scholarly journals The Interaction of Type Ia Supernovae with Planetary Nebulae: The Case of Kepler’s Supernova Remnant

Galaxies ◽  
2020 ◽  
Vol 8 (2) ◽  
pp. 38
Author(s):  
A. Chiotellis ◽  
P. Boumis ◽  
Z. T. Spetsieri
Keyword(s):  
Supernova Remnants ◽  
Ambient Medium ◽  
Planetary Nebulae ◽  
Northern Region ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Partial Interaction ◽  
Ia Supernovae ◽  
Progenitor Stars ◽  
Good Agreement

One of the key methods for determining the unknown nature of Type Ia supernovae (SNe Ia) is the search for traces of interaction between the SN ejecta and the circumstellar structures at the resulting supernova remnants (SNRs Ia). So far, the observables that we receive from well-studied SNRs Ia cannot be explained self-consistently by any model presented in the literature. In this study, we suggest that the circumstellar medium (CSM) being observed to surround several SNRs Ia was mainly shaped by planetary nebulae (PNe) that originated from one or both progenitor stars. Performing two-dimensional hydrodynamic simulations, we show that the ambient medium shaped by PNe can account for several properties of the CSM that have been found to surround SNe Ia and their remnants. Finally, we model Kepler’s SNR considering that the SN explosion occurred inside a bipolar PN. Our simulations show good agreement with the observed morphological and kinematic properties of Kepler’s SNR. In particular, our model reproduces the current expansion parameter of Kepler’s SNR, the partial interaction of the remnant with a dense CSM at its northern region and finally the existence of two opposite protrusions (‘ears’) at the equatorial plane of the SNR.

scholarly journals Convection and spin-up during common envelope evolution: the formation of short-period double white dwarfs

2020 ◽  
Vol 497 (2) ◽  
pp. 1895-1903 ◽  
Author(s):  
E C Wilson ◽  
J Nordhaus
Keyword(s):  
Stellar Evolution ◽  
White Dwarfs ◽  
Orbital Parameter ◽  
Type Ia Supernovae ◽  
Core Mass ◽  
Common Envelope ◽  
Short Period ◽  
Type Ia ◽  
Ia Supernovae ◽  
Progenitor Stars

ABSTRACT The formation channels and predicted populations of double white dwarfs (DWDs) are important because a subset will evolve to be gravitational-wave sources and/or progenitors of Type Ia supernovae. Given the observed population of short-period DWDs, we calculate the outcomes of common envelope (CE) evolution when convective effects are included. For each observed white dwarf (WD) in a DWD system, we identify all progenitor stars with an equivalent proto-WD core mass from a comprehensive suite of stellar evolution models. With the second observed WD as the companion, we calculate the conditions under which convection can accommodate the energy released as the orbit decays, including (if necessary) how much the envelope must spin-up during the CE phase. The predicted post-CE final separations closely track the observed DWD orbital parameter space, further strengthening the view that convection is a key ingredient in CE evolution.

scholarly journals 16O(p,α)13N makes explosive oxygen burning sensitive to the metallicity of the progenitors of type Ia supernovae

2019 ◽  
Vol 627 ◽  
pp. A146
Author(s):  
E. Bravo
Keyword(s):  
Supernova Remnants ◽  
Fusion Reaction ◽  
Reaction Rates ◽  
Type Ia Supernovae ◽  
Fusion Reactions ◽  
Maximum Brightness ◽  
Theoretical Predictions ◽  
Type Ia ◽  
Standard Values ◽  
Ia Supernovae

