Delay time distribution of type Ia supernovae

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Presentation transcript:

Delay time distribution of type Ia supernovae Nicki Mennekens, Dany Vanbeveren, Jean-Pierre De Greve & Erwin De Donder

Type Ia supernovae (SNe Ia) Only in multiple star systems Critical for understanding of galactic chemical evolution Standard candles: validation of LCDM cosmological model Thermonuclear disruption of white dwarf (WD) reaching Chandrasekhar limit Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010

Progenitors: SD vs. DD Single Degenerate: WD pushed over Chandrasekhar limit by accretion from main sequence (MS) or red giant (RG) companion Double Degenerate: merger of two WDs after spiral-in due to gravitational wave radiation emission Which is most dominant (or both)? Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010

Delay Time Distribution DTD = number of SN Ia events per unit time, as function of time elapsed since starburst Measured by observations of elliptical (~starburst) galaxies at similar metallicity and different redshift, e.g. Totani et al. (2008) and Mannucci et al. (2005) Open question: What is contribution of SD and DD in starburst galaxies? T. Totani, T. Morokuma, T. Oda, M. Doi & Y. Yasuda, PASJ 60, 1327, 2008 Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010

Our work Previous studies by Ruiter et al. (2009), Hachisu et al. (2008), Han & Podsiadlowski (2004) and Yungelson & Livio (2000) We investigate influence of mass transfer efficiency b during Roche Lobe Overflow (RLOF) in close binaries Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010

Assumptions Updated evolutionary code of De Donder & Vanbeveren (2004) SD progenitors: as given by Hachisu et al. (2008), including mass stripping effect DD progenitors: every evolution resulting in WD-merger exceeding 1.4 Msun I. Hachisu, M. Kato & K. Nomoto, ApJ 679, 1390, 2008 Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010

Parameter study Fraction b of RLOF-material accepted by accretor Lost matter leaves system with specific angular momentum of second Lagrangian point Energy conversion during common envelope (CE) phase: Webbink (1984) Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010

Typical DD SN Ia evolutions RLOF with b = 1 + CE (SN Ia at 3.4 Gyr) RLOF with b = 0 (no SN Ia) CE + CE (SN Ia at 97 Myr) 4.0+3.6 Msun P = 5.0 d 6.0+5.4 Msun P = 1000 d 0.65+7.0 Msun P = 160 d 0.65+3.6 Msun Merger! 0.91+5.4 Msun P = 5.6 d 0.57+6.7 Msun P = 170 d 0.80+5.4 Msun P = 5.6 d 0.57+0.88 Msun P = 0.19 d 0.80+0.76 Msun P = 700 s Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010

b = 1 Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010

Important results Most SD events created through WD+MS channel, not WD+RG Most DD events created through quasi-conservative RLOF phase followed by CE evolution, as shown by DTDs for different b Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010

Double degenerate Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010

Influence of CE-scenario DTD critically affected by description of CE-evolution: Alpha-scenario of Webbink (1984): balance of energy Gamma-scenario of Nelemans & Tout (2005): balance of angular momentum (for WD-binary evolution) Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010

b = 1, gamma-scenario Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010

Absolute number of SNe Ia Theoretical models underestimate observed rate by factor 2-3 at 11 Gyr May be partially caused by uncertainties on observational conversion factor Possible solution: faster-than-synchronous stellar rotation  heavier MS convective cores (CCs)  heavier WD remnants  more DD SNe Ia Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010

b = 1, CC mass +10% Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010

Conclusions SD alone incompatible with observations Most DD SNe Ia created through quasi-conservative RLOF followed by CE Critical dependence of DTD on mass transfer efficiency during RLOF and physics of CE  way to find out more about these processes? More info: Mennekens et al., A&A, 2010 (arXiv:1003.2491) Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010

Delay time distribution of type Ia supernovae Nicki Mennekens 25/05/2010