Paweł Moskal

HADRONS IN NUCLEAR MEDIUM IIKEK Tokai Campus (JPARC), Japan, 24-25 October 2014

Jagiellonian University, Cracow, Poland

Interaction of pseudoscalar mesonswith nucleons and nuclei

Abstract:We will review experiments and phenomenology

of the η, η and K mesons interaction with nucleons and nucleip.m., Few Body Syst. 55 (2014) 667

historical entanglement

Jagiellonian University

1364

Collegium Maius at the university since 1400

historical entanglement

Jagiellonian University

1364

Collegium Maius at the university since 1400

ηꞌ K+ K-η

Production of mesons at threshold

• experimental aspects

• natural width of the η meson • η -proton interaction

• production dynamics

• η-proton-proton interaction• Borromean-states?

• η-nucleus interaction• mesic-nuclei ?

• challenges to theory

in the laboratory

before reaction:

L = 1, S = 1

1 GeV/c

1 GeV/c

P

P

h

after reaction:

L = 0, l=0

3 GeV/c

P

P

h

in the centre of mass system

Reaction parameter b 0.2 fm3P01S0s

threshold as a spin filter

experimental challenge !

• polarised and unpolarised proton and deuteron beams

• stochastic and electron cooling

• momentum range: 600 – 3700 MeV/c

• meson production up to (1020)

COoler SYnchrotron COSY

The natural width of the η meson

η

• experimental aspects

• natural width of the η meson • η -proton interaction

• production dynamics

• η-proton-proton interaction• Borromean-states?

• η-nucleus interaction• mesic-nuclei ?

• K+K- interaction

COSY-11Clustertarget

driftchambers

scintillator

scintillator

COSY-11cluster target

drift chambers

scintillators

scintillator

COSY-11

E. Czerwinski, p.m. et al., Phys. Rev. Lett. 105 (2010) 122001

COSY-11: Phys. Rev. Lett. 105 (2010) 122001

The η - proton hadronic interaction

E. Czerwinski, p.m. et al., Phys. Rev. Lett. 113 (2014) 062004

η p

σ = dVps |M|2F

1

|M|2 ~ |M0|2 |MFSI|2

in the laboratory

before reaction:

L = 1, S = 1

1 GeV/c

1 GeV/c

P

P

h

after reaction:

L = 0, l=0

3 GeV/c

P

P

h

in the centre of mass system

Reaction parameter b 0.2 fm3P01S0s

threshold as a spin filter

The η - proton hadronic interaction

E. Czerwinski, p.m. et al., Phys. Rev. Lett. 113 (2014) 062004

η p

σ = dVps |M|2F

1

|M|2 ~ |M0|2 |MFSI|2

Production mechanism

η

• experimental aspects

• natural width of the η meson • η -proton interaction

• production dynamics

• η-proton-proton interaction• Borromean-states?

• η-nucleus interaction• mesic-nuclei ?

• K+K- interaction

dynamics → |M0|2

ONE NUMBER and MANY GRAPHS

What would the first experimental physicists tell us?

What would the best student of the Jagellonian University tell us?

He is encouraging us to continue:

For what is determinate cannot have innumerable explanations

NICOLAUS COPERNICUS ”Minor Works III, Letter against Wagner”

Salviati. But if, of many computations, not even two came out in agreement, what would you think of that? Simplicio. If that is how the matters stand, it is truly a serious defect GALILEO GALILEI ”Dialogue concerning the two chief world systems”

production dynamics e.g. meson η

σ = dVps |M|2F

1

|M|2 ~ |M0|2 |MFSI|2

dynamics → |M0|2

LARGE → RESONANSE

CELSIUS

COSY

SATURNE

STRONG ISOSPIN DEPENDENCE

Eta meson is by factor of 12 more coupiously produced when the total isospin of nucleons

is equal to 0 than when it is equal to 1 Strong evidence of isovector meson

exchange in production mechanism

CELSIUSCOSYSATURNE

X X X

X X XX

This was PREDICTED already about 2500 years ago by the very first physicists

Thus, it is suggested that among created beingsthere must be some basic agent which will move things and bring them together

