scholarly journals The infancy of supernova remnants: evolving a supernova into its remnant in 3D

2017 ◽  
Vol 12 (S331) ◽  
pp. 141-147 ◽  
Author(s):  
Michael Gabler ◽  
Hans-Thomas Janka ◽  
Annop Wongwathanarat
Keyword(s):  
Supernova Remnants ◽  
Supernova Explosion ◽  
Observational Constraints ◽  
Late Time ◽  
First Principle ◽  
Self Consistent ◽  
Supernova Explosions ◽  
Explosion Mechanism ◽  
Cas A

AbstractRecently, first neutrino-driven supernova explosions have been obtained in 3D, self-consistent, first-principle simulations, these models are still not always exploding robustly and, in general, the explosions are not sufficiently energetic. To constrain the explosion mechanism, and the related uncertainties, it is thus very helpful to consider observational constraints: pulsar kicks, progenitor association and supernova remnants (SNR). Recent observations of asymmetries in the supernova ejecta of Cas A are very promising, to compare to long-term simulations of the explosion. In addition 3D observations of SN87A are becoming more constraining on the geometry of the ejected material during the explosion. In this talk I will discuss our efforts to model the late time evolution of a 3D supernova explosion, where we include the effects of beta decay, which inflates the structures rich in 56Ni. The structures we find in the simulations depend on the quantities plotted.

scholarly journals Light-Echo Spectrum Reveals the Type of Tycho Brahe's 1572 Supernova

2011 ◽  
Vol 7 (S281) ◽  
pp. 335-336
Author(s):  
T. Usuda ◽  
O. Krause ◽  
M. Tanaka ◽  
T. Hattori ◽  
M. Goto ◽  
...  
Keyword(s):  
Supernova Remnants ◽  
Three Dimensional ◽  
Supernova Explosion ◽  
Cassiopeia A ◽  
Type Ia ◽  
Light Echoes ◽  
Explosion Mechanism ◽  
Cas A ◽  
Ia Supernovae ◽  
Insight Into

AbstractWe successfully obtained the first optical spectra of the faint light echoes around Cassiopeia A and Tycho Brahe's supernova remnants (SNRs) with FOCAS and the Subaru Telescope. We conclude that Cas A and Tycho's SN 1572 belong to the Type IIb and normal Type Ia supernovae, respectively. Light echo spectra are important in order to obtain further insight into the supernova explosion mechanism of Tycho's SN 1572: how the Type Ia explosion actually proceeds, and whether accretion occurs from a companion or by the merging of two white dwarfs. The proximity of the SN 1572 remnant has allowed detailed studies, such as the possible identification of the binary companion, and provides a unique opportunity to test theories of the explosion mechanism and the nature of the progenitor. Future light-echo spectra, obtained in different spatial directions of SN 1572, will enable to construct a three-dimensional spectroscopic view of the explosion.

NEUTRINO CAPTURE INDUCED SUPERNOVA EXPLOSIONS

2010 ◽  
Vol 19 (08n10) ◽  
pp. 1483-1490 ◽  
Author(s):  
T. STROTHER ◽  
W. BAUER
Keyword(s):  
Kinetic Theory ◽  
Heavy Ion Collisions ◽  
Supernova Explosion ◽  
Heavy Ion ◽  
High Energy ◽  
Transport Equations ◽  
Core Collapse ◽  
Ion Collisions ◽  
Supernova Explosions ◽  
Explosion Mechanism

Motivated by the success of kinetic theory in the description of observables in intermediate and high energy heavy-ion collisions, we use kinetic theory to model the dynamics of core collapse supernovae. The specific way that we employ kinetic theory to solve the relevant transport equations allows us to explicitly model the propagation of neutrinos and a full ensemble of nuclei and treat neutrino–matter interactions in a very general way. With these abilities, our simulations have observed dynamics that may prove to be an entirely new neutrino capture induced supernova explosion mechanism.

scholarly journals The Early Evolution of Supernova Remnants

1986 ◽  
Vol 89 ◽  
pp. 141-165
Author(s):  
Claes Fransson
Keyword(s):  
Supernova Remnants ◽  
Supernova Remnant ◽  
Supernova Explosion ◽  
Early Evolution ◽  
Interesting Aspect ◽  
Free Expansion ◽  
Expansion Phase ◽  
Cas A ◽  
New Instruments ◽  
Infrared Telescopes

In his review in 1972 Woltjer [1] divided the evolution of supernova remnants into three different phases, the free expansion phase, the adiabatic Sedov phase and the radiative phase, when cooling of the gas becomes important. The first of these was only briefly discussed and little connection between the supernova explosion and the remnant phase was made. The reason for this is also easy to understand in view of the difficulty of determining the type of explosion even for well-known, young remnants like Cas A, Tycho, Kepler and the Crab remnant.This situation has changed considerably during the last five years or so, mainly due to observations with new instruments like VLA, IUE and Einstein. With these, as well as large optical and infrared telescopes, the information about the supernova explosion and the early evolution of the supernova remnant has increased dramatically, and a more or less new picture of the explosion has emerged. Instead of a free expansion into a virtual vacuum, with few observational consequences, the supernova undergoes a complex interaction with its immediate surroundings, with a wealth of observational information. In this stage both the structure of the supernova ejecta and the circumstellar medium is crucial for the observational properties. Perhaps, the most interesting aspect of it is that we in this way can bridge the gap between the supernova explosion and the remnant stage.

