significant amount of 56 Ni, ranging from 0.1 M ⊙ to 1.1 M ⊙ , compatible not only with normal-Branch type Ia supernova but also with the subluminous and super-Chandrasekhar subset. Nevertheless, the distribution mass-function of white dwarfs favors collisions among 0.6 − 0.7 M ⊙ objects, leading to subluminous events.

show abstract

“…The fluid axisymmetric SPH scheme implemented in the present study uses a corrective function for density calculation near the symmetry axis. Further, the density correction leads to a corrected momentum equation [22].…”

Section: Fluid Solvermentioning

confidence: 99%

SPH modelling of a cavitation bubble collapse near an elasto-visco-plastic material

Joshi

Franc

Ghigliotti

et al. 2019

Journal of the Mechanics and Physics of Solids

View full text Add to dashboard Cite

A Smoothed Particle Hydrodynamics axisymmetric solver was developed in order to simulate the collapse of a single cavitation bubble close to an elastic-plastic material and study plasticity formation and hence material erosion. Findings indicate the relative importance of the material deformation due to the impact of the micro-jet and the shock wave that develop during collapse. A shock-wave dominated impact has a much higher material erosion ability compared to a micro-jet impact. Strain rate is found to have a significant effect on plastic deformation, with an overestimation of the plastic deformation up to 60% if strain rate effects are neglected in the case of stainless steel A2205. We also demonstrate that, although the impact pressure is maximum just below the collapsing bubble, maximum plastic strain occurs at a radial offset from the symmetry axis. This is the result of inertial effects that have an impact on both the magnitude and the position of the plastic domain in the material. A new non-dimensional parameter called effective pressure is introduced that can predict plastic strain location accurately for higher stand-off ratios. Alternatively, a characteristic time analysis also shows that it can be used for prediction of plastic strain zone in the solid for detached cavities.

show abstract

Axisymmetric smoothed particle hydrodynamics with self-gravity

Cited by 21 publications

References 21 publications

IS THERE A HIDDEN HOLE IN TYPE Ia SUPERNOVA REMNANTS?

IS THERE A HIDDEN HOLE IN TYPE Ia SUPERNOVA REMNANTS?

High-resolution simulations of the head-on collision of white dwarfs

SPH modelling of a cavitation bubble collapse near an elasto-visco-plastic material

Contact Info

Product

Resources

About