Even though the main nucleosynthetic products of type Ia supernovae belong to the iron-group, intermediate-mass alpha-nuclei (silicon, sulfur, argon, and calcium) stand out in their spectra up to several weeks past maximum brightness. Recent measurements of the abundances of calcium, argon, and sulfur in type Ia supernova remnants have been interpreted in terms of metallicity-dependent oxygen burning, in accordance with previous theoretical predictions. It is known that α-rich oxygen burning results from 16O→12C followed by efficient 12C+12C fusion reaction, as compared to oxygen consumption by 16O fusion reactions, but the precise mechanism of dependence on the progenitor metallicity has remained unidentified so far. I show that the chain 16O(p,α)13N(γ,p)12C boosts α-rich oxygen burning when the proton abundance is large, increasing the synthesis of argon and calcium with respect to sulfur and silicon. For high-metallicity progenitors, the presence of free neutrons leads to a drop in the proton abundance and the above chain is not efficient. Although the rate of 16O(p,α)13N can be found in astrophysical reaction rate libraries, its uncertainty is unconstrained. Assuming that all reaction rates other than 16O(p,α)13N retain their standard values, an increase by a factor of approximately seven of the 16O(p,α)13N rate at temperatures in the order 3−5 × 109 K is enough to explain the whole range of calcium-to-sulfur mass ratios measured in Milky Way and LMC supernova remnants. These same measurements provide a lower limit to the 16O(p,α)13N rate in the mentioned temperature range, on the order of a factor of 0.5 with respect to the rate reported in widely used literature tabulations.

scholarly journals Modelling the early time behaviour of type Ia supernovae: effects of the 56Ni distribution

2018 ◽  
Vol 614 ◽  
pp. A115 ◽  
Author(s):  
M. R. Magee ◽  
S. A. Sim ◽  
R. Kotak ◽  
W. E. Kerzendorf
Keyword(s):  
Density Profile ◽  
Early Time ◽  
Initial Study ◽  
Light Curves ◽  
Parameter Study ◽  
Type Ia Supernovae ◽  
Monte Carlo Code ◽  
Type Ia ◽  
Ia Supernovae ◽  
Good Agreement

Recent studies have demonstrated the diversity in type Ia supernovae (SNe Ia) at early times and highlighted a need for a better understanding of the explosion physics as manifested by observations soon after explosion. To this end, we present a Monte Carlo code designed to model the light curves of radioactively driven, hydrogen-free transients from explosion to approximately maximum light. In this initial study, we have used a parametrised description of the ejecta in SNe Ia, and performed a parameter study of the effects of the 56Ni distribution on the observed colours and light curves for a fixed 56Ni mass of 0.6 M⊙. For a given density profile, we find that models with 56Ni extending throughout the entirety of the ejecta are typically brighter and bluer shortly after explosion. Additionally, the shape of the density profile itself also plays an important role in determining the shape, rise time, and colours of observed light curves. We find that the multi-band light curves of at least one SNe Ia (SN 2009ig) are inconsistent with less extended 56Ni distributions, but show good agreement with models that incorporate 56Ni throughout the entire ejecta. We further demonstrate that comparisons with full UV OIR colour light curves are powerful tools in discriminating various 56Ni distributions, and hence explosion models.

scholarly journals FITTING THE LUMINOSITY DATA FROM TYPE Ia SUPERNOVAE IN THE FRAME OF THE COSMIC DEFECT THEORY

2009 ◽  
Vol 18 (03) ◽  
pp. 501-512
Author(s):  
A. TARTAGLIA ◽  
M. CAPONE ◽  
V. CARDONE ◽  
N. RADICELLA
Keyword(s):  
Accelerated Expansion ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Expansion Of The Universe ◽  
The One ◽  
Ia Supernovae ◽  
The Universe ◽  
Good Agreement

The cosmic defect (CD) theory is reviewed and used to fit the data for the accelerated expansion of the universe, obtained from the apparent luminosity of 192 SnIa 's. The fit from the CD theory is compared with the one obtained by means of ΛCDM. The results from the two theories are in good agreement and the fits are satisfactory. The correspondence between the two approaches is discussed and interpreted.

scholarly journals O, S, Ar from Planetary Nebulae Data and the Chemical Evolution of the Galactic Disk

