1 / 27

Supernovae of type Ia: the final fate of low mass stars in close bynary systems Oscar Straniero INAF – Oss. Astr. di Co

Supernovae of type Ia: the final fate of low mass stars in close bynary systems Oscar Straniero INAF – Oss. Astr. di Collurania (TE). CMB Temperature fluctuations (COBE B OOMERANG WMAP ). High-z Team (Brian Schmidt & co). Supernova Cosmology Project . (Saul Perlmutter & co.).

emery
Download Presentation

Supernovae of type Ia: the final fate of low mass stars in close bynary systems Oscar Straniero INAF – Oss. Astr. di Co

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Supernovae of type Ia: the final fate of low mass starsin close bynary systemsOscar Straniero INAF – Oss. Astr. di Collurania (TE)

  2. CMB Temperature fluctuations (COBE BOOMERANG WMAP)

  3. High-z Team (Brian Schmidt & co) • Supernova Cosmology Project (Saul Perlmutter & co.) 0.25 mag fainter than for an EMPTY Universe Fainter = Further The Universe is Accelerating:

  4. Standard Model CMB + SNe + H0 = LCDM model

  5. SNe + CMB SNe: Perlmutter et al. 1998, Riess et al. 1998 14.5"1 Gyr (Ho=63) SNe+WMAP+HST 13.2"0.4 Gyr (Ho=71) Spergel et al. 2003 13.7"0.2 Gyr

  6. II p Type II H Core collapse of massive stars II L SNe I b (strong He) I c (weak He) No H Type I Thermonuclear explosion I a (strong Si) based on spectra and light curve morphology SNe Classification

  7. Standard Candles • Bright • Homogeneous • No evolutionary effects Supernovae Ia  Thermonuclear Explosion of a CO WD M~MChandrasekhar Light Curve L 56Ni 56Co 56 Fe ~ 1.4 M time L  MNi

  8. Riess et al. , 1997 Brighter Slower Decline Dimmer Faster Decline Observed Relations

  9. Maximum Brightness - Decline Relation Phillips et al. 1996, 1999 <> = 0.17 mag Calibrated locally

  10. Hamuy et al., 2000 Ivanov et al. 2000 Do Supernovae change with z ?? Hints... • SN Ia rate is smaller in Ellipticals Cappellaro et al. 1997 • SN Ia LCs Slower (brighter) in Bluer Galaxies • Hamuy et al. , 1995, 1996 • Branch et al. 1996 Back in time>>Progenitors Younger & more metal-poor

  11. The conceptually simplest model for a thermonuclear supernova is just an analog of a runaway chemical reaction that become explosive : a conventional bomb. …… bombs often fail. Similarly, most models for astrophysical bombs (Sne Ia) often fail. …… Further, astrophysical bombs must occur naturally and at the correct rate: there must be a convincing astronomical context.

  12. Non-degenerate log P r4/3 relativistic M2 M1 r5/3 Non-relativistic log r collapse The virial theorem

  13. Massive stars and core collapse Limongi, Straniero & Chieffi, 2001 • e-+p à n+ne (10 MeV) • 56Fe+g à 13a+4n (124 MeV)

  14. PN 0.6 CO 0.5 He AGB 0.55 He 0.2 CO 0.6 CO HB RGB 0.1 He WD MS Evolutionary track of low mass stars M=1 Mu t=10 Gyr Remnant: CO WD 0.6 Mu Prada Moroni & Straniero 2002

  15. M<0.8 M¤ 0.8<M/M¤<8 8<M/M¤<11 11<M/M¤<100 M>100 M¤ t>1/HO 15 Gyr<t<30 Myr 0.5<Mf /M¤<1.1 CO WD t.10-30 Myr Mf =1.2-1.3 M¤ ONeMg WD t.1-10 Myr Mf =1.2-2.5 M¤ Fe (Ye.0.45) collapse NS or BH t#1Myr O (pair jnstability) (Ye=0.5) may or may not explode Stellar evolution

  16. RG C or He detonation WD C-deflagration WD WD C-delayed detonation Induced Core collapse (nuclear runaway fails) Pair instability, core collapse & O explosion (core collapse fails) Astrophysical Explosive Devices Thermonuclear SNe Gravitational collapse

  17. He-detonation Nucleosynthesisin Thermonuclear SNe C-deflagration C-delayed detonation

  18. SNe Ia Light Curves: mass and metallicity effects Domínguez, Hoflich, Straniero 2001

  19. RG MS H accreting WDs Most of the accreted material is lost during the H-pulse: too long time

  20. Merging scenario:Double degenerate systems: CO+CO a) GWR loss b) secondary tidal disruption c) accretion 10-5 Myr-1 Too fast accretion

  21. Double Degenerate CO WDs (M=8H10-6 Myr-1) (M=10-8 Myr-1)

  22. Single Degenerate.Massive WDs: the lifting effect of rotation H He CO Dominguez, Straniero, Isern & Tornambe’ 1996

  23. d e c f g ---- disk ----WD Double DegenerateAngular momentum deposition & GWR c) accretion 10-5 Myr-1 (expansion) d) “critical” accretion (contraction) e) tri-axial configuration and energy loss via GWR f) balance between ang. mom. deposition and energy loss (steady accretion) g) Viscous dissipation and explosion Piersanti, Gagliardi, Iben & Tornambe’ 2003

  24. Our main results for SNe Ia: Up toMMAX =0.2 mag C/O WDs due todifferent MMS correlated withvph & trise No dependence of MMAX with initial Z • Open Problems: • Progenitors ?? Accretion, Rotation. • Propagation of the burning front (1D/3D) ?? Transition density • How stellar populations evolve with z ??

  25. The future

More Related