INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium...

23
INDRA GANIL experiments: Equilibrium constants “Valid treatment of the correlations and clusterization in low density matter” R. Bougault, LPC Caen INDRA collaboration (work related to Quin et al. publication Texas A&M) RIN FIDNEOS

Transcript of INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium...

Page 1: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

INDRA GANIL experiments:

Equilibrium constants“Valid treatment of the correlations and clusterization in low density matter”

R. Bougault, LPC Caen

INDRA collaboration

(work related to Quin et al. publication Texas A&M)

RIN FIDNEOS

Page 2: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Astrophysics: life cycle of a star

Page 3: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Light and Heavy clusters are present

• In inner crust of neutron stars (cold stellar matter)

• In core-collapse supernova matter (warm nuclear matter)

Astrophysics: life cycle of a star

Page 4: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Core Collapse: electron capture on protons (free or within nuclei) reduces the electronfraction and realeases neutrinos.Trapping of neutrinos could halt the process: reabsorption of the neutrinos on neutrons (free or within nuclei) - neutrino opacity.

Astrophysics: CCSNe

Cold Neutron Star

2.Neutronization &

by

emission

csm.ornl.gov

Cooling

neutrino

EXPLOSION of CORE COLLAPSE SUPERNOVAEAccretion of matter onto the central object, known as the proto-neutron star (hot and lepton rich)

Page 5: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Clusters influence supernova properties: the clusters can modify the neutrino transport, affecting the cooling of the proto-neutron star.

Astrophysics: CCSNe

Cold Neutron Star

2.Neutronization &

by

emission

csm.ornl.gov

Cooling

neutrino

EXPLOSION of CORE COLLAPSE SUPERNOVAEAccretion of matter onto the central object, known as the proto-neutron star (hot and lepton rich)

Page 6: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Actual CCSNe Nuclear Statistical Equilibriummodels does not include d, t, 3He, Li light clusters.

Astrophysics: CCSNe

Cold Neutron Star

2.Neutronization &

by

emission

csm.ornl.gov

Cooling

neutrino

EXPLOSION of CORE COLLAPSE SUPERNOVAEAccretion of matter onto the central object, known as the proto-neutron star (hot and lepton rich)

Page 7: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Color: electron fraction

• From Symmetric matter (0.5) red

• To Neutron matter (0) blue

T. Fischer et al. Astro. Phys. Journal 194:39 (2011)

Phase space covered in

Core-Collapse Supervova

simulations

Astrophysics: supernova modelisation

Questions for nuclear physics: what is the chemical composition at these densities and temperatures & measure in medium effects.

15 MSUN progenitor

1st second

post-bounce evolution

TE

MP

ER

AT

UR

E (

MeV

)

Baryon DENSITY (fm-3)

Page 8: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

TE

MP

ER

AT

UR

E (

MeV

)

Baryon DENSITY (fm-3)

Color: electron fraction

• From Symmetric matter (0.5) red

• To Neutron matter (0) blue

T. Fischer et al. Astro. Phys. Journal 194:39 (2011)

Phase space covered in

Core-Collapse Supervova

simulations15 MSUN progenitor

Astrophysics: supernova

HEAVY ION COLLISIONS

Page 9: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

How to create low density nucl. matter

STUDY of a Gas

composed of light clusters

formed

in central collisions

INDRA@GANIL136,124Xe+124,112Sn 32 A MeV

Treatment of the gas material in a statistical/equilibrium

framework(equilibrium demonstration: R. Bougault et al. PRC 97(2018)024612)

136Xe

There is

• Temperature & expansion:

hot expanding source

• Coulomb effects:

corrections to go back to the

original velocity spectra at

cluster creation time

Page 10: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Original velocity spectra at cluster creation time

1- Coulomb correction

The velocity is a clock:

each velocity bin

represents the state of

the evolving source at

a given time.

