An Extended Grid of Nova Models. II. The Parameter Space of Nova Outbursts

By O. Yaron, D. Prialnik, M. Shara, A. Geophysics, Planetary Sciences, Sackler Faculty of Exact Sciences, Tel Aviv University Department of Astrophysics, A. W. .. S. O. Physics, Astronomy, T. O. S. University. 2005

427 citations recorded by the source corpus.

This paper is a sequel to an earlier paper devoted to multiple, multicycle nova evolution models (Prialnik & Kovetz, Paper I), which showed that the different characteristics of nova outbursts can be reproduced by varying the values of three basic and independent parameters: the white dwarf mass, MWD, the temperature of its isothermal core, TWD, and the mass transfer rate, . Here we show that the parameter space is constrained by several analytical considerations and find its limiting surfaces. Consequently, we extend the grid of multicycle nova evolution models presented in Paper I to its limits, adding multicycle nova outburst calculations for a considerable number of new parameter combinations. In particular, the extended parameter space that produces nova eruptions includes low mass transfer rates down to 5 × 10-13 M☉ yr-1 and more models for low TWD. Resulting characteristics of these runs are added to the former parameter combination results to provide a full grid spanning the entire parameter space for carbon-oxygen white dwarfs. The full grid covers the entire range of observed nova characteristics, even those of peculiar objects, which have not been numerically reproduced until now. Most remarkably, runs for very low lead to very high values for some characteristics, such as outburst amplitude A ≳ 20, high super-Eddington luminosities at maximum, heavy element abundance of the ejecta Zej ≈ 0.63, and high ejected masses mej ≈ 7 × 10-4 M☉.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/383de541d1ddd5baa63daa12497df8754040d2c0

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. D. Maoz
2. F. Mannucci
3. G. Nelemans
4. B. Paxton
5. E. Berger
6. M. Zorotovic
7. L. Bildsten
8. N. Langer

In Instrumentation

1. D. Maoz
2. F. Mannucci
3. G. Nelemans
4. M. Zorotovic
5. B. Gänsicke
6. B. Paxton
7. B. Schaefer
8. M. Schreiber

Citations in the corpus

• HYDROGEN BURNING ON ACCRETING WHITE DWARFS: STABILITY, RECURRENT NOVAE, AND THE POST-NOVA SUPERSOFT PHASE (2013, methodology): “We compare recurrence times to the previous results from Iben (1982), Livio et al. (1989), Cassisi et al. (1998), and Yaron et al. (2005).”
• On the Progenitors of Type Ia Supernovae (2018, neutral): “10−8 M yr−1), the WD appears to be losing more mass during nova outbursts than the mass it accretes between outbursts (e.g., Livio & Truran 1992; Yaron et al. 2005).”
• Post common envelope binaries from SDSS - XI. The white dwarf mass distributions of CVs and pre-CVs (2011, background): “Simulations of nova outbursts predict that the amount of ejected mass is larger than the amount of accreted matter (see e.g. Prialnik & Kovetz 1995; Yaron et al. 2005), except in the case of very high mass-transfer rates (>∼ 10 −8M⊙ yr −1), which implies that in most of the cases the mass of the WD…”
• COMPREHENSIVE PHOTOMETRIC HISTORIES OF ALL KNOWN GALACTIC RECURRENT NOVAE (2009, background): “Changes in the mass of the white dwarf are dominated by the regular nova eruptions (like the ‘1866’ event) for which more mass is ejected than accreted (Yaron et al. 2005), with the RN episodes too short to make any difference.”
• Observational Clues to the Progenitors of Type Ia Supernovae (2013, background): “As a result, during the burning, some of the original WD material is blown away, along with the ashes of the accreted material (e.g. Yaron et al. 2005).”
• Thermal Stability of White Dwarfs Accreting Hydrogen-rich Matter and Progenitors of Type Ia Supernovae (2006, positive): “This boundary, which is Ṁstable ’ 10 7 M yr 1 at M = 0.8 M and higher for more massive white dwarfs, is consistent with fully time-dependent calculations (e.g., Paczyński & Żytkow 1978; Sion et al. 1979; Iben 1982; Prialnik & Kovetz 1995; Yaron et al. 2005).”
• Gamma-ray binaries and related systems (2013, methodology): “This value also agrees well with the accretion rates required by multicycle nova evolution models (Yaron et al. 2005) for RS Oph like binary systems, with MWD = 1.4 M% and a recurrence period of 22 years.”
• Are the Models for Type Ia Supernova Progenitors Consistent with the Properties of Supernova Remnants? (2007, background): “For even lower values of Ṁ , however, the flashes become stronger, effectively turning into nova explosions that erode theWD (Yaron et al. 2005).”
• EVLA OBSERVATIONS CONSTRAIN THE ENVIRONMENT AND PROGENITOR SYSTEM OF Type Ia SUPERNOVA 2011fe (2012, background): “Models of such a system show that 2 × 10−7 M⊙ yr −1 is incident upon the WD (Yaron et al. 2005; Shen & Bildsten 2009); we assume that 1% of this transferred material is lost to the binary to form the CSM at small radii.”