1993 ◽  
Vol 155 ◽  
pp. 576-576
Author(s):  
J.A. De Freitas Pacheco
Keyword(s):  
Chemical Evolution ◽  
Galactic Disk ◽  
Planetary Nebulae ◽  
Hii Regions ◽  
Type Ia Supernovae ◽  
Type I ◽  
Intermediate Mass ◽  
B Stars ◽  
Type Ia ◽  
Ia Supernovae

The O, S, Ar abundances for a sample of 122 planetary nebulae (merging LNA data and those by Köppen, Acker and Stenholm 1991) were analysed. Average abundances were calculated for progenitors having different metallicities (ages). Our study suggests that type I planetaries, whose progenitors are not older than 1–2 Gyr, have average oxygen abundances 0.2 dex lower than the solar value. This agrees with O-abundance determinations in HII regions, intermediate mass supergiants and B stars in young associations. S and Ar show a different behaviour. We suggest that such a paucity of O in the ISM is produced by recent infalling gas from the halo, having abundance ratios similar to those expected from type Ia supernovae.

scholarly journals The single degenerate channel for the progenitors of Type Ia supernovae

2008 ◽  
Vol 4 (S252) ◽  
pp. 379-382
Author(s):  
Xiangcun Meng ◽  
Xuefei Chen ◽  
Zhanwen Han
Keyword(s):  
Stellar Evolution ◽  
Supernova Remnants ◽  
Birth Rate ◽  
Binary Systems ◽  
Supernova Explosion ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Rich Material ◽  
The Moment ◽  
Ia Supernovae

AbstractWe have carried out a detailed study of the single-degenerate channel for the progenitors of type Ia supernovae (SNe Ia). In the model, a carbon-oxygen white dwarf (CO WD) accretes hydrogen-rich material from an unevolved or a slightly evolved non-degenerate companion to increase its mass to Chandrasekhar mass limit. Incorporating the prescription of Hachisuet al. (1999a) for the accretion efficiency into Eggleton's stellar evolution code and assuming that the prescription is valid for all metallicities, we performed binary stellar evolution calculations for more than 25,000 close WD binary systems with various metallicities. The initial parameter spaces for SNe Ia are presented in an orbital period-secondary mass (logPi,M2i) plane for eachZ.Adopting the results above, we studied the birth rate of SNe Ia for variousZvia binary population synthesis. From the study, we see that for a highZ, SNe Ia occur systemically earlier and the peak value of the birth rate is larger if a single starburst is assumed. The Galactic birth rate from the channel is lower than (but comparable to) that inferred from observations.We also showed the distributions of the parameters of the binary systems at the moment of supernova explosion and the distributions of the properties of companions after supernova explosion. The former provides physics input to simulate the interaction between supernova ejecta and its companion, and the latter is helpful for searching the companions in supernova remnants.

scholarly journals Progenitor's Signatures in Type Ia Supernova Remnants

2011 ◽  
Vol 7 (S281) ◽  
pp. 331-334 ◽  
Author(s):  
A. Chiotellis ◽  
D. Kosenko ◽  
K. M. Schure ◽  
J. Vink
Keyword(s):  
White Dwarf ◽  
Supernova Remnants ◽  
Morphological Properties ◽  
Type Ia Supernovae ◽  
X Ray ◽  
Type Ia Supernova ◽  
Circumstellar Gas ◽  
Type Ia ◽  
Ia Supernovae ◽  
Shed Light

AbstractThe remnants of Type Ia supernovae (SNe Ia) can provide important clues about their progenitor histories. We discuss two well-observed supernova remnants (SNRs) that are believed to have resulted from SNe Ia, and use various tools to shed light on the possible progenitor histories. We find that Kepler's SNR is consistent with a symbiotic binary progenitor consisting of a white dwarf and an AGB star. Our hydrosimulations can reproduce the observed kinematic and morphological properties. For Tycho's remnant we use the characteristics of the X-ray spectrum and kinematics to show that the ejecta has likely interacted with dense circumstellar gas.

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