Hydrodynamic Studies of Accretion onto Massive White Dwarfs: ONeMg-enriched Nova Outbursts. I. Dependence on White Dwarf Mass

Politano, M.; Starrfield, S.; Truran, J. W.; Weiß, A.; Sparks, W. M.

doi:10.1086/176009

Cited by 137 publications

(155 citation statements)

References 0 publications

Supporting

Mentioning

143

Contrasting

Order By: Relevance

“…In massive WDs, about one-tenth of hydrogen is consumed by nuclear burning to produce thermal and gravitational energy during the early phase of the outburst (Politano et al 1995;Prialnik & Kovetz 1995). Supposing that ΔX = 0.1 of hydrogen is converted into helium, the hydrogen/ helium ratio becomes X/Y = (0.7 − 0.1)/(0.28 + 0.1) = 1.6.…”

Section: System Parameters Of Optically Thick Wind Modelmentioning

confidence: 99%

A Universal Decline Law of Classical Novae. Iv. V838 Her (1991): A Very Massive White Dwarf

Kato

Hachisu

Cassatella

2009

ApJ

View full text Add to dashboard Cite

We present a unified model of optical and ultraviolet (UV) light curves for one of the fastest classical novae, V838 Herculis (Nova Herculis 1991), and estimate its white dwarf (WD) mass. Based on an optically thick wind theory of nova outbursts, we model the optical light curves with free-free emission and the UV 1455 Å light curves with blackbody emission. Our models of 1.35 ± 0.02 M WD simultaneously reproduce the optical and UV 1455 Å observations. The mass lost by the wind is ΔM wind ∼ 2 × 10 −6 M . We provide new determinations of the reddening, E(B − V ) = 0.53 ± 0.05, and of the distance, 2.7 ± 0.5 kpc.

show abstract

Section: System Parameters Of Optically Thick Wind Modelmentioning

confidence: 99%

A Universal Decline Law of Classical Novae. Iv. V838 Her (1991): A Very Massive White Dwarf

Kato

Hachisu

Cassatella

2009

ApJ

View full text Add to dashboard Cite

show abstract

“…These conditions might be encountered at the peak of a nova outburst on an O-Ne white dwarf. Initial abundances were taken from Politano et al (1995). Abundances were tracked until just after hydrogen exhaustion, which occurred after about 200 s. Note that the time scale is set by the rate of hydrogen consumption in the CNO region rather than in the Ne-Si region.…”

Section: Network Calculationsmentioning

confidence: 99%

Synthesis of the elements in stars: forty years of progress

et al. 1997

View full text Add to dashboard Cite

Forty years ago Burbidge, Burbidge, Fowler, and Hoyle combined what we would now call fragmentary evidence from nuclear physics, stellar evolution and the abundances of elements and isotopes in the solar system as well as a few stars into a synthesis of remarkable ingenuity. Their review provided a foundation for forty years of research in all of the aspects of low energy nuclear experiments and theory, stellar modeling over a wide range of mass and composition, and abundance studies of many hundreds of stars, many of which have shown distinct evidence of the processes suggested by B 2 FH. In this review we summarize progress in each of these fields with emphasis on the most recent developments. [S0034-6861(97)

show abstract

“…The level of sophistication of such studies has significantly increased in the last decade. Some examples: X-ray burst simulations (with coupled hydrodynamics and nuclear networks) with different 15 O(α,γ) 19 Ne reaction rates [12] and examining overall reaction flows [13]; core collapse supernova simulations with different 132 Sn(n,γ) 133 Sn rates [14]; Type II supernova simulations with different weak reaction rates [15]; and multi-zone post-processing nova simulations with different 17 F(p,γ) 18 Ne [16] and 18 F(p,α) 15 O [17] reaction rates. For the future, it is imperative to vigorously pursue sensitivity studies with even mo re sophisticated models and, especially, more complete nuclear data sets.…”

