fazia/indra scientific program ganil …scientific program ganil experiments: equilibrium constants...

FAZIA/INDRA Scientific ProgramGANIL experiments:

Equilibrium constants

R. Bougault, LPC Caen for the FAZIA collaboration

FAZIAFrance, Italy, Poland, Romania

new

FAZIA Demonstrator192 telescopes

Si(300m)/Si(500m)/CsI(10cm)

Blocks of 16 (20x20mm2) telescopes

with in vacuum FEE

(digitized signals for Pulse Shape

identification)

Extend (A,Z) identification

FAZIA

SHORT TERM 2019-…

FAZIA coupled with INDRA

GANIL: 58,64Ni@35-65 A.MeV

INDRA

Existing GANIL

INDRA multi-detector• (A,Z,E) for light charged

particles

• (Z,E) for heavier fragments

The basic FAZIA module(looking very standard, but actually somewhat special)

1st

Si2d

Si

CsI(Tl) + photodiode

Si(300m)/Si(500m)/CsI(10cm)

20x20mm2


1st element: reverse mount 300 μm thick, nTD Silicon of doping uniformity

(2% RMS) adapted to Pulse Shape Analysis of signals

1st

Si2d

Si


Identification by PSA

on 1st Si




2nd element: reverse mount 500 μm thick, nTD Silicon for redundant PSA

1st

Si2d

Si

CsI(Tl) + photodiodeIdentification by

ΔE1- E2





3rd element: 10 cm long CsI(Tl) crystal, coupled to Si-photodiode

1st

Si2d

Si


Identification by

(ΔE1+ ΔE2) - E3





3rd element: 10 cm long CsI(Tl) crystal, coupled to Si-photodiode

First and second Silicon detectors are cut out of a <100> crystal along a

properly selected direction in order to avoid channelling.

1st

Si2d

Si


Identification by

(ΔE1+ ΔE2) - E3

Identification by

ΔE1- E2

Identification by PSA

on 1st Si

CsI

FAZIA PSA performance: Z

(First Silicon detector ONLY)

No limits seen

for Z

identification.

Progress with

respect to

previous results

is evident.

Z=54

129Xe + 58Ni @ 35 MeV/n

EN

ER

GY

(ch

an

nel)

First Si Charge signal Rise Time (ns)

DE E

CsI

FAZIA operation has definitely confirmed the superior performance of this correlation

PSA-based mass discrimination up to Z ≈ 20 is available using this correlation, with

refined digital processing with the now used faster ADCs.

Z=63

FAZIA PSA performance: Z and A

(First Silicon detector ONLY)

DE E

CsIDE E

No channelling with a

properly cut Silicon…

Note full Z identification

Isotopic (mass)

identification up to Z~25

with ~5GeV full range

FAZIA PSA performance: DE/E

Z=5Z=54

129Xe + 58Ni @ 35 MeV/n

FAZIA PSA performance: DE/E

FAZIA Demonstrator

It exists!

FAZIA

EXPERIMENTS

INDRA/FAZIA

in GANIL 2019…

FAZIA Scientific Program

• Nuclear matter Equation of State• Density, Temperature, (N-Z)/A

• Cluster in nuclear medium

• Nuclear matter Transport properties• In medium nucleon-nucleon interaction

• Hot nucleus Thermodynamics• Level density at finite temperature

• Phase transition, spinodal

IMPORTANCE OF (A,Z) Identification of reaction products

GANIL, LNS, LNL

Nuclear Matter Equation of StateSymmetry energy versus density

J. Margueron, R. Hoffmann Casali, F. Gulminelli Phys. Rev. C 97, 025805 (2018)

Nuclear EOS (meta-modeling): high order Taylor expansion

Varying all

empirical

parameters

together (+/- s)

𝜌𝑠𝑎𝑡

SY

MM

ET

RY

EN

ER

GY

DENSITY

2018 status

Constraints:

• Experimental data/Model

prediction

• Functionals:

• 35 Skyrme

• 11 RMF

• 4 RHF

• 2 ab_initio

Nuclear Matter Equation of StateSymmetry energy versus density

J. Margueron, R. Hoffmann Casali, F. Gulminelli Phys. Rev. C 97, 025805 (2018)

Nuclear EOS (meta-modeling): high order Taylor expansion

Varying all

empirical

parameters

together (+/- s)

