Explosive Events in the Universeand H-Burning

Jordi José
Dept. Física i Enginyeria Nuclear, Univ. Politècnica de Catalunya (UPC),& Institut d’Estudis Espacials de Catalunya (IEEC), Barcelona

Nuclear Astrophysics

Type Ia (or thermonuclear) Supernovae [SN Ia]
WDClassical Nova Outbursts [CN]X-Ray Bursts [XRBs]: NSJ. José

J. José

Nuclear Astrophysics

Stellar Mergers and Collisions

Detonations in white dwarf dynamic interactions
Aznar-Siguán, García-Berro, Lorén-Aguilar, JJ &Isern, MNRAS (2013)
Guerrero, García-Berro & Isern, A&A (2004)

f ~ f(SNIa in spiral galaxies)

Explosive Events in the Universe and H-Burning
Type Ia Supernovae || Classical Novae || Type I X-Ray Bursts

I. Type Ia Supernovae

J. JoséExplosive Events in the Universe and H-Burning
Type Ia Supernovae || Classical Novae || Type I X-Ray Bursts

J. JoséThermonuclear Supernovaev ∼ 104 km/s, LPeak ~ 1010 L, E ∼ 1051 erg, Mej = 1.4 M
no remnant left
* homogeneity: ∼70% of all SN Ia have similar spectra, light curves
and peak absolute magnitudes (Li et al. 2011): diversity of SNIa
progenitors??
* main Fe factories in the Universe (> SN II)* Scenario: not fully understood- Single degenerate scenario: WD + ‘Normal’ companion(H or He accretion)- Double degenerate scenario: WD + WD
(He or C-O accretion)

Explosive Events in the Universe and H-Burning

J. JoséType Ia Supernovae || Classical Novae || Type I X-Ray Bursts

Thermonuclear Supernovae: Nucleosynthesis
Supernovae are crucial for life... But never get too close!
Parikh, JJ, Seitenzahl & Röpke,A&A (2013)

443 isotopes (H − Kr); 5267 links

Explosive Events in the Universe and H-Burning
Type Ia Supernovae || Classical Novae || Type I X-Ray Bursts

J. JoséW7 DDT W7+DDT

Nuclear Uncertainties

Parikh, JJ, Seitenzahl & Röpke,A&A (2013)

Explosive Events in the Universe and H-Burning
Type Ia Supernovae || Classical Novae || Type I X-Ray Bursts

II. Classical Novae

J. JoséExplosive Events in the Universe and H-Burning

J. JoséType Ia Supernovae || Classical Novae || Type I X-Ray Bursts

Novae have been observed in all wavelengths (but detected in γ-rays
only at E > 100 MeV)

The Classical Nova ID Card
Moderate rise times (<1 – 2 days):
8 – 18 magnitude increase in brigthness

LPeak ~ 104 – 105 L
Stellar binary systems: WD + MS
(often, K-M dwarfs)
Recurrence time: ~ 10 yr (RNe) –105 yr (CNe)Frequency: 30 ± 10 yr-1
[Observed frequency: ~ 5 yr-1]
E ∼ 1045 ergs
Mass ejected: 10-4 – 10-5 M
(~103 km s-1)

Nova Cygni 1975

Explosive Events in the Universe and H-Burning
Type Ia Supernovae || Classical Novae || Type I X-Ray Bursts

The Nova Nuclear SymphonyClassical Novae: ~100 relevant isotopes(A<40) & a (few) hundred nuclear
reactions (Tpeak ~ 100 – 400 MK)
Nova Cygni 1992

Novae as unique stellar explosions forwhich the nuclear physics input is (willbe) primarily based on experimental
information (JJ, Hernanz & Iliadis,Nucl. Phys. A 2006)

J. JoséCa

Model 1.35 M
(50% ONe enrichment)

K
Ar
Cl

T = 3.2×108 K
Tpeak2-3
ρ = 5.1×10 g cm
εnuc = 4.3×1016 erg g-1 s-1
SiΔMenv = 5.4×10-6 M

Endpoint ~ CaS
P20heavy metals17 18 19No

produced!

