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On the nuclear astrophysics from astrophysics

perspective

Andrzej Odrzywołek

Dept. of General Relativity & Astrophysics

22 May 2018

(n,γ) (d,γ)

(n,γ)

(n,γ)

(p,γ) (p,γ)

(p,γ) (ν,e-) (e+,

ν) free decay

(d,p) (n,p) (d,n)

To Be 7

From Be 7 From Be

8

From Li 7

To Li 7 Exoergic Direction

(d,p) (t,pn) (He3,2p) (He4 ,γ)

(d,n) (He3,pn) (t,2n) (n,He

4 ) (γ,He

4 ) (p,He 4 )

(He4 ,γ)

p d

He3 He4

t

n

78Ni 80Zn 79Cu 81Ga

82Ge 80Ge

68Ni 66Ni

60Fe 54Cr

58Fe 56Fe 54Fe

56Ni 55Co

0.4 0.5

0.001 0.005 0.010 0.050 0.100 0.500 1.000

Ye

Abundance

kT=0.5 MeV, lg Ρ=10 @gcm3D

ƒ

0.2 0.3

0.4

0.4 0.45

0.45

0.5

0.5 0.5

0.55 0.6

0.7

0.8

0.3 0.4 0.5 0.6 0.7 0.8 0.9

4 6 8 10

kT @MeVD lgΡ@gcm3D

(2)

Why Nuclear Astrophysics?

1 Big Bang Nucleosynthesis

2 Nuclear Evolution of the Universe (production of elements)

3 Stellar Amnesia (thermodynamic equlibrium)

4 Supernovae, Novae, Kilonovae

5 Neutrino emission, evolution of neutron excess

6 Neutron stars: interiors, pasta phases, EOS

7 Pyconuclear reactions, explosive hydrogen burning

8 Rotating liquid drop models vs rotating stars/disks

9 Extrasolar planet composition: super-Earths, blue ocean, etc.

(3)

Astronomy vs Astrophysics

(4)

Big Bang Nucleosynthesis

Three stages

1 p, n in thermodynamic equilibrium (∆ “ 1.2933 MeV) Nn

Np “ e´mnc2{kT

e´mpc2{kT “ e´∆{kT

2 weak freezeout (kT » 0.7 MeV), neutron decay/ d , t,3He photodisintegration (20kT ą 2.2MeV )

p ` e´Ø n ` νe, n Ø p ` e´` ¯νe, p ` ¯νe Ø n ` e`

3 full nuclear reaction network in expanding matter

(n,γ) (d,γ)

(n,γ)

(n,γ)

(p,γ) (p,γ)

(p,γ) (ν,e-) (e+, free decayν)

(d,p) (n,p) (d,n)

To Be 7

From Be 7 From Be

8 From Li 7

To Li7 Exoergic Direction

(d,p) (t,pn) (He3,2p) (He4 ,γ)

(d,n) (He3,pn) (t,2n) (n,He

4 ) (γ,He

4 ) (p,He 4 )

(He4 ,γ)

p d

He3 He4

t

n

(5)

Weak freezeout

Proton/neutron mixture kinetics

dnnptq

dt ` 3Hptqnn“ ´λenn` λp ¯νenp´ λβ´nn` λpe´ν¯enp´ λne`nn` λpe´np

dnpptq

dt ` 3Hptqnp“ `λenn´ λp ¯νenp` λβ´nn´ λpe´ν¯enp` λne`nn´ λpe´np

Hptq - Hubble „constant”; nnptq, npptq - number density of neutrons and protons; λi - reaction rate.

All reaction rates are remarkably similar, e.g:

λe “ ln 2 xftym5e

ż8

pEe` ∆q2Eea

Ee2´ m2e 1 ` epEe´∆q{kT

ˆ

1 ´ 1

1 ` eEe{kT

˙ dEe

and except for phase-space/blocking factors can be tracked down do free neutron lifetime!

(6)

Weak freezeout

Proton/neutron mixture kinetics

dnnptq

dt ` 3Hptqnn“ ´λenn` λp ¯νenp´ λβ´nn` λpe´ν¯enp´ λne`nn` λpe´np

dnpptq

dt ` 3Hptqnp“ `λenn´ λp ¯νenp` λβ´nn´ λpe´ν¯enp` λne`nn´ λpe´np

Hptq - Hubble „constant”; nnptq, npptq - number density of neutrons and protons; λi - reaction rate.