Section: Prioritizationmentioning

confidence: 99%

“…and other theoretical calculations, it is imperative to design software systems that enable anyone to run and visualize these calculations. The Computational Infrastructure for Nuclear Astrophysics features explosive element burning ("reaction network" [18]) calculations using a post-processing approach [16] wherein the temperature and density evolution in time are pre-determined from separate, lengthy simulations where hydrodynamics and nuclear effects are fully coupled [19]. The suite facilitates sensitivity studies by enabling quick comparisons of the results of explosive nucleosynthesis simulations that utilize different, custom input nuclear data sets created by the User (fig.…”

Section: Prioritizationmentioning

confidence: 99%

“…Other important 19 Ne reaction rate using a Monte Carlo nucleosynthesis approach [3]. criteria include the activity of experimentalists, the quality of the existing datasets, the number of astrophysical modelers who require the information, the manpower required for an evaluation project, and the availability of scientists interested in performing the evaluations.…”

Section: Prioritizationmentioning

confidence: 99%

See 1 more Smart Citation

Nuclear data for astrophysics: resources, challenges, strategies, and software solutions

Smith

Lingerfelt

Nesaraja

et al. 2007

Nd2007

View full text Add to dashboard Cite

Abstract. One of the most exciting utilizations of nuclear data is to help unlock the mysteries of the Cosmos -the creation of the chemical elements, the evolution and explosion of stars, and the origin and fate of the Universe. There are now many nuclear data sets, tools, and other resources online to help address these important questions. However, numerous serious challenges make it important to develop strategies now to ensure a sustainable future for this work. A number of strategies are advocated, including: enlisting additional manpower to evaluate the newest data; devising ways to streamline evaluation activities; and improving communication and coordination between existing efforts. Software projects are central to some of these strategies. Examples include: creating a virtual "pipeline" leading from the nuclear laboratory to astrophysics simulations; improving data visualization and management to get the most science out of the existing datasets; and creating a nuclear astrophysics data virtual (online) community. Recent examples will be detailed, including the development of two first-generation software pipelines, the Computational Infrastructure for Nuclear Astrophysics for stellar astrophysics and the bigbangonline suite of codes for cosmology, and the coupling of nuclear data to sensitivity studies with astrophysical simulation codes to guide future research. Background and motivationThe interdisciplinary field of nuclear astrophysics was established because fundamental knowledge of science at length scales of 10 −13 cm is required to address fascinating astrophysical questions such as the origins of the elements that make life possible, the evolution and explosions of stars, and the origin, composition, age, and ultimate fate of the Universe. Indeed, nuclear reaction information (e.g., cross sections, s-factors, reaction rates), nuclear structure information (e.g., masses, decays, resonance properties), and other specialized data sets (e.g., the nuclear equation of state) serve as the empirical foundation of our knowledge of many astrophysical sites and events. The availability of incredible images and data from powerful space-and ground-based observatories (e.g., Hubble, Chandra, Wilkinson, Keck, Subaru, and others), as well as the sophisticated astrophysical simulation codes that run on the fastest supercomputers, have led to a tremendous growth in this field. With new nuclear accelerator laboratories on the horizon (e.g., RIKEN RI Beam Factory, GSI/FAIR, RIA) that promise tremendous amounts of new data, this growth will definitely continue in the future.This growth is strong motivation to expand efforts to bolster the nuclear foundation of astrophysical studies. Improved nuclear science is needed, for example, to decipher the latest measurements using satellite observatories of longlived radionuclides [e.g., 26 Al, 44 Ti, 18 F] that are synthesized in and dispersed by supernova [1] and/or nova [2] explosions. Improved nuclear data -especially uncertainty and covariance information -is also ne...

show abstract

Hydrodynamic Studies of Accretion onto Massive White Dwarfs: ONeMg-enriched Nova Outbursts. I. Dependence on White Dwarf Mass

Cited by 137 publications

References 0 publications

A Universal Decline Law of Classical Novae. Iv. V838 Her (1991): A Very Massive White Dwarf

A Universal Decline Law of Classical Novae. Iv. V838 Her (1991): A Very Massive White Dwarf

Synthesis of the elements in stars: forty years of progress

Nuclear data for astrophysics: resources, challenges, strategies, and software solutions

Contact Info

Product

Resources

About