𝜌𝑠𝑎𝑡

SY

MM

ET

RY

EN

ER

GY

DENSITY

DENSITY

SY

MM

ET

RY

EN

ER

GY

Varying only Ksym

Nuclear Matter Equation of Stateat very low densities

K. Hagel, J.B. Natowitz, G. Röpke Eur. Phys. Journal A 50 (2014) 39

Prediction of the nuclear EOS : The symmetry energy at subsaturation

density and finite temperature

Data versus

• Quasiparticle Mean-Field Approach (RMF without cluster)

• Quantum Statistical (QS) approach (with clusters)

In the low-density region: the symmetry energy is

strongly depending on temperature

Mean field (no cluster): linear

increase of the symmetry energy.

QS: formation of clusters leads to an

increase of the symmetry energy at

low densities.

IMPORTANCE OF CLUSTERS

+ and o: data Texas A&M

Heavy-Ion collisionsHeavy-ion collisions at Fermi energies:

unique tool to study low density exotic nuclear matter

(region located at mid-rapidity)

Study of the chemistry/particle composition

Low density window

124Xe

B. Tsang

Thank you for the picture

Equilibrium constant KcData from NIMROD detector

TEXAS A&M

(mid-rapidity region, central collisions)

AT VERY LOW DENSITIES

Z 11𝐻 + (𝐴 − 𝑍) 0

1𝑛 ↔ 𝑍𝐴𝑋

Chemistry of proto-neutron star

(neutrino-sphere)

Measure in medium effects (Helena Pais)

Cold Neutron Star

2.Neutronization &

by

emission

3. Long-term cooling:

Neutrino cooling epoch

Photon cooling epoch

few minutes

105 years

csm.ornl.gov

1. Accretion of matter onto the central object,

known as the proto-neutron star (hot and lepton rich)

Cooling

neutrino

proto-Neutron Star

• Dominated by neutrinos.

• Large part of the process occurs

near the surface (neutrinosphere)

which is composed of warm low

density neutron rich material.

Clusters/Symmetry energy

influence the neutrino response of

the neutrinosphere material.

Core Collapse Supernova explosion

INDRA@GANIL experimentEquilibrium Constants 2d measurement

INDRA = 4pi multidetector

(A,Z,E) for light charged particles

(Z,E) for heavier fragments

136,124Xe+124,112Sn 32 A MeV

Analysis restricted to the forward part of the c.m.

INDRA@GANIL experiment

Selection: central events & ½ rapidity

CENTRAL EVENTS

½ rapidity production

½ rapidity=60°-90° angles

Quasi-projectile and mid-rapidity sources (in the c.m.)

Ecm (MeV)

𝐝𝐌

𝐝𝐄𝐜𝐦𝐝𝛀𝐜𝐦

124Xe+124Sn 32 A MeV

c.m. angle=60°-90°(mid-rapidity)

Central collisions

INDRA@GANIL experimentBasic observables: energy spectra of detected particles

Scenario: Hot expanding source

Detected particle energy spectra = Temperature + Coulomb

Particle energy spectra

at emission time:

Coulomb correction.

Surface energy

Surface velocity (Vsurf)

time2>time1

time1

For each step/bin of Vsurf

(i.e time) coalescence n,p

to form a cluster.

Ec = 10 MeV per Z

(Szi ½ rapidity)

Texas A&M analysisFor each step/bin of Vsurf (i.e time) coalescence n,p

to form a cluster.

with

Albergo et al. Il Nuovo Cimento 89 (1985) pp1-28

(equilibrium)

RVsurf = Y(2H) Y(4He)/Y(3H)Y(3He)

Coalescence radius

in

momentum space

Coalescence volume

(density)

T.C. Awes et al. PRC24 (1981) 89

A. Mekjian PL89B (1980) 177

Texas A&M analysis: comments!For each step/bin of Vsurf (i.e time) coalescence n,p

to form a cluster.

with

Albergo et al. Il Nuovo Cimento 89 (1985) pp1-28

(equilibrium)