All reaction rates are remarkably similar, e.g:

λβ´ “ ln 2 xftym5e

ż me

pEe` ∆q2Ee

aEe2´ m2e 1 ` e´Ee{kT

ˆ

1 ´ 1

1 ` eEe{kT

˙ dEe

and except for phase-space/blocking factors can be tracked down do free neutron lifetime!

(7)

Importance of neutron lifetime

BBN uncertainties

BBN now (could) become zero-parameter (?) model:

1 traditional BBN free parameter, baryon-to-photon ratio PDG2015, [PDG2018, 95% CL (2σ)]:

η ” nB

nγ » 6.05 ˘ 0.07 ˆ 10´10, 6.2 ˘ 0.4 ˆ 10´10 which determine initial conditions for BBN reaction network, now known from Cosmic Microwave Background/Planck satellite.

2 number of neutrino families:

Nν “ 2.984 ˘ 0.008 known from CERN LEP.

3 lifetime of neutron measured:

τn“ 880.2 ˘ 1.0 seconds.

(8)

Neutron lifetime

(9)

Notable BBN software

Kawano, PArthENoPE - original Wagoner/Hoyle code and clones, http://parthenope.na.infn.it/

Alter BBN, https://alterbbn.hepforge.org/

PRIMAT - Mathematica code, https://arxiv.org/abs/1801.08023 F.X.Timmes BBN code,

http://cococubed.asu.edu/code pages/net bigbang.shtml Experiments devoted to improve low-energy cross-sections, e.g:

d pp, γq3He

1 LUNA (Laboratory for Underground Nuclear Astrophysics), Laboratori Nazionali del Gran Sasso (LNGS), Italy

(10)

Hydrogen burning: ppI cycle

p ` p Ñ d ` e`` νe reaction rate λpp

p ` d Ñ 3He ` γ reaction rate λpd

3He `3He Ñ α ` 2p reaction rate λ33

Kinetic equations:

n9p“ ´2λppnp2´ λpdnpnd` 2λ33n23 n9d“ `λppn2p´ λpdnpnd

n93“ `λpdnpnd´ 2λ33n23 n9α“ λ33n23

Baryon number conservation:

ÿ4 i “1

Aini “ np` 2nd` 3n3` 4nα“ const,

n9p` 2 9nd ` 3 9n3` 4 9nα “ 0.

(11)

From cross-section/S-factor to reaction rate

λ9 ż8

0

e´kTE σpE qE dE “ ż8

0

e´kTE S pE q

E e´2πηE dE

Boltzmann distribution e´kTE (thermal energy tail) Sommerfeld parameter (v “a

2E {m - relative velocity): (quantum electrostatic barrier tunneling)

η “ αZ1Z2

v {c Z1Z2 20v

(12)

General nuclear burning: hardwired vs soft-wired

With increased amount of measured/computed nuclei and

cross-sections reaction networks become prohibitively complicated and poorly understood. Statistical methods can help!

NP

N P

487 Isotopes 5892 Rates 96.4% Sparse Flows (#/sec):

5.14E+15 1.80E+12 6.28E+08 2.20E+05 7.68E+01 -3.72E+01 -1.07E+05 -3.05E+08 -8.71E+11 -2.49E+15 -7.13E+18 (n,γ)

(α,p) (α,γ) (α,n) (p,γ) (p,n)

(γ,p) (p,α)

(γ,α) (n,α) (γ,n)

(n,p)

See e.g. http://cococubed.asu.edu/code pages/net torch.shtml

(13)

Nuclear Statistical Equilibrium

idea dates back to F. Hoyle, „nuclear statistical mechanics”

„The synthesis of the elements from hydrogen”, MNRAS, 106 (1946) 343.

Hoyle proposed two pathways to nucleosynthesis theory:

1 find equilibrium for known objects [in 1946 just stars]

2 analyze whole T ´ ρ plane, select interesting regions then look for appropriate phenomena in cosmos [now: stars,

thermonuclear & core-collapse supernovae, novae, X-ray bursts, NS-NS mergers, Big Bang, cosmic-ray, ...?]

P. Holfich coined „stellar amnesia” idea - regardless of complicated history matter finish in equilibrium state

in famous B2FH articleSynthesis of the Elements in Stars, E. Burbridge, G. Burbridge, W.

Fowler, F. Hoyle, Rev. Mod. Phys. 29 (1957) 547 NSE is referred to as e-Process.

above article established Nuclear Astrophysics as separate branch of physics; many nuclear physicists retrained as

astrophysicists, incl. H. Bethe and many our colleagues here in Cracov e.g. K. Grotowski

(14)

NSE: assumptions

1 Full equilibrium determined by 2 parameters T and ρ only (baryon number B and electric charge Q conservation) is very rare, because of properties of neutrinos.

