*
Cococubed.com


Novae

Home

Astronomy research
  Software Infrastructure:
     MESA
     FLASH
     STARLIB
     My codes
  White dwarf supernova:
     Colliding white dwarfs
     Merging white dwarfs
     Ignition conditions
     Metallicity effects
     Central density effects
     Detonation density effects
     Tracer particle burning
     Subsonic burning fronts
     Supersonic burning fronts
     W7 profiles
  Massive star supernova:
     Rotating progenitors
     3D evolution
     26Al & 60Fe
     44Ti, 60Co & 56Ni
     Yields of radionuclides
     Effects of 12C +12C
     SN 1987A light curve
     Constraints on Ni/Fe ratios
     An r-process
     Compact object IMF
  Stars:
     Pre-SN variations
     MC white dwarfs
     SAGB
     Classical novae
     He shell convection
     Presolar grains
     He burn on neutron stars
     BBFH at 40 years
  Chemical Evolution:
     Hypatia catalog
     Zone models H to Zn
     Mixing ejecta
     γ-rays within 100 Mpc
  Thermodynamics & Networks
     Stellar EOS
     Reaction networks
     Proton-rich NSE
     MC reaction rates
  Verification Problems:
     Validating an astro code
     Su-Olson
     Cog8
     Mader
     RMTV
     Sedov
     Noh
Software instruments
Presentations
Illustrations
Videos
Bicycle adventures

AAS Journals
2017 MESA Marketplace
2017 MESA Summer School
2017 ASU+EdX AST111x
Teaching materials
Education and Public Outreach


Contact: F.X.Timmes
my one page vitae,
full vitae,
research statement, and
teaching statement.
The Effects of the pep Nuclear Reaction and Other Improvements on Simulations of the Classical Nova (2009) Outburst

Nova explosions occur on the white dwarf (WD) component of a cataclysmic variable binary stellar system which is accreting matter lost by its companion. When sufficient material has been accreted by the WD, a thermonuclear runaway (TNR) occurs and ejects material in what is observed as a classical nova (CN) explosion. In this paper by Starrfield et al, we continue our studies of TNRs on 1.25 M and 1.35 M WDs (ONeMg composition) under conditions which produce mass ejection and a rapid increase in the emitted light, by examining the effects of changes in the nuclear reaction rates on both the observable features and the nucleosynthesis during the outburst. We have incorporated a modern nuclear reaction network into our 1D, fully implicit, hydrodynamic computer tool. We find that the updates in the nuclear reaction rate libraries change the amount of ejected mass, peak luminosity, and the resulting nucleosynthesis. Because the evolutionary sequences on the 1.35 M WD reach higher temperatures, the effects of library changes are more important for this mass. We discovered that the pep reaction (p + e,- + p → d + ν) was not included in our previous studies, or to the best of our knowledge those of other investigators. Although the energy production from this reaction is not important in the Sun, the densities in WD envelopes can exceed 104 g cm-3 and the presence of this reaction increases the energy generation during the time that the pp chain is operating. Since it is only the pp chain that is operating during most of the accretion phase prior to the final rise to the TNR, the effect of the increased energy generation is to reduce the evolution time to the peak of the TNR and, thereby, the accreted mass as compared to the evolutionary sequences done without this reaction included.

image
Temperature profiles 1.25 M
image
Temperature profiles 1.35 M
image
Nuclear Luminosity 1.25 M
image
Nuclear Luminosity 1.35 M
image
Luminosity 1.25 M
image
Luminosity 1.35 M
image
Abundance pattern 1.25 M
image
Abundance pattern 1.35 M


Surface Hydrogen Burning Modeling of Super Soft Xray Binaries: Are They Supernova Ia Progenitors? (2004)

Nova explosions occur on the white dwarf (WD) component of a Cataclysmic Variable stellar system which is accreting matter lost by a companion. A Type Ia supernova explosion is thought to result when a WD, in a similar binary configuration, grows in mass to the Chandrasekhar Limit. In this paper by Starrfield we present calculations of accretion of Solar matter, at a variety of mass accretion rates, onto hot (2.3×105K), luminous (30 L), massive (1.25 M, 1.35 M) Carbon-Oxygen WDs. In contrast to our nova simulations where the WD has a low initial luminosity and a thermonuclear runaway (TNR) occurs and ejects material, these simulations do not eject material (or only a small fraction of the accreted material) and the WD grows in mass. A hydrogen TNR does not occur because hydrogen fuses to helium in the surface layers, and we call this process Surface Hydrogen Burning (SHB). As the helium layer grows in mass, it gradually fuses either to carbon and oxygen or to more massive nuclei depending on the WD mass and mass accretion rate. If such a WD were to explode in a SN Ia event, therefore, it would show neither hydrogen nor helium in its spectrum as is observed. Moreover, the luminosities and effective temperatures of our simulations agree with the observations of some of the Super Soft X-ray Binary Sources and, therefore, our results strengthen previous speculation that some of them (CAL 83 and CAL 87 for example) are probably progenitors of SN Ia explosions. Finally, we have achieved SHB for values of the mass accretion rate that almost span the observed values of the Cataclysmic Variables.

image
HR of accreting WDs and SSS


On Heavy Element Enrichment in Classical Novae (2004)

Many classical nova ejecta are enriched in CNO and Ne. Rosner et al. recently suggested that the enrichment might originate in the resonant interaction between large-scale shear flows in the accreted H/He envelope and gravity waves at the interface between the envelope and the underlying C/O white dwarf. The shear flow amplifies the waves, which eventually form cusps and break. This wave breaking injects a spray of C/O into the superincumbent H/He. Using two-dimensional simulations, in this paper by Alexakis et al we formulate a quantitative expression for the amount of C/O per unit area that can be entrained, at saturation, into the H/He. The fraction of the envelope that is enriched depends on the horizontal distribution of shear velocity and the density contrast between the C/O white dwarf and the H/He layer but is roughly independent of the vertical shape of the shear profile. Using this parameterization for the mixed mass, we then perform several one-dimensional Lagrangian calculations of an accreting white dwarf envelope and consider two scenarios: that the wave breaking and mixing is driven by the convective flows; and that the mixing occurs prior to the onset of convection. In the absence of enrichment prior to ignition, the base of the convective zone, as calculated from mixing-length theory with the Ledoux instability criterion, does not reach the C/O interface. As a result, there is no additional mixing, and the runaway is slow. In contrast, the formation of a mixed layer during the accretion of H/He, prior to ignition, causes a more violent runaway. The envelope can be enriched by ≤25% of C/O by mass (consistent with that observed in some ejecta) for shear velocities, over the surface, with Mach numbers ≤ 0.4.

image
Breaking C/O waves
image
12C mass fraction


7Be and 22Na (1998)

image
7Be decay
image
22Na upper limits