2- Hot expanding source

J. Wang et al. PRC72 (2005) 024603

<E

mis

sio

n tim

e>

(fm

/c)

AMD-V model

Page 11: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Statistical/equilibrium framework

For each Vsurf bin (i.e. time)1- Temperature: from Yields (2H 4He)/(3H 3He)

S. Das Gupta and A.Z. Mekjian Phys. Rep. 72 (1981) 131

S. Albergo et al. Nuovo Cimento 89 (1985) 1

3- Momentum space density Power law:

2- Neutrons: from Yields (3H/3He)

Cluster momentum spectrum versus (proton momentum spectrum)A

(neutron spect. = proton spect., Coulomb correction)

Page 12: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Statistical/equilibrium framework

For each Vsurf bin (i.e. time)1- Temperature: from Yields (2H 4He)/(3H 3He)

S. Das Gupta and A.Z. Mekjian Phys. Rep. 72 (1981) 131

S. Albergo et al. Nuovo Cimento 89 (1985) 1

3- Momentum space density Power law:

2- Neutrons: from Yields (3H/3He)

VOLUME measurement DENSITY

Page 13: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Density: low values are achieved

Page 14: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Temperature and proton fraction

T = few MeV Yp = entrance chan.

(T, r, Yp) useful for CCSNe

Page 15: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Mass fractions: N/Z dependence

FERMIONS

BOSONS

FERMIONS

Page 16: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Equilibrium constant Kc

Z 11𝐻 + (𝐴 − 𝑍) 0

1𝑛 ↔ 𝑍𝐴𝑋

Law of mass action (Guldberg et Waage)Equilibrium, same phase.

aA+bB↔gC+dDConstant Kc is relative to concentrations and stoichiometric coef.

Kc = ([C]g.[D]d)/([A]a.[B]b)

The equilibrium reaction is characterized by Kc whose value is constant for a given reaction and a given temperature.

Gas of protons & neutrons in equilibrium with clusters

Basic chemistry course!!!

The equilibrium constant is a universal characteristics

Page 17: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Equilibrium constant Kc

no N/Z dependence

Page 18: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Equilibrium constant Kc: Texas A&MData from NIMROD detector

TEXAS A&M

(mid-rapidity region, central collisions)

AT VERY LOW DENSITIES

Z 11𝐻 + (𝐴 − 𝑍) 0

1𝑛 ↔ 𝑍𝐴𝑋

Page 19: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

INDRA versus Texas A&M: Kc (4He)

INDRA

Equilibrium constant values are different

Page 20: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

INDRA versus Texas A&M: Temp.

INDRA

The thermodynamical paths are different

Page 21: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Relativistic Mean-Field with clusters

RMF approach: clusters as new degrees of freedom, with effective mass dependent on density.• In-medium effects: clusters interact with medium via the mesoncouplings, or effective mass shifts, or both

Helena Pais (CFisUC, University of Coimbra, visitor LPC), F. Gulminelli (LPC-Caen),

C. Providência (Univ. Coimbra), G. Roepke (Univ. Rostock).

Change the cluster effective mass

Broadly speaking:Free nucleons & nucleons within nuclei: same mean-field (Xs=1)Free nucleons & nucleons within nuclei: different mean-field (Xs<1)

H. Pais et al. PRC97, 045805 (2018) – H. Pais et al. PRC99, 055806 (2019)

Page 22: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Relativistic Meam-Field versus DATA

INDRA & RMF Texas A&M & RMF

1) Clear deviations from Ideal gas: in medium effectsare present

2) Some deviations data/RMF calculations at very lowdensitiesindra Xs=0.9 while Texas A&M Xs=0.85

Page 23: INDRA GANIL experiments: Equilibrium constantsINDRA versus Texas A&M: K c (4He) INDRA Equilibrium constant values are different. INDRA versus Texas A&M: Temp. INDRA The thermodynamical

Conclusions• Nuclear matter characterization at very low densities is

possible using Heavy-ion reactions

• NM is far away from Ideal Gas hypothesis

• In-medium effects are present: nucleons within clusters

have to be treated differently as compare to free

nucleons.

• Implication: mean-field effets, binding energy shift,…

• CCSNe: EOS and neutrino opacity (clusters)

• The work is in progress to explain the difference between

the two experiments, improved method to extract

temperature and density: INDRA + H. Pais (CFisUC,

Univ. of Coimbra, visitor LPC), F. Gulminelli (LPC-Caen),

C. Providência (Univ. Coimbra), S. Mallik (Variable

Energy Cyclotron Centre, Kolkata, visitor LPC) and

discussion with Texas A&M.