Recurrent novae as a progenitor system of type ia supernovae. I. rs ophiuchi subclass -- systems with a red giant companion

@article{Hachisu2001RecurrentNA,
  title={Recurrent novae as a progenitor system of type ia supernovae. I. rs ophiuchi subclass -- systems with a red giant companion},
  author={Izumi Hachisu and Mariko Kato},
  journal={The Astrophysical Journal},
  year={2001},
  volume={558},
  pages={323-350}
}
Theoretical light curves of four recurrent novae in outburst are modeled to obtain various physical parameters. The four objects studied here are those with a red giant companion, i.e., T Coronae Borealis, RS Ophiuchi, V745 Scorpii, and V3890 Sagittarii. Our model consists of a very massive white dwarf (WD) with an accretion disk and a red giant companion. Light-curve calculation includes reflection effects of the companion star and the accretion disk together with a shadowing effect on the… Expand
THE PROGENITOR OF THE TYPE Ia SUPERNOVA THAT CREATED SNR 0519-69.0 IN THE LARGE MAGELLANIC CLOUD
Models for the progenitor systems of Type Ia supernovae can be divided into double-degenerate systems, which contain two white dwarfs, and single-degenerate systems, which contain one white dwarfExpand
Exclusion of a luminous red giant as a companion star to the progenitor of supernova SN 2011fe
TLDR
The luminosity of the progenitor system (especially the companion star) is 10–100 times fainter than previous limits on other type Ia supernova progenitors systems, allowing us to rule out luminous red giants and almost all helium stars as the mass-donating companion to the exploding white dwarf. Expand
WD MS Systems as Progenitors of Type Ia Supernovae with Different Metallicities
The single-degenerate model for the progenitors of type Ia supernovae (SNe Ia) is one of the two most popular models, in which a carbon–oxygen white dwarf accretes hydrogen-rich material from itsExpand
3D simulations of RS Ophiuchi : from accretion to nova blast
Context. The binary star system RS Ophiuchi is a recurrent nova, with outbursts occurring about every 22 years. It consists of a red giant star (RG) and a wind accreting white dwarf close to theExpand
The Mass of the White Dwarf in the Recurrent Nova CI Aquilae
Abstract If recurrent novae (RNe) are progenitors of Type Ia Supernovae (SNe Ia), their white dwarfs (WD) must have masses close to the Chandrasekhar limit. The most reliable means of determining WDExpand
Early X-ray emission from Type Ia supernovae originating from symbiotic progenitors or recurrent novae
One of the key observables for determining the progenitor nature of Type Ia supernovae is provided by their immediate circumstellar medium, which according to several models should be shaped by theExpand
Simulations of the symbiotic recurrent nova V407 Cyg. I. Accretion and shock evolutions
The shock interaction and evolution of nova ejecta with a wind from a red giant star in a symbiotic binary system are investigated via three-dimensional hydrodynamics simulations. We specificallyExpand
Constraints on the progenitor system of the type Ia supernova 2014J from pre-explosion Hubble Space Telescope imaging
We constrain the properties of the progenitor system of the highly reddened Type Ia supernova (SN Ia) 2014J in Messier 82 (M82; d 3.5 Mpc). We determine the supernova (SN) location using Keck-IIExpand
ASASSN-16oh: A Nova Outburst with No Mass Ejection—A New Type of Supersoft X-Ray Source in Old Populations
ASASSN-16oh is a peculiar transient supersoft X-ray source without a mass-ejection signature in the field of the Small Magellanic Cloud. Maccarone et al. (2019) concluded that ASASSN-16oh is theExpand
Numerical Simulations of Supernovae Type Ia: The Early X-ray Emission
An insight of the origin of Type Ia supernovae (SN Ia) could be provided by the study of the interaction of the SN blast wave with the circumstellar medium, shaped by mass outflows from theExpand
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 100 REFERENCES
Recurrent Novae as a progenitor system of Type Ia Supernovae
Theoretical light curves of 8 recurrent novae in outburst are modeled to obtain various physical parameters. Light curve calculation includes reflection effects of the companion star and theExpand
A Theoretical Light-Curve Model for the 1999 Outburst of U Scorpii.
TLDR
A theoretical light curve for the 1999 outburst of U Scorpii is presented in order to obtain various physical parameters of the recurrent nova, which are exactly the same as those predicted in a new progenitor model of Type Ia supernovae. Expand
A New Interpretation for the Second Peak of T Coronae Borealis Outbursts: A Tilting Disk around a Very Massive White Dwarf
A new interpretation for the second peak of T Coronae Borealis outbursts is proposed based on a thermonuclear runaway (TNR) model. The system consists of a very massive white dwarf (WD) with aExpand
A Theoretical Light-Curve Model for the 1985 Outburst of RS Ophiuchi.
  • Hachisu, Kato
  • Physics, Medicine
  • The Astrophysical journal
  • 2000
TLDR
A theoretical light-curve model of the 1985 outburst of RS Ophiuchi based on a thermonuclear runaway model is presented and RS Oph is certainly a strong candidate for a Type Ia supernova progenitor. Expand
A New Evolutionary Path to Type Ia Supernovae: A Helium-rich Supersoft X-Ray Source Channel
We have found a new evolutionary path to Type Ia supernovae (SNe Ia) that has been overlooked in previous work. In this scenario, a carbon-oxygen white dwarf (C+O WD) is originated not from anExpand
A theoretical light-curve model for the recurrent nova V394 Coronae Australis
A theoretical light curve for the 1987 outburst of V394 Coronae Australis (V394 CrA) is modeled to obtain various physical parameters of this recurrent nova. We then apply the same set of parametersExpand
A New Model for Progenitor Systems of Type IA Supernovae
We propose a new model for progenitor systems of Type Ia supernovae. The model consists of an accreting white dwarf and a lobe-filling, low-mass red giant. When the mass accretion rate exceeds aExpand
A Model for the Quiescent Phase of the Recurrent Nova U Scorpii.
TLDR
A theoretical light curve is constructed for the quiescent phase of the recurrent nova U Scorpii in order to resolve the existing distance discrepancy between the outbursts and the quyingcences, indicating a mass outflow of approximately 3x10-7 M middle dot in circle yr-1 through the outer Lagrangian points in quiescence. Expand
The nature of the recurrent novae
The basic properties of individual recurrent nova systems are reviewed, and the mechanisms of their outbursts are studied. Some general properties associated with accretion events and thermonuclearExpand
Accreting white dwarf models for type I supernovae. I. Presupernova evolution and triggering mechanisms
As a plausible explosion model for a Type I supernova, the evolution of carbon-oxygen white dwarfs accreting helium in binary systems was investigated from the onset of accretion up to the point atExpand
...
1
2
3
4
5
...