Evolution and Final Fates of Accreting White Dwarfs. Ken Nomoto (Kavli IPMU / U. Tokyo)
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1 Evolution and Final Fates of Accreting White Dwarfs Ken Nomoto (Kavli IPMU / U. Tokyo)
2 AD 1572 Korean & Chinese Record Guest Star as bright as Venus (Sonjo Sujong Sillok: Korea)
3 AD 1572 Tycho Brahe s Supernova Stella Nova (Tycho Brahe 1573) Astronomie Populaire by Camille Flammarion (Paris, 1884)
4 Remnant of Tycho s Supernova Green Yellow Blue X-ray (Hot gas with millions of degree) Red Infrared (Circumstellar/ Synthesized dust) (Image: MPIA) White Optical (Foreground/ background stars)
5 Light Echo of SN 1572 (Tycho) Echo: Oort, Zwicky,,,Rest+, Krause+
6 Spectrum of (SUBARU 2008) Echo (Krause, Tanaka, Usuda, Hattori, Goto, Nomoto 2008 Nature) Iron Magnesium Sulfur Silicon Calcium Wavelength (Angstrom)
7 Spectra Bright SN Ia Normal SN Ia Faint SN Ia
8 High Velocity Ca Feature 8
9 The Progenitors of Type Ia Supernovae?? Single Degenerate(SD) vs. Double Degenerate(DD) Chandrasekhar Mass WD vs. Sub-Chandrasekhar Mass WD C He Companion Thermonuclear Explosions of White Dwarfs!!
10 SN Ia: PTF11kx (Dilday et al. 2012)
11 PTF11kx: Symbiotic Recurrent Nova (Dilday et al. 2012) RG wind + Recurrent nova ejecta (P~ 10 yrs) SD (RG+WD)
12 SN Ia : No Companion Star? SNR Tycho (Kerzendorf+ 09) (see, however, Ruiz- Lapuente+ 04) SNR in LMC (Shaefer & Pagnotta 12) SN 2011fe in M101 (Li+ 11) DD?
13 DD, SD Sub-Ch, Chandra surface burning sub-ch Chandra c (g cm -3 ) ~ DD C-detonation? C-det steady C-burning? ONeMg WD no ignition? C-deflag SD He flashes? C-deflag He detonation? C-det
14 Double Degenerates ( M ) SPH Simulations of C+O WD Merging example: N = 4 x 10 6 (Nakasato+ 12)
15 WD Merging ( ) T max Carbon detonation? (Pakmor+ 09, 11) Carbon burning? (Nakasato+ 11)
16 Double Degenerate Scenario Is C-detonation (or He detonation) ignited near the surface? If yes, central C-detonation (Pakmor+ 09, 11) M(eff) ~ M(primary WD) ~ M c ~ g cm -3 sub-chandra If not, ~ steady state
17 WD Merging ( ) T max Carbon detonation? Carbon burning? (Nakasato+ 11)
18 ONeMg WD Double Degenerate Scenario If T max < 6 x 10 8 K (~ surface) C+C rate < Neutrino cooling rate no surface C-ignition (Yoon+2007) central C-ignition (accretion rate?) ( Chandra or super-chandra ) If T max > 6 x 10 8 K (~ surface) C+C rate > Neutrino cooling rate surface C-Ignition ( inward)
19 WD Merging: T max (M 1, M 2 ) Carbon Ignition Neutrino Cooling (Nakasato )
20 Carbon Flame C+O WD O+Ne+Mg WD C+O O+Ne+Mg / M Saio & Nomoto (1985, 1998) (Saio & Nomoto) A&A, ApJ
21 Electron Capture in ONeMg WD 24 Mg(e -,n) 24 Na (e -,n) 24 Ne > gcm -3 collapse
22 Single Degenerate Scenario (1) Compressional Heating M Gravitational Energy Release T WD ignition Compressional Heating M (, T) Thermonuclear Explosions ( M ) Radiative Cooling
23 (2) Nuclear Burning H (1) Steady H-b (2) M > 10-8 M O yr -1 > M Weak H-flashes 10-9 Novae H He Weak He-flashes M < M CH He H M M CH C+O He C+O center Carbon Deflagration He-Detonation
24 Hydrogen Burning in Accreting WD Accretion Rate Nomoto (1982) White Dwarf Mass
25 (3) White Dwarf Wind (Hachisu, Kato, & Nomoto 1996)
26 Stripping of Companion s Mass Mass Transfer Rate reduced Massive (young) Companion SN Ia Circumstellar Matter km/s Hachisu, Kato, Nomoto (2008a) ApJ 679, 1390)