Coalescence radius

in

momentum space

Coalescence volume

(density)

Rnp is n/p of the

evolving source

½ rapidity neutron

spectra are not measured

(Texas A&M and INDRA):

deduced from 3H and 3He

production

Mn=Mp (M3H/M3He)

INDRA data: equilibrium

achieved

Coulomb Ec not measured


Evolving source N/Z ratio deduced from 3H/3He ratio

Black: 124Xe+124Sn

Blue: 124Xe+112Sn

Difference for the two systems reflects different initial N/Z

𝜌(3𝐻)

𝜌 3𝐻𝑒=

𝜌 𝑛𝑒𝑢𝑡𝑟𝑜𝑛 2 𝜌(𝑝𝑟𝑜𝑡𝑜𝑛)

𝜌 𝑛𝑒𝑢𝑡𝑟𝑜𝑛 𝜌 𝑝𝑟𝑜𝑡𝑜𝑛 2 =𝜌 𝑛𝑒𝑢𝑡𝑟𝑜𝑛

𝜌 𝑝𝑟𝑜𝑡𝑜𝑛


Time sequence: proton rich material emission then neutron rich.

Black: 124Xe+124Sn

Blue: 124Xe+112Sn

𝜌(3𝐻)

𝜌 3𝐻𝑒=

𝜌 𝑛𝑒𝑢𝑡𝑟𝑜𝑛 2 𝜌(𝑝𝑟𝑜𝑡𝑜𝑛)

𝜌 𝑛𝑒𝑢𝑡𝑟𝑜𝑛 𝜌 𝑝𝑟𝑜𝑡𝑜𝑛 2 =𝜌 𝑛𝑒𝑢𝑡𝑟𝑜𝑛


TIME

Suggestion: looks like EES model of Friedman

Black: 124Xe+124Sn

Blue: 124Xe+112Sn


Coalescence radius in momentum spaceEvolving source N/Z ratio included

NO DIFFERENCE between N/Z reaction (thus n/z evolving source)

n/p from 3H/3He systematic error (possible to correct with models)

Comment concerning neutrons

Model correction or compare observables using 3H/3He and not n/p

n/p ratio compared to 3H/3He ratio

for a given proton fraction (0.41)

RMF MODEL (FSU) – different coupling constants

𝜌(3𝐻)

𝜌 3𝐻𝑒∝

𝜌 𝑛𝑒𝑢𝑡𝑟𝑜𝑛


(Helena Pais, private communication)


Same temperature for all studied systems

(lcp production are very different!)

RVsurf = Y(2H) Y(4He)/Y(3H)Y(3He)TEMPERATURE


VOLUME

(Density = nucleons/Volume)

Black: 124Xe+124Sn

Idem TexasA&M: deuton are different (« fragile »)


Black: 124Xe+124Sn

Blue: 124Xe+112Sn

VOLUME

(Density = nucleons/Volume)

Same results for the different systems


Black: 124Xe+124Sn

EQUILIBRIUM CONSTANTS versus DENSITY


Black: 124Xe+124Sn

Blue: 124Xe+112Sn

EQUILIBRIUM CONSTANTS versus DENSITY

Idem for all systems

INDRA@GANIL experimentEQUILIBRIUM CONSTANTS versus DENSITY

COMMENT:

Neutron density is not measured and is

deduced from proton density multiplied by 3H/3He (Texas A&M and INDRA).

For model comparison: would be better to use

the experimental prescription.

INDRA@GANIL experimentEQUILIBRIUM CONSTANTS: INDRA versus TEXAS A&M

deuton


triton


3He


4He

EQUILIBRIUM CONSTANTS: INDRA versus TEXAS A&M

INDRA experiment: conclusion

Analysis: framework of Texax A&M

• We confirmed the very low densities

measurements of Texas A&M.

• Equilibrium constants d, t, 3He, 4He

and 6He (new!).

• Equilibrium constants differences: steeper

with INDRA data.

• Comments about Coulomb and n/p versus 3H/3He.

FAZIA/INDRA exp.

