Numerical Study of White Dwarf Thermonuclear...
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Numerical Study of White Dwarf Thermonuclear Explosions induced
by Tidal Disruption EventsAtaru Tanikawa (The University of Tokyo)
The 8th East Asian Numerical Astrophysics Meeting National Cheng-Kung University Tainan, Taiwan, Oct. 22nd, 2018
Tanikawa et al. (2017, ApJ, 839, 81) Tanikawa (2018, ApJ, 858, 26)
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Tidal Disruption Event
• Tidal disruption of a star (e.g. main sequence stars) by a BH
• Bright flare powered by accretion of the stellar debris
• Several ten candidates (Kommosa 2015)
• TDEs of main sequence stars
• No conformed WD TDEs
ASASSN-15lh
Leloudas+16
Komossa 15
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Tidal detonation• Supersonic combustion induced by a tidal field of a BH
• The WD is compressed in z-direction.
• The compression induces a shock wave.
• The shock wave triggers a detonation wave.
• The detonation wave synthesizes large amounts of 56Ni.
• The WD TDE can be powered by radioactive decay 56Ni, similarly to SNe Ia.
x
yz
BH
WDBH gravity
Orbital motion
z
xy-plane
WD surface Shock wave
Nuclear burning
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Probe to search for Intermediate mass black hole • Tidal detonation requires a WD TDE.
• A WD can be tidally disrupted only by an IMBH.
• swallowing a stellar-mass BH.
• swallowed by a massive BH.
• WD TDEs can illuminate only IMBHs.
• WD TDEs can be probes to search for IMBHs.
0.2M⦿
0.6M⦿
1.2M⦿
Kawana, AT+ 17 (see also Luminet, Pichon 1989 Rosswog et al. 2009; MacLeod et al. 2016)
β=Rt/Rp
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Previous and our studies
• Previous studies
• Demonstration of large amounts of 56Ni yielded
• No convergence check about mass resolution
• No demonstration of shock generation
• Our studies
• Convergence check
• Demonstration of shock generation
Rosswog et al. (2008; 2009)
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SPH simulation• We have performed SPH simulations in the same way as in previous studies, but with higher-mass resolution (Nsph ~ 107)
• The amounts of yielded 56Ni are not converged with increasing Nsph in various WDs.
The number of SPH particles
Iron-group elements [M
☉]
Tanikawa et al. (2017, ApJ, 839, 81)
Nsph=9.8x104 Nsph=6.3x106
ONeMg WD CO WD He WD
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Interpretation• The reason for active nucleosynthesis in low mass resolution
• The number of SPH particles is too small in the direction normal to the orbital plane.
• Distant particles interact incorrectly.
• Artificial viscosity switches on falsely.
• The reason for inactive nucleosynthesis in high mass resolution
• A shock wave should be generated in the outermost part of a WD.
• Our SPH simulation cannot resolve such a thin structure even if Nsph ~ 107.
• Note that SPH simulation does not work well in low-density regions.
Orbital plane
z-axis Supersonic motion
Interact, incorrectly
Supersonic motion
WD surface
Shock wavesToo thin for our SPH
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Switch 3D to 1D• 3D SPH simulation
• 0.45M⦿ HeWD disrupted by 300M⦿ IMBH
• N~3x108 for the He WD
• without nuclear reactions
• Extracting z-columns indicated by white crosses
• 1D mesh simulation
• z-columns
• with nuclear reactions
0.05M⦿
0.01M⦿
Tanikawa (2018, ApJ, 858, 26)
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Movies
Failure case Success case
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Results
Success
Failure
success success success
success success success
success Failure Failure
More than 80% of this WD is detonated.
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Nucleosynthesis
• The detonation wave leaves 20% 4He and 80% 56Ni. • The detonated region has high density (>106 gcm-3).
• The total 56Ni mass is about 0.3M⦿, comparable to SNeIa.
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Summary• We have studied tidal detonation of WDs. • We should be careful of spurious heating in low-resolution SPH simulation (Tanikawa et al. 2017, ApJ, 839, 81).
• We have verified tidal detonation of WDs in the case of He WD with 0.45M⦿ in which large amount of 56Ni (~0.3M⦿) is synthesized (Tanikawa 2018, ApJ, 858, 26).
• WD TDEs can be a clue to search for IMBHs.