scholarly journals Excluding supersoft X-ray sources as progenitors for four Type Ia supernovae in the Large Magellanic Cloud

2019 ◽  
Vol 484 (1) ◽  
pp. 1317-1324 ◽  
Author(s):  
J Kuuttila ◽  
M Gilfanov ◽  
I R Seitenzahl ◽  
T E Woods ◽  
F P A Vogt
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Type Ia Supernovae ◽  
X Ray ◽  
Type Ia ◽  
Ia Supernovae

scholarly journals Supersoft X-ray nebulae in the Large Magellanic Cloud

2020 ◽  
Vol 497 (3) ◽  
pp. 3234-3250 ◽  
Author(s):  
Diego A Farias ◽  
Alejandro Clocchiatti ◽  
Tyrone E Woods ◽  
Armin Rest
Keyword(s):  
Interstellar Medium ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
The Other ◽  
X Rays ◽  
X Ray ◽  
Upper Limits ◽  
Type Ia ◽  
Source Models ◽  
Flux Measurements

ABSTRACT Supersoft X-rays sources (SSSs) have been proposed as potential Type Ia supernova (SN Ia) progenitors. If such objects are indeed persistently X-ray luminous and embedded in sufficiently dense interstellar medium (ISM), they will be surrounded by extended nebular emission. These nebulae should persist even long after an SN Ia explosion, due to the long recombination and cooling times involved. With this in mind, we searched for nebular [O iii] emission around four SSSs and three SNRs in the Large Magellanic Cloud, using the 6.5-m Baade telescope at Las Campanas Observatory and the imacs camera. We confirm that, out of the four SSS candidates, only CAL 83 can be associated with an [O iii] nebula. The [O iii] luminosity for the other objects is constrained to ≲17 per cent of that of CAL 83 at 6.8 pc from the central source. Models computed with the photoionization code cloudy indicate that either the ISM densities in the environments of CAL 87, RX J0550.0-7151, and RX J0513.9-6951 must be significantly lower than surrounding CAL 83 or the average X-ray luminosities of these sources over the last ≲10  000 yr must be significantly lower than presently observed, in order to be consistent with the observed luminosity upper limits. For the three SNRs we consider (all with ages <1000 yr), our [O iii] flux measurements together with the known surrounding ISM densities strongly constrain the ionizing luminosity of their progenitors in the last several thousand years, independent of the progenitor channel.

scholarly journals On the Progenitors of Type Ia Supernovae

2002 ◽  
Vol 187 ◽  
pp. 103-108
Author(s):  
X.-D. Li ◽  
E. P. J. van den Heuvel
Keyword(s):  
Nuclear Fuel ◽  
White Dwarfs ◽  
Radiation Temperature ◽  
Type Ia Supernovae ◽  
Characteristic Radiation ◽  
X Ray ◽  
Bolometric Luminosity ◽  
Type Ia ◽  
Ia Supernovae ◽  
Eddington Limit

Supersoft X-ray sources (hereafter SSS) are a class of luminous (bolometric luminosity ~ 1037 − 1038 erg s−1) objects with a characteristic radiation temperature of 30 to 60 eV (Hasinger 1994; Kahabka & Trümper 1996). The most popular model for SSS is that they are massive white dwarfs steadily burning nuclear fuel accreted from a more massive binary companion at a rate near or above the Eddington limit (van den Heuvel et al. 1992).

scholarly journals CONSTRAINTS ON THE COSMOLOGICAL DENSITY PARAMETERS AND COSMIC TOPOLOGY

2007 ◽  
Vol 16 (02n03) ◽  
pp. 207-217 ◽  
Author(s):  
M. J. REBOUÇAS
Keyword(s):  
Mass Fraction ◽  
Type Ia Supernovae ◽  
Data Sets ◽  
X Ray ◽  
Set Constraints ◽  
Type Ia ◽  
Ia Supernovae ◽  
The Universe ◽  
Nontrivial Topology ◽  
Spatial Section

A nontrivial topology of the spatial section of the universe is an observable which can be probed for all homogeneous and isotropic universes, without any assumption on the cosmological density parameters. We discuss how one can use this observable to set constraints on the density parameters of the universe by using a specific spatial topology along with type Ia supernovae and X-ray gas mass fraction data sets.

scholarly journals Theory of Nova Outbursts and Type Ia Supernovae

2015 ◽  
Vol 2 (1) ◽  
pp. 205-211
Author(s):  
M. Kato ◽  
I. Hachisu
Keyword(s):  
Near Infrared ◽  
Light Curves ◽  
Infrared Light ◽  
Type Ia Supernovae ◽  
Theoretical Understanding ◽  
X Ray ◽  
Classical Novae ◽  
Type Ia ◽  
Ia Supernovae ◽  
Nova Outbursts

We briefly review the current theoretical understanding of the light curves of novae. These curves exhibit a homologous nature, dubbed the universal decline law, and when time-normalized, they almost follow a single curve independently of the white dwarf (WD) mass or chemical composition of the envelope. The optical and near-infrared light curves of novae are reproduced mainly by free-free emission from their optically thick winds. We can estimate the WD mass from multiwavelength observations because the optical, UV, and soft X-ray light curves evolve differently and we can easily resolve the degeneracy of the optical light curves. Recurrent novae and classical novae are a testbed of type Ia supernova scenarios. In the orbital period versus secondary mass diagram, recurrent novae are located in different regions from classical novae and the positions of recurrent novae are consistent with the single degenerate scenario.

scholarly journals Novae and Accreting White Dwarfs as Progenitors of Type Ia Supernovae

2011 ◽  
Vol 7 (S281) ◽  
pp. 172-180
Author(s):  
Mariko Kato
Keyword(s):  
White Dwarfs ◽  
Main Sequence ◽  
Accretion Rate ◽  
Type Ia Supernovae ◽  
Light Curve Analysis ◽  
X Ray ◽  
Type Ia ◽  
Recurrent Nova ◽  
Red Giant ◽  
Ia Supernovae

AbstractI review various phenomena associated with mass-accreting white dwarfs (WDs) in relation to progenitors of Type Ia supernovae (SNe Ia). The WD mass can be estimated from light curve analysis in multiwavelength bands based on the theory of optically thick winds. In the single degenerate scenario of SNe Ia, two main channels are known, i.e., WD + main sequence (MS) channel and WD + red giant (RG) channel. In each channel, a typical binary undergoes three evolutionary stages before explosion, i.e., the wind phase, supersoft X-ray source (SSS) phase, and recurrent nova phase, in this order because the accretion rate decreases with time as the companion mass decreases. For some accreting WDs we can identify the corresponding stage of evolution. Intermittent supersoft X-ray sources like RX J0513.9−6951 and V Sge correspond to wind phase objects. For the SSS phase, CAL 87-type objects correspond to the WD+MS channel. For the WD + RG channel, soft X-ray observations of early type galaxies give statistical evidence of SSS phase binaries. Recurrent novae of U Sco-type and RS Oph-type correspond to the WD + MS channel and WD + RG channel, respectively. The majority of recurrent novae host a very massive WD (≳ 1.35 M⊙) and often show a plateau phase in their optical light curves corresponding to the long-lasting supersoft X-ray phase. These properties are indications of increasing WD masses.

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