scholarly journals Supernova remnants dynamics

2017 ◽  
Vol 12 (S331) ◽  
pp. 164-173
Author(s):  
Anne Decourchelle
Keyword(s):  
Supernova Remnants ◽  
Surrounding Medium ◽  
Supernova Explosion ◽  
Large Set ◽  
Reverse Shock ◽  
Field Amplification ◽  
Shock Heating ◽  
Forward Shock ◽  
Explosion Mechanism ◽  
Domain I

AbstractSupernova remnants are the site of a number of physical processes (shock-heating, non-equilibrium ionization, hydrodynamic instabilities, particle acceleration, magnetic field amplification). Their related emission processes provide us with a large set of observational data. Supernova remnants result from the interaction of high-velocity material ejected by the supernova explosion with the medium surrounding the progenitor star. This interaction gives rise to a double-shock structure that lasts for hundreds of years, with a forward shock and a reverse shock compressing and heating to tens million of degrees the surrounding medium and the ejecta, respectively. It is mostly in this phase that young supernova remnants provide information on their explosion mechanism through spectro-imaging observations of the ejected nucleosynthesis products and their dynamics, notably in the X-ray domain. I will review these observations and their implications for our current understanding of the dynamics of supernova remnants. I will conclude on the prospects with future facilities.

scholarly journals Thermonuclear Supernova Explosions and Their Remnants: The Case of Tycho

2005 ◽  
Vol 192 ◽  
pp. 233-238
Author(s):  
Carles Badenes ◽  
Eduardo Bravo ◽  
Kazimierz J. Borkowski
Keyword(s):  
Supernova Remnants ◽  
Relevant Information ◽  
Type Ia Supernovae ◽  
Test Case ◽  
X Ray ◽  
Type Ia ◽  
Supernova Explosions ◽  
Explosion Mechanism ◽  
Ia Supernovae ◽  
The Impact

SummaryWe propose to use the thermal X-ray emission from young supernova remnants (SNRs) originated in Type Ia supernovae (SNe) to extract relevant information concerning the explosion mechanism. We focus on the differences between numerical 1D and 3D explosion calculations, and the impact that these differences could have on the modeling of young SNRs. We use the remnant of the Tycho supernova (SN 1572) as a test case to compare with our predictions, discussing the observational features that allow to accept or discard a given model.

scholarly journals Long-term evolution of surviving companion stars of Type Iax supernovae

2020 ◽  
Vol 500 (1) ◽  
pp. 301-309
Author(s):  
Zheng-Wei Liu ◽  
Yaotian Zeng
Keyword(s):  
Stellar Evolution ◽  
Main Sequence ◽  
Three Dimensional ◽  
Late Time ◽  
One Dimensional ◽  
Term Evolution ◽  
Post Impact ◽  
Explosion Mechanism ◽  
Hydrodynamical Simulations

ABSTRACT The nature of the progenitors and explosion mechanism of Type Iax supernovae (SNe Iax) remain a mystery. The single-degenerate (SD) systems that involve the incomplete pure deflagration explosions of near-Chandrasekhar-mass white dwarfs (WDs) have recently been proposed for producing SNe Iax in which non-degenerate companions are expected to survive from SN explosions. In this work, we concentrate on the main-sequence (MS) donor SD progenitor systems. By mapping the computed companion models from three-dimensional hydrodynamical simulations of ejecta-companion interaction into a one-dimensional stellar evolution code mesa, we investigate the long-term appearance and observational signatures of surviving MS companions of SNe Iax by tracing their post-impact evolution. Depending on different MS companion models, it is found that the shocked surviving companion stars can significantly expand and evolve to be more luminous (5–$500\, L_{\odot }$) for a time-scale of 10–104 yr. Comparing with the late-time light curve of an observed SN Iax (SN 2005hk), it is suggested that surviving MS companions of SNe Iax would expect to be visible about 1000 d after the explosion when SN itself has been faded.

scholarly journals The Core-Collapse Supernova Explosion Mechanism

2016 ◽  
Vol 12 (S329) ◽  
pp. 17-24 ◽  
Author(s):  
Bernhard Müller
Keyword(s):  
Supernova Explosion ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
The Core ◽  
Supernova Explosions ◽  
Explosion Mechanism ◽  
Standing Problem

AbstractThe explosion mechanism of core-collapse supernovae is a long-standing problem in stellar astrophysics. We briefly outline the main contenders for a solution and review recent efforts to model core-collapse supernova explosions by means of multi-dimensional simulations. Focusing on the neutrino-driven mechanism, we summarize currents efforts to predict supernova explosion and remnant properties.