ARISTOTLE “Metaphysics”

rp

R. Czyżykiewicz, p.m. et al., Phys. Rev. Lett. 98 (2007) 122003

WASA-at-COSY p p p p M 109 and 1011 π0 on discs

p p p p 106 mesons on discs ; Polarization of about 70% (factor of 500 larger statistics )

→

WASA

WASA A WARSHIP built for the war with Poland which sank in 1628 in the middle of Stockholm harbour after sailing barely 1300 meters

• polarised and unpolarised proton and deuteron beams

• stochastic and electron cooling

• momentum range: 600 – 3700 MeV/c

• meson production up to (1020)

WASA-at-COSY pp pp pd 3He

Borromean state ?

η

• experimental aspects

• natural width of the η meson • η -proton interaction

• production dynamics

• η-proton-proton interaction• Borromean-states?

• η-nucleus interaction• mesic-nuclei ?

• K+K- interaction •

σ = dVps |M|2F

1

|M|2 ~ |M0|2 |MFSI|2

|MFSI|2 ~ |Mpp|2 |Mp1η|2 |Mp2η|2

dynamics → |M0|2

interaction → σ (Q)

CELSIUS, COSY, SATURNE

+

+ η

S. Wycech, Acta Phys. Polon. B 27 (1996) 2981

Borromean rings from nucleons6He

++

Borromean nuclei: 6He, 11Li, 14Be

+

+ η

A. Deloff, AIP Conf. Proc. 950 (2207) 150

Correlation femtoscopy

P. Klaja, p.m. et al., J. Phys. G 37 (2010) 055003

„At present it is not possible to draw a solid quantitative conclusion about the size of the system since e.g. in the case of the pp → pp reaction it would require to solvea three-body problem where pp and p-eta interactions are not negligible and both contribute significantly to the proton-proton correlation. However, based on semiquantitative predictions one can estimate that the system must be unexpectedly large with a radius in the order of 4 fm”

COSY TOF, COSY-11, WASA/CELSIUS

V. Baru et al., PRC 67 (2003) 024002

p.m. et al., Phys.Rev. C69 (2004) 025203

pp pp pp pp ꞌ

P. Klaja, p.m. et al., Phys.Lett. B684 (2010) 11-16

WASA-at-COSY p p p p M 109 and 1011 π0 on discs

p p p p 106 mesons on discs ; Polarization of about 70% (factor of 500 larger statistics )

→

Mesic nuclei ?

η

• experimental aspects

• natural width of the η meson • η -proton interaction

• production dynamics

• η-proton-proton interaction• Borromean-states?

• η-nucleus interaction• mesic-nuclei ?

• K+K- interaction

3He interaction (pd 3He X)

++

η

- 3He

• dp 3He γ 3He 3He

ANKE: T. Mersmann et al., Phys. Rev. Lett. 98 242301 (2007)

COSY-11: J. Smyrski et al., Phys. Lett B 649 258-262 (2007)

η

++

COSY MAMI

MAMI: M. Pfeiffer et al., Phys. Rev. Lett. 92 252001 (2004)

F. Pheron et al., Phys. Lett. B709 21 (2012)

Phys.Lett. B734 (2014) 333

- 3He

η

++

COSY-ANKE

C.Wilkin et al., Phys. Lett. B654 (2007) 92

–Attractive interaction between η and N – (R. Bhalerao and L. C. Liu, Phys. Lett. B54 (1985) 685 )

– – possible existence of bound states – of the η meson with nuclei for A>10 (Q. Haider and L. C. Liu, Phys. Lett. B172 (1986) 257 )

(C.Garcia-Recio, T. Inoue, J.Nieves,

E. Oset, Phys. Lett. B550 (2002) 47).

3He-η 3H-η 4He-η

η bound state possible with the light nucleiC. Wilkin, Phys. Rev. C47 (1993) 938

Supported by model calculations of: - S. Wycech et al., Phys. Rev. C52(1995)544

(the multiple scattering theory)