Extend Kc measurements to heavier isotopes

Thresholds

FAZIA A & Z identification

80Kr+40-48Ca @ 35 A MeV IsoFazia experiment, June 2015, LNS Catania

D. Gruyer et al.

Supernova explosionSupernova explosion occurs via core-collapse in very massive stars (M>8Msun)

Present best 3D hydro simulations do not produce successful explosions

– Model and progenitor dependence - Great sensitivity to the microphysics

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

TE

MP

ER

AT

UR

E (

MeV

)

Baryon DENSITY (fm-3)

15 MSUN progenitor

EOS controls explosion

HI collisions (T, density)

SUPERNOVA 1054

Datation 1054.

REMNANT = CRAB NEBULA

Reign title: CHIH-HO, AD 1054-1055

Reign title: CHIA-YU, AD 1056-1063

Emperor JEN TSUNG (AD 1023-1063)Jen Tsung used nine reign titles, casting coins for all of them

“In the first year of the period Chih-ho (1054), the 5th

moon, the day chi-ch’ou (July 4th) (a “guest-star”)

appeared appromately several inches south-east of

T’ien-kuan (Tauri). After more than a year it gradually

become invisible”.

On the day hsin-wei (of the 3rd moon of the 1st year of

the period Chia-yu (April 17, 1056) the Chief of the

astromomical Bureau reported that from the 3th moon of the 1st year of the period

Chih-ho (June 9-July 7,1054) a guest-star had appeared In the morning in the eastern

heavens……….

Written around 1350

THANK YOU

INDRA@GANIL experimentImpact parameter selector:

transverse energy of lcp

Analysis restricted to the forward part of the c.m.

INDRA@GANIL experimentQuasi-projectile (0°-30°) mid-rapidity (60°-90°)

For central events: EQUILIBRIUM (124+124=136+112) for ½ rapidity and QP

Impact parameter selector:

transverse energy of lcp


Quasi-projectile and mid-rapidity sources (in the c.m.)

INDRA experiment

Black: 124Xe+124Sn

Blue: 124Xe+112Sn

𝐝𝐌

𝐝𝐕𝐬𝐮𝐫𝐟𝐝𝛀𝐜𝐦

Vsurf (MeV)

124Xe+124Sn 32 A MeV

c.m. angle=60°-90°(mid-rapidity)

Central collisions


L. Qin et al. PRL108 (2012)

INDRA

(preliminary)



Nuclear Matter Equation of StatePrediction of the nuclear EOS :

• Directly from Ab-initio approaches

• Directly from more simple interactions (Skyrme,…)

• From experimental measurements

It is possible to do:

• Taylor expansion around saturation density (empirical property)

Binding energy => 휀(𝜌𝑛 + 𝜌𝑝, 𝜌𝑛 − 𝜌𝑝) = 휀𝑖𝑠 𝜌𝑛 + 𝜌𝑝 + 휀𝑖𝑣 𝜌𝑛 + 𝜌𝑝 (𝜌𝑛−𝜌𝑝

𝜌𝑛+𝜌𝑝)2+⋯

Isoscalar 𝜌𝑛 + 𝜌𝑝 𝑒𝑛𝑒𝑟𝑔𝑦 ⇒ 휀𝑖𝑠 = 𝐸𝑠𝑎𝑡 +1

2𝐾𝑠𝑎𝑡𝛿

2 +1

3!𝑄𝑠𝑎𝑡𝛿

3 +1

4!𝑍𝑠𝑎𝑡𝛿

4

Isovector 𝜌𝑛 − 𝜌𝑝 𝑒𝑛𝑒𝑟𝑔𝑦 ⇒ 휀𝑖𝑣 = 𝐸𝑠𝑦𝑚 + 𝐿𝑠𝑦𝑚𝛿 +1

2𝐾𝑠𝑦𝑚𝛿

2 +1

3!𝑄𝑠𝑦𝑚𝛿

3 +1

4!𝑍𝑠𝑦𝑚𝛿

4

𝛿 =(𝜌𝑛+𝜌𝑝) − 𝜌𝑠𝑎𝑡

3𝜌𝑠𝑎𝑡

휀𝑖𝑣 𝑖𝑠 𝑜𝑓𝑡𝑒𝑛 𝑐𝑎𝑙𝑙𝑒𝑑 𝑡ℎ𝑒 𝑠𝑦𝑚𝑚𝑒𝑡𝑟𝑦 𝑒𝑛𝑒𝑟𝑔𝑦: 𝑆(𝜌𝑛 + 𝜌𝑝)

e does not change under (n,p) interchange, odd terms=0 (charge invariance of strong interaction).

