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Title: Hydrodynamic Simulations of Classical Novae: Accretion onto CO White Dwarfs as SN Ia Progenitors

We report on our continuing studies of Classical Nova explosions by following the evolution of thermonuclear runaways (TNRs) on carbon-oxygen (CO) white dwarfs (WDs). We have varied both the mass of the WD and the composition of the accreted material. Rather than assuming that the material has mixed from the beginning, we now rely on the results of the multidimensional (multi-D) studies of mixing as a consequence of the TNRs in WDs that accreted only Solar matter. The multi-D studies find that mixing with the core occurs after the TNR is well underway and reach enrichment levels in agreement with observations of the ejecta abundances. We report on 3 studies in this paper. First, simulations in which we accrete only Solar matter with NOVA (our 1-D, fully implicit, hydro code). Second, we use MESA for similar studies in which we accrete only Solar material and compare the results. Third, we accrete Solar matter until the TNR is initiated and then switch the composition in the accreted layers to a mixed composition: either 25% core and 75% Solar or 50% core and 50% Solar. The amount of accreted material is inversely proportional to the initial 12C abundance. Thus, accreting Solar materialmore » results in more material to fuel the outburst - much larger than in the earlier studies where mixed materials were used from the beginning. We tabulate the amount of ejected gases, their velocities, and abundances. We predict the amount of 7Li and 7Be produced and ejected by the explosion and compare our predictions to our Large Binocular Telescope (LBT) high dispersion spectra which determined the abundance of 7Li in nova V5668 Sgr. Finally, many of these simulations eject significantly less mass than accreted and, therefore, the WD is growing in mass toward the Chandrasekhar Limit.« less
Authors:
 [1] ;  [1] ;  [2] ; ORCiD logo [3] ;  [4] ;  [5] ;  [6] ;  [7]
  1. Arizona State Univ., Tempe, AZ (United States). Earth and Space Exploration
  2. Univ. of North Carolina, Chapel Hill, NC (United States). Dept. of Physics and Astronomy
  3. Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States); Univ. of Tennessee, Knoxville, TN (United States)
  4. Large Binocular Telescope Observatory, Tucson, AZ (United States); The Ohio State Univ., Columbus, OH (United States). Dept. of Astronomy
  5. Univ. of Minnesota, Minneapolis, MN (United States)
  6. Univ. Polytechnic of Catalunya, Barcelona, Catalunya (Spain)
  7. Inst. of Space Sciences, Barcelona, Catalunya (Spain)
Publication Date:
Grant/Contract Number:
AC05-00OR22725; 14-ATP14-0007; FG02-97ER41041
Type:
Accepted Manuscript
Journal Name:
PoS Proceedings of Science
Additional Journal Information:
Journal Volume: 315; Journal Issue: 066; Journal ID: ISSN 1824-8039
Publisher:
SISSA
Research Org:
Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
Sponsoring Org:
USDOE Office of Science (SC), Nuclear Physics (NP) (SC-26); National Aeronautics and Space Administration (NASA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS
OSTI Identifier:
1495963

Starrfield, Sumner, Bose, Maitrayee, Iliadis, Christian, Hix, William Raphael, Wagner, R. Mark, Woodward, Charles E., Jose, Jordi, and Hernanz, Margarita. Hydrodynamic Simulations of Classical Novae: Accretion onto CO White Dwarfs as SN Ia Progenitors. United States: N. p., Web. doi:10.22323/1.315.0066.
Starrfield, Sumner, Bose, Maitrayee, Iliadis, Christian, Hix, William Raphael, Wagner, R. Mark, Woodward, Charles E., Jose, Jordi, & Hernanz, Margarita. Hydrodynamic Simulations of Classical Novae: Accretion onto CO White Dwarfs as SN Ia Progenitors. United States. doi:10.22323/1.315.0066.
Starrfield, Sumner, Bose, Maitrayee, Iliadis, Christian, Hix, William Raphael, Wagner, R. Mark, Woodward, Charles E., Jose, Jordi, and Hernanz, Margarita. 2018. "Hydrodynamic Simulations of Classical Novae: Accretion onto CO White Dwarfs as SN Ia Progenitors". United States. doi:10.22323/1.315.0066. https://www.osti.gov/servlets/purl/1495963.
@article{osti_1495963,
title = {Hydrodynamic Simulations of Classical Novae: Accretion onto CO White Dwarfs as SN Ia Progenitors},
author = {Starrfield, Sumner and Bose, Maitrayee and Iliadis, Christian and Hix, William Raphael and Wagner, R. Mark and Woodward, Charles E. and Jose, Jordi and Hernanz, Margarita},
abstractNote = {We report on our continuing studies of Classical Nova explosions by following the evolution of thermonuclear runaways (TNRs) on carbon-oxygen (CO) white dwarfs (WDs). We have varied both the mass of the WD and the composition of the accreted material. Rather than assuming that the material has mixed from the beginning, we now rely on the results of the multidimensional (multi-D) studies of mixing as a consequence of the TNRs in WDs that accreted only Solar matter. The multi-D studies find that mixing with the core occurs after the TNR is well underway and reach enrichment levels in agreement with observations of the ejecta abundances. We report on 3 studies in this paper. First, simulations in which we accrete only Solar matter with NOVA (our 1-D, fully implicit, hydro code). Second, we use MESA for similar studies in which we accrete only Solar material and compare the results. Third, we accrete Solar matter until the TNR is initiated and then switch the composition in the accreted layers to a mixed composition: either 25% core and 75% Solar or 50% core and 50% Solar. The amount of accreted material is inversely proportional to the initial 12C abundance. Thus, accreting Solar material results in more material to fuel the outburst - much larger than in the earlier studies where mixed materials were used from the beginning. We tabulate the amount of ejected gases, their velocities, and abundances. We predict the amount of 7Li and 7Be produced and ejected by the explosion and compare our predictions to our Large Binocular Telescope (LBT) high dispersion spectra which determined the abundance of 7Li in nova V5668 Sgr. Finally, many of these simulations eject significantly less mass than accreted and, therefore, the WD is growing in mass toward the Chandrasekhar Limit.},
doi = {10.22323/1.315.0066},
journal = {PoS Proceedings of Science},
number = 066,
volume = 315,
place = {United States},
year = {2018},
month = {4}
}