2 additional parameter is required, related to [electron] lepton number Le conservation

3 usually it is either neutron excess η or lepton-to-baryon number ratio Ye:

η “ Nn´ Np

NB , Ye “ Ne

NB ” Np

NB, η “ 1 ´ 2Ye

4 Ye is assumed constant because:

1 slow weak interactions compared to strong interactions

2 kinetic β equilibrium: identical νe and ¯νe emission

(15)

NSE: equations

Niso

ÿ

k“0

Xk “ 1 (1a)

Niso

ÿ

k“0

Zk Ak

Xk “ Ye (1b)

Abundance Xk k-th nuclide of atomic number Zk and mass number Ak:

Xk “ 1

2GkpT qˆ 1 2ρNAλ3

˙Ak´1

Ak5{2XnAk´ZkXpZkeQkkT. (2) Temperature-dependent partition function:

GkpT q “

imax

ÿ

i “0

p2Jik ` 1qe´EikkT (3)

(16)

NSE: solution

1 two unknowns: proton and neutron abundance Xp and Xn

2 very high order polynomial system (up to XA, e.g.238U)

3 basic nuclear structure enough:

nuclear mass or binding energy ground state spin

excited energy levels and spins

4 input variables: T ´ ρ ´ Ye triad

(17)

NSE: viewgraphs

n p

4He 58Fe

54Cr

50Ti

0.2 0.4 0.6 0.8 1.0

0.001 0.005 0.010 0.050 0.100 0.500 1.000

kT @MeVD

Abundance

Ye=0.45, lg Ρ=6 @gcm3D

(18)

NSE: viewgraphs

n

p 56Ni

78Ni

54Fe 56Fe

80Zn

55Co

3Li

82Ge

0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9

0.2 0.4 0.6 0.8 1.0

Ye

Abundance

kT=0.5 MeV, lg Ρ=10 @gcm3D

(19)

NSE: viewgraphs

78Ni

80Zn

81Ga 79Cu

82Ge 80Ge

68Ni 66Ni

60Fe

54Cr

58Fe 56Fe 54Fe

56Ni 55Co

0.4 0.5

0.001 0.005 0.010 0.050 0.100 0.500 1.000

Ye

Abundance

kT=0.5 MeV, lg Ρ=10 @gcm3D

ƒ

(20)

Explosive phenomena in the Universe

1 either by kinetic equations or equilibrium methods we are able to find conditions responsible for a subset of produced nuclei

2 most sites are now established

3 it is not enough to produce elements — they must be ejected/spread into the Galaxy

4 we must enter formidable area of numerical simulations of supernovae, novae , compact object (black holes, neutron stars, white dwarfs) mergers and accretion disks

5 nuclear physics provides essential input data in form of:

nuclear cross-sections / reaction rates binding energies and structure of nuclei weak interaction rates (β decays, e˘captures)

last but not least: Equation Of State for nuclear matter

(21)

Supernovae

Two physical types of supernova

Given two known primary sources of energy in the Universe:

1 Thermonuclear supernova - nuclear explosion or even detonation of the whole star [Type Ia, PISN?]

2 Core-Collapse supernova - gravitational collapse of the central region of the star [Type Ib/c, II, long-GRB]

Crash-course in stellar evolution:

burn H Ñ He Ñ C/O Ñ „iron” as far as initial mass goes UP if M ă Md He white dwarf forms with M ă Md

if 1Mdă M ă 8Md C/O white dwarf forms with M » Md if M ą 8Md iron white dwarf forms at the center with Mdă MFeă 2Md and subsequently collapse to neutron star if M " 25Md quiet collapse to a black of a whole star [or possibly thermonuclear explosion of massive C/O core]

(22)

Type Ia (thermonuclear) supernova

1 every white dwarf is a ticking unexploded bomb waiting for

„ 109 years for explosion

2 slow-match fuse is either accretion from companion star in binary system, or emission of gravitational waves

3 after ignition mass threshold, explosive thermonuclear burning front incinerate whole star in few seconds

(23)

Deflagration-Detonation Transition: click:[D-D-T]

White dwarf merger: click:[WD Merger]

(24)