27 Candidate Progenitor Systems for Carbon Ignitors Companion (1) H: leaving M.S. M 2 ~ M 2 / KH (~ M 24 ) ~ M 2,ms ~ 1M 2M ~8M < M (M O yr -1 ) < He H Hachisu, Kato, Nomoto Lee, van den Heuvel Han, Podsiadlowski M 2. > M WD (2) H: sub giant, red giant H-shell b. M 2. < M WD M 2 ~ M 2 / nuclear ~ 10-8 ~ 10-6 M /yr He M
28 SN Ia Progenitor System(MS, RG)
29 Recurrent Nova C-ig: M=1.38 M
30 Single Degenerate Scenario M(wd, 0) + M 2,0 : P 0 (initial orbital period) M(wd, final) [~ 1.38 M ] + M 2 (final) (1) Compressional Heating (M) (2) H & He Burning (3) Radiation-driven WD Winds (4) Steady Hydrogen Burning (5) Recurrent Novae Central Ignition of Carbon Burning
31 Mass Transfer in a SD system (T. Matsuda)
32 Evolution of Rotating White Dwarfs (Uniform rotation) Angular Momentum M(wd) (e.g., Ostriker, Pacynski, Narayan, Hachisu, Piersanti, Yoon, Saio)
33 Structure of Rotating WDs Uniform Rotation M=1.48 M, J=4.63 Rotation Period = 2.3sec ρ c =2.0e9 (Ignition) q=0.66 (Uenishi, Nomoto, Hachisu 03) Differential Rotation M=2.03 M ρ c =2.0e9 (Ignition) (Yoon, Langer 05) Uenishi et al.
34 SD Scenario for Rotating WDs (Spin-up, Spin-down scenario: Justham 11, Di Stehano+ 11, HKN 12) M(wd, 0) + M 2 (P_0) Accretion Spin-Up of WD (uniform rotation) Accretion continues beyond M(wd) = 1.4 M (1) M(wd, final) = 1.5 M (prompt C-ignition) (2) M(wd, final) = M (no C-ignition) dm/dt < 1 x 10-7 M y -1 strong Nova outbursts : mass ejection M(wd) does not increase
35 SNe Ia from Uniformly Rotating WDs (1) M wd, final /M = 1.5 (~ 55 %) : Prompt Carbon-Ignition ( e.g., PTF11kx ) (2) M wd, final /M = (~ 45 %) Spin-down: angular momentum loss ( magnetic wind,,,,,,,) Delayed Carbon-Ignition
36 Uniformly Rotating WDs: Prompt vs. Delayed Carbon-Ignition Prompt C-ig Delayed C-ig Prompt C-ig Delayed C-ig
37 Mass Distribution of Rotating WDs Prompt C-ignition C-ignition (uniform rotation) (differential rotation) Delayed C-ig (Spin down)
38 Companions of Rotating WDs M 2 continues to decrease by mass transfer (~1 x 10-8 M y -1 ) during the spin-down time. (1) RG He WD by losing H-envelope (2) MS low mass MS (M 2 < 1 M ), or He WD by losing H-envelope Companions become low mass, compact stars: missing companions Circumstellar matter : dispersed.
39 Single Degenerate Scenario Rotating White Dwarfs Prompt & Delayed Carbon Ignition Spin-up, Spin-down scenario can solve the missing companion problem. - mechanism & timescale of spin-down (e.g., Ilkov & Soker 11)
40 Nucleosynthesis in Chandrasekhar Mass Models 56 Ni 56 Fe c > 10 9 g cm Ni r Carbon deflagration at NSE & Electron Capture lower Y e (neutron-rich) 58 Ni, 56 Fe Late time spectra: Ni, Fe Nuclear Statistical Equilibrium (NSE: Y e )
41 Chandrasekhar Mass Models Urca cooling Higher c 25 Mg<-> 25 Na, 23 Na<-> 23 Ne : high metallicity smaller M(wd,0) Delayed C-ig Higher c more 58 Ni, 56 Fe Late time spectra: 58 Ni, 56 Fe Type Iax (2002cx-like)? (Foley+13) low M(ej), M( 56 Ni), E 3D higher c Ejecta + Bound WD remnant (Jordan+12; Kromer+13)
42 URCA cooling (ONeMg core) 25 Mg<-> 25 Na 23 Na<-> 23 Ne (Jones+13)
43 SN Ia Late-Time Spectra Optical: Leloudas+ 09 NIR: Motohara+ 06
44 Electron capture elements (Maeda+ 10)
45 SUBARU/OHS observations of SNe Ia 05W, 03du, 03hv (Motohara )
46 (Jha 2013)
47 DD, SD Chandra, Sub-Ch surface burning sub-ch Chandra c (g cm -3 ) ~ [late time 58 Ni, 56 Fe] DD C-detonation? C-det steady C-burning? ONeMg WD no ignition? C-deflag Prompt and Delayed C-ignition SD He flashes? C-deflag He detonation? C-det
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