scholarly journals Magnetorotational Mechanism of Supernova Explosions - Results of 2D Simulations

1998 ◽  
Vol 11 (1) ◽  
pp. 376-376
Author(s):  
S.G. Moiseenko
Keyword(s):  
Magnetic Field ◽  
Equations Of State ◽  
Supernova Explosion ◽  
Neutrino Energy ◽  
Energy Losses ◽  
Rotational Momentum ◽  
Supernova Explosions ◽  
2D Numerical Simulation ◽  
Lagrangian Scheme ◽  
The Magnetic Field

Results of 2D numerical simulation of the magneto rotational mechanism of a supernova explosion are presented. Simulation has been done for the real equations of state and neutrino energy losses have been taken into account. Simulation has been done on the basis of an Implicit Lagrangian scheme on atriangular grid with grid reconstructuring. It is shown that, due to differential rotation of the star, a toroidal component of the magnetic field appears and grows with time. Rotational momentum transfers outwards as the toroidal component grows with time. With the evolution of the process, part of the envelope of the star is ejected. The amounts of the thrown-off mass and energy are estimated. The results of the simulation could be used as a possible explanation for the supernova explosion picture.

An Action-Based Approach to Improving Pain Management in Long-Term Care

2010 ◽  
Vol 29 (4) ◽  
pp. 503-517 ◽  
Author(s):  
Sharon Kaasalainen ◽  
Kevin Brazil ◽  
Esther Coker ◽  
Jenny Ploeg ◽  
Ruth Martin-Misener ◽  
...  
Keyword(s):  
Nous Avons ◽  
Term Care ◽  
Soins De Santé ◽  
Gestion De La Douleur ◽  
Longue Duree ◽  
Longue Durée ◽  
Cas A ◽  
Groupes De Discussion ◽  
Systèmes De Santé

RÉSUMÉObjectif : Les objectifs de cette étude étaient double : (1) d’explorer les obstacles à la gestion de la douleur et ceux associés à la mise en œuvre d’un programme de gestion de la douleur en soins de longue durée (SLD) et (2) de développer une approche interprofessionelle afin d’améliorer la gestion de la douleur en soins de longue durée.Méthodes : Une étude de cas a inclus tous les deux éléments, quantitatifs et qualitatifs. Nous avons recueilli des données sur deux sites LTC à l’aide de sept groupes de discussion pour les infirmières autorisées, fournisseurs de soins non réglementés, et médecins, et 10 entretiens avec des autres groupes de fournisseurs de soins de santé, l’administration et des résidents. Nous avons examiné les documents et administré un sondage à court aux participants à l’étude pour évaluer les perceptions des obstacles à la gestion de la douleur.Résultats : Les résultats ont révélé des obstacles à la gestion efficace de la douleur au niveau des soins de longue durée des résidents et des familles, des fournisseurs de soins de santé, et des systèmes de santé. Nous avons ensuite élaboré un modèle à six niveaux, avec les interventions proposées pour surmonter ces obstacles.Conclusions : Ce modèle peut guider le développement d’approches novatrices pour améliorer la gestion de la douleur dans les établissements de soins de longue durée.

scholarly journals Fingerprint of Galactic Loop I on polarized microwave foregrounds

2018 ◽  
Vol 617 ◽  
pp. A90 ◽  
Author(s):  
Hao Liu
Keyword(s):  
Supernova Explosion ◽  
Large Area ◽  
Microwave Background ◽  
Local Bubble ◽  
Galactic Emission ◽  
Primordial Gravitational Waves ◽  
Polarized Emission ◽  
Supernova Explosions ◽  
Foreground Analysis ◽  
The Magnetic Field

Context. Currently, detection of the primordial gravitational waves using the B-mode of cosmic microwave background (CMB) is primarily limited by our knowledge of the polarized microwave foreground emissions. Improvements of the foreground analysis are therefore necessary. As we revealed in an earlier paper, the E-mode and B-mode of the polarized foreground have noticeably different properties, both in morphology and frequency spectrum, suggesting that they arise from different physicalprocesses, and need to be studied separately. Aims. I study the polarized emission from Galactic loops, especially Loop I, and mainly focus on the following questions: Does the polarized loop emission contribute predominantly to the E-mode or B-mode? In which frequency bands and in which sky regions can the polarized loop emission be identified? Methods. Based on a well known result concerning the magnetic field alignment in supernova explosions, a theoretical expectation is established that the loop polarizations should be predominantly E-mode. In particular, the expected polarization angles of Loop I are compared with those from the real microwave band data of WMAP and Planck. Results and conclusions. The comparison between model and data shows remarkable consistency between the data and our expectations at all bands and for a large area of the sky. This result suggests that the polarized emission of Galactic Loop I is a major polarized component in all microwave bands from 23 to 353 GHz, and a considerable part of the polarized foreground likely originates from a local bubble associated with Loop I, instead of the far more distant Galactic emission. This result also provides a possible way to explain the E-to-B excess problem by contribution of the loops. Finally, this work may also provide the first geometrical evidence that the Earth was hit by a supernova explosion.

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