15 16
Al
Negligible contribution from anyMg(p,γ)(n,γ) or (α,γ) reaction (that alsoNa
13 14
Zapplies
to 15O(α,γ)!)Ne11 12F
Fuel (H) is not fully consumed in(β+)(p,α)
Othe explosion
9 10N
8C
T =(Reaction
1 x 107Fluxes)
KLog
7
B
: -2
Main
nuclear path: -3
6close to the valley ofBe
: -4
5 stability, and driven by
Li: -53 4
He: -6(p,γ), (p,α) and β+: -7Hinteractions
012N

Degeneracy LiftingTTρρTbase = 3×107 KTTψψρψT

JJ (2015),in preparation

ψρρ

Tρ

NCNOOCLiAlNeLiNaNe Mg
AlNaSiH HeSiPClMg
PClK
S Ar CaHK
S Ar CaFFB

HeB

1.15 M ONe

1.15 M CON

O
PLiCSiNa

AlClS

NeFAr
HBMg

K

He

JJ (2015), in preparation

1.35 M ONeCa

Explosive Events in the Universe and H-Burning
Type Ia Supernovae || Classical Novae || Type I X-Ray Bursts

J. JoséNuclear Uncertainties

Main nuclear uncertainties: [18F(p,α)15O, 25Al(p,γ)26Si, 30P(p,γ)31S]

Explosive Events in the Universe and H-Burning
Type Ia Supernovae || Classical Novae || Type I X-Ray Bursts

J. JoséPhys. Rev. C, submitted

Explosive Events in the Universe and H-Burning

J. JoséType Ia Supernovae || Classical Novae || Type I X-Ray Bursts

τ ~ 1.04 Myr

26Al

26Al

26Mg*

26Mg

1.809 MeVCOMPTEL measurements:
map of the 1.809 MeV
emission in the Galaxy(Diehl et al., A&A, 1995;
Prantzos & Diehl, Phys.
Rep. 1996)
Galactic 26Al related to young progenitors
SN II vs. WR stars:
Diehl (2004), Diehl et al. (2006)
But 60Fe?

Explosive Events in the Universe and H-Burning
Type Ia Supernovae || Classical Novae || Type I X-Ray Bursts

J. JoséExplosive Events in the Universe and H-Burning
Type Ia Supernovae || Classical Novae || Type I X-Ray Bursts

J. José18F* γ-ray signature: 18F decay (T1/2 ~ 110 min) provides a source of
gamma-ray emission at 511 keV and below (related to electronpositron annihilation).
But! Uncertainties in the rates
translate into a factor ∼ 5 - 10
1.15 Mo CO
uncertainty in the expected fluxes!

Gómez-Gomar, Hernanz, JJ, &Isern (1998), MNRAS

D= 1 kpc

Explosive Events in the Universe and H-Burning
Type Ia Supernovae || Classical Novae || Type I X-Ray Bursts

J. JoséMultidimensional Models

Zmean ~ 0.2 – 0.3

Multi-D Hydro Simulations with the FLASH CodeMovie available at: http://www.fen.upc.edu/users/jjose/Downloads.html

Kelvin-Helmholtz instabilities

Explosive Events in the Universe and H-Burning
Type Ia Supernovae || Classical Novae || Type I X-Ray Bursts

III. Type I X-Ray Bursts

J. JoséExplosive Events in the Universe and H-Burning
Type Ia Supernovae || Classical Novae || Type I X-Ray Bursts

J. JoséNucleosynthesis
in Type I X-Ray Bursts
Santa Fe, NMNSTpeak > 109 K, ρmax ~ 106 g.cm−3

Detailed nucleosynthesis studies require hundreds of isotopes, up toSnSbTe mass region (Schatz et al. 2001) or beyond (the flow in
Koike et al. 2004 reaches 126Xe), and thousands of nuclear
interactions
Main nuclear reaction flow driven by the rp-process (rapid p-capturesand β+-decays), the 3α-reaction, and the αp-process (a sequence of(α,p) and (p,γ) reactions), and proceeds away from the valley ofstability, merging with the proton drip-line beyond A = 38 (Schatz etal. 1999)

Explosive Events in the Universe and H-Burning

J. JoséType Ia Supernovae || Classical Novae || Type I X-Ray Bursts

MODEL 3
1.4 M, 1.8 10-9 M.yr-1, Z=10-3

Type I XRB: JJ, Moreno, Parikh & Iliadis (2010), ApJSExplosive Events in the Universe and H-Burning
Type Ia Supernovae || Classical Novae || Type I X-Ray Bursts~ 50,000 post-processing calculations [21 CPU months!]
606 isotopes (1H to 113Xe) and 3551 nuclear processes

J. JoséExplosive Events in the Universe and H-Burning
Type Ia Supernovae || Classical Novae || Type I X-Ray Bursts

J. JoséThank you for your attention!

Explosive Events in the Universe and H-Burning
2nd Conference on Advances in Radioactive Isotope Science (ARIS2014)
Tokyo (Japan), June 4, 2014