………

ηꞌ-nuclear and η-nuclear bound states revisited D. Jido, H. Naghiro, S. Hirenzaki, Phys. Rev. C66 (2002) 045202 H. Nagahiro, S. Hirenzaki, Phys. Rev. Let. 94 (2005) 232503 S. Hirenzaki et al., Acta Phys. Pol. B41 (2010) 2211 E. Friedman, A. Gal, J. Mares, Phys. Lett. B725 (2013) 334 S. Hirenzaki, H. Nagahiro, Acta Phys. Pol. B45 (2014) 619

+

+ ηN*

N* π‾+

THE ETA-MESIC NUCLEUSη meson bound with nucleus via

STRONG INTERACTION

+

+ η

γ

THE ETA-MESIC NUCLEUSη meson bound with nucleus via

STRONG INTERACTION

γ

WASA-at-COSY

→

SIMULATIONS

d+d → (4He-η)bound→ 3He + p +

π-

d+d → 3He + p + π-

EXPERIMENT

Upper limit of about 25 nbWASA-at-COSY: Phys. Rev. C87(2013) 035204

- 4He

- 3He

~25nb -- Present experimental upper limit .

WASA-at-COSY: Phys. Rev. C87(2013) 035204

~ 4 nb -- Theoretical estimation . S. Wycech, W. Krzemien , Acta. Phys. Pol. B45 (2014) 745

~ few nb -- WASA-at-COSY data collected in 2010 .

~270 nb -- Present experimental upper limit pppπ- p.m., J. Smyrski, Acta Phys. Pol B41 (2010) 21

~80 nb -- Theoretical estimation .

C. Wilkin, Acta. Phys. Pol. B45 (2014) 603

~ 10nb -- expected from New WASA-at-COSY data collected in May 2014

3He interaction (pd 3He X)

++

η

dp 3He o

3He threshold

COSY-11Fig. from C. Kerboul et al., PL B181(1986)28

COSY-11

(dp (3He -) bound 3He o ) < 70 nbp.m., J.Smyrski, Acta Phys. Pol B41 (2010) 21

K+K- interaction

η

• experimental aspects

• natural width of the η meson • η -proton interaction

• production dynamics

• η-proton-proton interaction• Borromean-states?

• η-nucleus interaction• mesic-nuclei ?

• K+K- interaction

Provided and are therethe scalars have an“Inverted Spectrum”

pseudoscalar mesons vector mesons

Scalar multi-plet:

(500), (700), f0(980), a0(980)• (600) is it a meson ?

• Do , a0(980) i f0(980) belong

to the same qq nonet?

• If yes, then why the spectra are reversed?

qqqq states (Jaffe, Achasov et al., Maiani et al.)

KK molecules (Weinstein-Isgur, Close et al.,

Kalashnikova et al.)

scalar mesons structure ?

Physical motivation

- typical mass of neutron stars in universe - less than 1.5 M⊙

- maximum mass of neutron stars in conventional nuclear EOS - above 2 M⊙

Neutron star mass as a function of central density

G.Q. Li, C.-H. Lee and G.E. Brown, Nucl.Phys. A625 (1997) 372

Kaon pair production in nucleons collisions

Proton-proton collisions close to K+K- threshold

/

or

00

KppKfppapp

KppKpp

dipole

beam

K-

ppK+drift chambers

S1

silicon pads + scintillator

pp → ppK+K-

Multiplicity of kaon and anti-kaon production per participating nucleon for C+C, Ni+Ni, and proton-proton collisions

pp → ppK+K-

pp → pK+Λ

p.m. et al., J. Phys. G28 (2002) 1777

COSY-11: C. Quentmeier et al., Phys. Lett. B 515 (2001) 276.ANKE: Y. Maeda et al.., Phys. Rev. C 77 (2008) 01524.

COSY-11: P. Winter et al., Phys. Lett. B 635 (2006) 23.

DISTO: F. Balestra et al., Phys. Rev. C 63 (2001) 024004.

σ = dVps |M|2F

1

|M|2 ~ |M0|2 |MFSI|2

pp → ppK+K-

Dalitz plot pp Goldhaber plot ppK+K-

M. Silarski, p.m., Phys. Rev. C 88 (2013) 025205

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