Neutron stars in the laboratory · Reactions induced by heavy ions Relativistic beams to produce...

Neutron stars in the laboratory

José Benlliure on behalf of GENP

H. Alvarez, J.M. Boillos, P. Cabanelas, D. Cortina,

J. Díaz, M. Feijoo, E. Galiana, D. González

Universidade de Santiago de Compostela

December 21st, 2017

The strongly interacting world

Hadrons Atomic nuclei Big-Bang

nucleosynthesis Stellar evolution and

nucleosynthesis

Open questions:

- Hadron structure and non-perturbative QCD

- The equation of state of nuclear matter

- Nuclear force from first principles and the limits of the chart of nuclides

- The origin of the elements in the Universe

IGFAE retreat, December 2017 José Benlliure

The largest nuclei in the Universe

Neutron-rich nuclei

Equation of state

Subnucleonic

degrees of freedom

José Benlliure IGFAE retreat, December 2017

Neutron stars NN correlations

Neutron stars merger Nucleosynthesis

Binary neutron star merger

Igfae retreat, December 2017

Multi-messenger observation

kHz GW will constraint EoS

José Benlliure

Electromagnetic

signals provide

first evidence for

r-process

nucleosynthesis.

Neutron stars in the lab


Producing neutron star and binary neutron star merger matter

Reactions induced by heavy ions

Relativistic beams to produce dense nuclear matter (~2 o) and excite

subnucleonic degrees of freedom (nucleon resonances and hyperons)

Radioactive Beams to produce neutron-rich nuclei

@

R

R

R B

R3B@FAIR



~ 100 m

More than 4000 nuclear

species at reach.

In particular the most

neutron rich.

R3B@FAIR

R3B@FAIR


Complete kinematics, fixed target experiments with relativistic radioactive beams

isotopic identification of projectile remnants: forward detectors

complete identification of -rays, nucleons and clusters: target area detectors

neutrons

heavy fragments

protons

light fragments

-rays

protons

~ 250 scientists

R3B@FAIR

IGFAE retreat, December 2017 José Benlliure

Large-acceptance superconducting magnet

Large-area neutron detector

Tracking detectors

Target area Silicon tracker

CALIFA

See next talk by Pablo

Neutron-rich nuclei

Equation of state

Subnucleonic

degrees of freedom


Neutron star matter

NN correlations

Neutron stars merger

The origin of the heaviest

elements in the Universe

R3B@FAIR: GENP research program



Neutron star matter: structure of nuclei far from stability

Quasi-free scattering reactions (p,2p) and (p,pn) give access to:

Single-particle structure of nuclei far from stability.

Unbound nuclear states.

Limits of existence of nuclei in terms of isospin.

12C(p,2p)11B



Neutron star matter: structure of nuclei far from stability

Submmitted to PRC

Submmitted to PRL



Neutron star matter: NN correlations in nuclear matter

Long-range mean field

Short range subnucleonic degrees

of freedom

Tensor n-p pairs

R3B gives access to isospin asymmetry SRC using (p,2p) and (p,pn)

quasi-free scattering:

Complete kinematic measurements: recoil and knockout nucleons identification

Selection of nucleon pairs with high relative momentum

Future project by H. Alvarez and D. Cortina

José Benlliure


Neutron star matter: EoS for asymmetric-dense matter

Δ, N*, Λ, Ξ, …

Relativistic radioactive beams

make it possible to produce

asymmetric and dense ( ~2 o)

nuclear matter.

EoS is strongly influenced

by the neutron excess and

the excitation of subnucleonic

degrees of freedom.

GENP activities: next talk by Javier Díaz on the symmetry energy IGFAE retreat, December 2017

José Benlliure


Neutron star matter: subnucleonic degrees of freedom

EoS with realistic description

of the asymmetry term suggest

that nucleon resonances may

appear at lower densities than

hyperons.

GENP leads a program to investigate nucleon

resonances in asymmetric nuclear matter by using

isobar charge exchange reactions induced by

relativistic beams.

(1230)

(1440)

?

63Cu(112Sn,112Sb)X

IGFAE retreat, December 2017

n p

o

p p

-

op,n +,-

N

N

N

Proposal for the next GSI/FAIR PAC by J.L. Rodríguez and J. Benlliure

José Benlliure


Neutron star matter: future plans


Glad 3He

-

3ΛH

p K+

A large volume TPC inside the R3B magnet will

offer new opportunities to investigate:

- EoS for dense asymmetric nuclear matter

- Hypernuclei

- NN short-range correlations

Neutron-rich nuclei

Equation of state

Subnucleonic

degrees of freedom


Neutron star matter

NN correlations

Neutron stars merger

The origin of the heaviest

elements in the Universe




The origin of the heaviest elements: r-process stellar nucleosynthesis

Z

Closed shell

stability

line

Waiting

point

N Supernovae type II Neutron stars mergers

Most of the nuclei participating

in this process are not known



The origin of the heaviest elements: production and study of r-process nuclei

73 new neutron-rich nuclei close to the

r-process path discovered by GENP

r-process

faster than

expected



The origin of the heaviest elements: fission and the r-process Relativistic beams made it possible the first complete

identification of fission fragments.

José Benlliure

x ~ 200 m

ToF ~ 40 ps

E/E ~ 1%

Z ~ 0,4 FWHM

A ~ 0,7 FWHM



The origin of the heaviest elements: fission and the r-process

José Benlliure

Relativistic beams made it possible the first complete

identification of fission fragments.



The origin of the heaviest elements: future plans Most complete fission experiments

José Benlliure

coupling R3B + SOFIA

(p,2p)-induced fission

Soon @ R3B/FAIR Characterization of the fissioning nucleus (A, Z, E*)

(p,2p) with CALIFA+tracker

Characterization of the fission fragments (A, Z, TKE, )

SOFIA + NeuLAND

J. Benlliure and J.L. Rodríguez, proposal approved by the GSI/FAIR PAC

Conclusions and perspectives

José Benlliure

R3B@FAIR offers unique opportunities to investigate neutron star matter and binary neutron star

mergers nucleosynthesis.

GENP/IGFAE has a large impact in the experiment: spokesperson (D. Cortina), simulation and data

analysis WG convener (H. Alvarez), leading physics runs (J. Benlliure)

Physics interests: structure of nuclei far from stability, fission, Eos of asymmetric nuclear matter….

Hardware contribution: CALIFA (25%), future TPC under consideration


2015 2016 2017 2018 2019 2020 2021 2022 2023 2024

CALIFA

R3B TPC

(p,2p) fission experiment

in-medium experiment

Short-range correlations experiment

Green fields non or poorly covered by NP@IGFAE:

Hypernuclei, Eos of asymmetric dense nuclear matter or fundamental interactions in nuclei.

R3B, Panda, CBM @ FAIR, ALICE@CERN, ion traps

Neutron stars in the laboratory · Reactions induced by heavy ions Relativistic beams to produce...

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Transcript of Neutron stars in the laboratory · Reactions induced by heavy ions Relativistic beams to produce...