[Core-Collapse] Super-Nova

Baade&Zwicky (1930-40) find and name several supernovae final distinction between classical novae [Galactic] and super-novae [extragalactic]

they correctly (!) guess physical explosion mechanism: collapse to pure neutron object (neutron discovery: 1932)

finally super-nova becomes supernova

true Zwicky’s motivation for name still mystery

(25)

[Core-Collapse] Super-Nova

Baade&Zwicky (1930-40) find and name several supernovae final distinction between classical novae [Galactic] and super-novae [extragalactic]

they correctly (!) guess physical explosion mechanism: collapse to pure neutron object (neutron discovery: 1932)

finally super-nova becomes supernova

true Zwicky’s motivation for name still mystery

(26)

[Core-Collapse] Super-Nova

Baade&Zwicky (1930-40) find and name several supernovae final distinction between classical novae [Galactic] and super-novae [extragalactic]

they correctly (!) guess physical explosion mechanism: collapse to pure neutron object (neutron discovery: 1932)

finally super-nova becomes supernova

true Zwicky’s motivation for name still mystery

(27)

[Core-Collapse] Super-Nova

Baade&Zwicky (1930-40) find and name several supernovae final distinction between classical novae [Galactic] and super-novae [extragalactic]

they correctly (!) guess physical explosion mechanism: collapse to pure neutron object (neutron discovery: 1932)

finally super-nova becomes supernova

true Zwicky’s motivation for name still mystery

(28)

[Core-Collapse] Super-Nova

Baade&Zwicky (1930-40) find and name several supernovae final distinction between classical novae [Galactic] and super-novae [extragalactic]

they correctly (!) guess physical explosion mechanism: collapse to pure neutron object (neutron discovery: 1932)

finally super-nova becomes supernova

true Zwicky’s motivation for name still mystery

(29)

Core-collapse with GR1D

(30)

Core-collapse with GR1D

(31)

Core-collapse with GR1D

(32)

Core-collapse with GR1D

(33)

Core-collapse with GR1D

(34)

Core-collapse supernova problem

Supernova problem

1 so-called prompt supernova mechanism generally do not work, except for very soft EOS (K ! 200 MeV) and low-end stellar mass (8Mdă M ă 11Md with O-Ne-Mg core)

2 in typical situation shock retreat with infalling envelope with no explosion at all [quiet collapse]

3 above is in contradiction to hundreds of observed supernova events every year

(35)

Possible solutions include:

neutrino mechanism 2D/3D turbulence/ SASI neutron star rocket effect magnetic/rotation/jet [supernova remnants with ears]

(36)

Possible solutions include:

neutrino mechanism 2D/3D turbulence/ SASI neutron star rocket effect magnetic/rotation/jet [supernova remnants with ears]

(37)

Possible solutions include:

neutrino mechanism 2D/3D turbulence/ SASI neutron star rocket effect magnetic/rotation/jet [supernova remnants with ears]

(38)

Possible solutions include:

neutrino mechanism 2D/3D turbulence/ SASI neutron star rocket effect magnetic/rotation/jet [supernova remnants with ears]

(39)

Neutron star mergers (kilonova)

(40)

Neutron star mergers (kilonova)

(41)

Neutron star mergers (kilonova)

(42)

Neutron star mergers (kilonova)

(43)

Neutron star mergers (kilonova)

(44)

Conclusions

1 connection and influence from/to nuclear physics Ø astrophysics still strong

2 active research area related to r -process (Neutron Star mergers) and rp-process (explosive H burning)

3 huge amount of cross-sections, weak rates, masses measured and computed (incl. radioactive) . . .

4 . . . but a lot of effort required to use them, including purely technical/IT problems

5 significant lag between experimental knowledge (e.g. nuclear EOS, neutrino oscillations) and full astrophysical

implementation still persists due to historical reasons and legacy codes

(45)

Thank you!

(46)

Beyond simple H burning

H-burn in the Sun (pp-cycles) is well understood and experimentally confirmed (cf. our Borexino team)

CNO-cycle (catalyzed) is well understood, but CNO-neutrinos still not confirmed

standard CNO powers stars more massive than 2 Md

hot-CNO (explosive H burning) powers classical novae and X-ray bursts

explosion is a result of H accumulation on surface of compact degenerate object: white dwarf or neutron star

rp-process (rapid proton capture) operates at T ą 109 K reaction networks become complicated and might involved short-lived α-unstable nuclei

another intriguing case is H-burning in first stars after Big Bang yet another unexplored idea is antineutrino-accelerated hot H-burning:

¯

νe` p Ñ n ` e` imaginable e.g. after merger of massive starsA. Odrzywołek Nuclear astrophysics

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