Nuclear Matter Equation of StateIsoscalar 𝜌𝑛 + 𝜌𝑝 𝑒𝑛𝑒𝑟𝑔𝑦 ⇒ 휀𝑖𝑠 = 𝐸𝑠𝑎𝑡 +

1

2𝐾𝑠𝑎𝑡𝛿

2 +1

3!𝑄𝑠𝑎𝑡𝛿

3 +1

4!𝑍𝑠𝑎𝑡𝛿

4

Isovector 𝜌𝑛 − 𝜌𝑝 𝑒𝑛𝑒𝑟𝑔𝑦 ⇒ 휀𝑖𝑣 = 𝐸𝑠𝑦𝑚 + 𝐿𝑠𝑦𝑚𝛿 +1

2𝐾𝑠𝑦𝑚𝛿

2 +1

3!𝑄𝑠𝑦𝑚𝛿

3 +1

4!𝑍𝑠𝑦𝑚𝛿

4

𝛿 =(𝜌𝑛+𝜌𝑝) − 𝜌𝑠𝑎𝑡

3𝜌𝑠𝑎𝑡Empirical parameters at saturation density:

• Esat: saturation energy,

Ksat: incompressibility modulus,

Qsat: isoscalar sknewness,

Zsat: isoscalar kurtosis.

• Esym: symmetry energy,

Lsym: slope,

Ksym: isovector incompressibility,

Qsym: isovector sknewness,

Zsym: isovector kurtosis.

If you know all empirical parameters, EOS is known


• « Experimental » Not directly accesible from experiments without the use of a theoretical model

Bao-An Li, Xiao Han Phys. Lett. B 727 (2013) 276

Sym

metr

yE

nerg

yat r

sa

tS

lope

at r

sa

t


• Ab-initio approaches and more simple interactions (Skyrme,…)

𝜌𝑠𝑎𝑡

J. Margeron, R. Hoffmann Casali, F. Gulminelli nucl-th 1708.06894

Nuclear Matter Equation of State

𝜌𝑠𝑎𝑡

J. Margeron, R. Hoffmann Casali, F. Gulminelli nucl-th 1708.06894

Prediction of the nuclear EOS : all predictions together (meta-modeling)

DENSITY

SY

MM

ET

RY

EN

ER

GY

DENSITY

SY

MM

ET

RY

EN

ER

GY

Only Lsym variation Only Ksym variation


Coalescence radius in momentum spaceEvolving source N/Z ratio removed

Black: 124Xe+124Sn

Black: 124Xe+124Sn

Blue: 124Xe+112Sn


Coalescence radius in momentum spaceEvolving source N/Z ratio removed

DIFFERENCE between N/Z reaction (thus n/z evolving source)


Coalescence radius in momentum spaceEvolving source N/Z ratio included

Black: 124Xe+124Sn

INDRA@GANIL experimentINDRA = 4pi multidetector

(A,Z,E) for light charged particles

(Z,E) for heavier fragments

Cold Neutron Star

2.Neutronization &

by

emission

3. Long-term cooling:

Neutrino cooling epoch

Photon cooling epoch

few minutes

105 years

csm.ornl.gov

1. Accretion of matter onto the central object,

known as the proto-neutron star (hot and lepton rich)

Cooling

neutrino

Core Collapse Supernova explosion

FAZIA Scientific Program

• Nuclear matter Equation of State• Density, Temperature, (N-Z)/A

• Cluster in nuclear medium

• Nuclear matter Transport properties• In medium nucleon-nucleon interaction

• Hot nucleus Thermodynamics• Level density at finite temperature

• Phase transition, spinodal

IMPORTANCE OF (A,Z) Identification of reaction products

GANIL, LNS, LNL

fazia/indra scientific program ganil …scientific program ganil experiments: equilibrium constants...

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