1 Nuclear and Particle Physics 3 lectures: Nuclear Physics Particle Physics 1 Particle Physics 2.
NUCLEAR MATTER NUCLEAR PHYSICS QCD HADRON PHYSICS NUCLEAR STRUCTURE HEAVY ION REACTIONS MANY-BODY...
Transcript of NUCLEAR MATTER NUCLEAR PHYSICS QCD HADRON PHYSICS NUCLEAR STRUCTURE HEAVY ION REACTIONS MANY-BODY...
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NUCLEAR MATTER NUCLEAR PHYSICS
QCDHADRON PHYSICS
NUCLEARSTRUCTURE
HEAVY IONREACTIONS
MANY-BODYSYSTEMS
ASTROPHYSICS
Specific and non-trivial relationsamong different fields
M. Baldo
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CataniaPisa
Milano
Ferrara
M. BaldoG.F. BurgioL.G. CaoM. Di ToroG. GiansiracusaV. GrecoU. LombardoC. MaieronO. NicotraH.J. SchultzeX.R. Zhou
I. BombaciA. FabrociniG. Lugones
A. DragoF. FronteraG. PagliaraI. Parenti
P. AvogadroP.F. Bortignon R.A. BrogliaG. Colo’P. DonatiG. GoriF. RamponiP.M. PizzocheroE. Vigezzi
A. Lavagno
Torino
CT51LS31MI31OG51PI31PI32
Iniziativespecifiche INFN
Roma
O. BenharV. FerrariL. GualtieriS. Marassi
Trieste
S, FantoniA. IlarionovK.E. Schmidt
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I. Bombaci NPA 754(2005)335c
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J.M. Lattimer , M. Prakash, Science 304(2004)
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The structure and the properties of a compact star (“NS”) are determined by the equation of state (EOS) of dense hadronic matter.
interactions
matter’s constituents
EOS
R
M
Mmax R M(R), …
“stiff” EOS
“soft”
“soft”
density
Pre
ssur
e “stiff” EOS
Mmax = (1.4 – 2.5) M Oppenheimer-Volkoff mass
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M. Baldo, G. Giansiracusa, U. Lombardo, H.Q. Song, PLB 473(2000)1A. Akmal, V.R. Pandharipande, D.G. Ravenhall, PRC58(1998)1804
BBG
Variational
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X.R.Zhou, G.F. Burgio, U. Lombardo, H.-J. Schultze, W. Zuo, PRC69(2004)18801
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-stable nuclear matter
Equilibrium with respect to the weak interaction processes e
epn
Charge neutrality nnn ep To be solved for any given value of the total baryon number density nB
e
e
epn
nep
np
e
MeVm
e
e 6.105if
0 neutrino-free matter
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Composition of asymmetric and beta-stable matterincluding hyperons
•Composition of stellar matter
i) Chemical equilibrium among the
different baryonic species
ii) Charge neutrality
iii) Baryon number conservation
np
ep
n
pn
e
epn
2
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I. Vidaña, Ph.D. thesis (2001)
Baryon chemical potentials in dense hyperonic matter
en
n
n + e- - + e
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BHF
GM3
GM3 EOS: Glendenning, Moszkowski, PRL 67(1991) Relativistic Mean Field Theory of hadrons interacting via meson exchange
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H.J. Schulze, A. Polls, A. Ramos, I. Vidana PRC 73, 058801 (2006)
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Quark Matter in Neutron Stars
QCD
Ultra-Relativistic Heavy Ion Collisions
Quark-deconfinement phase transition
The core of the most massive Neutron Stars is one of the best candidates in the Universe where such a deconfined phase of quark matter can be found
2SC
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“Neutron Stars”
“traditional” Neutron Stars
Hyperon Stars
Hadronic Stars
Hybrid Stars
Strange Stars
Quark Stars
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Including Quark matter
Since we have no theory which describes both confined and deconfined phases, one uses two separate EOS for baryon and quark matter assuming a first order phase transition.
a) Baryon EOS.
b) Quark matter EOS. MIT bag model Nambu-Jona Lasinio Color dielectric model
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The value of B is constrained in symmetric matter from reaction experiments, suggesting that transition to quark matter does not occur before 1 GeV/fm3
Symmetric matter β-stable matter
Density-dependentBag constant
G.F. Burgio, M Baldo, P.K.Saku, H.-J. SchultzePhys. Rev. C66(2002)25802
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Hybrid star composition
Mass-radiusrelation
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Color dielectric model Effective bag constant
C. Maieron, M. Baldo, G.F. Burgio,H.J. Schulze, PRD70(2004)43010
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Color and flavour-conserving transition from a hadronic to a superconducting quark star
No transition
Transition to a hybrid star
Transition to a strange star
G. Lugones, I. Bombaci, Phys. Rev. D72(2005)65021
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Densities of u,d,s quark are the same in the two phases
Pairing between u and d, u and d quarks (same chemical potential)
Paired phase favoured for largegaps, which compensate thelocking of chemical potential
Free quarks,electrons
Pairing Bagconstant
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A. Lavagno, G. Pagliara, EPJ A27(2006)289 M. Baldo, M. Buballa, G.F. Burgio, F.Neumann, M. Oertel, H.J. Schultze, PLB 562(2003)153
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Hadronic Hadronic MatterMatter
QM dropQM drop
RR Quantum fluctuations of a virtual drop of quark matter in hadron matter
R- R+
EE
U(R) = (4/3) R3 nQ* (Q* - H ) + 4 R2U(R)
R
I.M. Lifshitz and Y. Kagan, 1972; K. Iida and K. Sato, 1998
A closer look at the quark phase transition:A closer look at the quark phase transition:quantum nucleation theory quantum nucleation theory
Z. Berezhiani, I. Bombaci, A. Drago, F, Frontera, A. Lavagno, Apj 586(2003)1250
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Tuniv ~ 41017s
Tuniv
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The critical mass of metastable Hadronic Stars
Def.: Mcr = MHS(=1yr)
HS with MHS < Mcr are metastable with = 1 yr
The critical mass Mcr plays the role of an effective maximum mass for the hadronic branch of compact stars
HS with MHS > Mcr are very unlikely to be observed
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Hadronic Stars: nucleons + hyperons
I.Bombaci, I. Parenti, I. Vidaña, APJ 614(2004)314
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A.Drago, G. Pagliara, I. Parenti astro-ph/0608224
What changes in a protoneutron star?Temperature, neutrinotrapping(Nicotra)
Can the deconfinementprocess be associatedwith gamma-ray bursts?(Pagliara)
Can one make a hydrodynamicaldescription of thehadronic -> quarktransition?(Parenti)
O. Nicotra, M. Baldo, G.F. Burgio, H.-J. Schultze, astro-ph/0608021
A. Drago, A. Lavagno, I. Parenti, astro-ph/0512652
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A. Drago, A. Lavagno. G. Pagliara, Nucl. Phys. B138(2005)522
M. Alford, M. Braby, M. Paris, S. Reddy,APJ 629(2005)969
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Can we approach the quark phase transition with neutron-rich heavy-ion beams?
M. Di Toro, A. Drago, T. Gaitanos, V. Greco, A. Lavagno, NPA 775(2006)102
132Sn+132Sn
1GeV A
300 MeV A
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A signature of strange stars in gravitational waves
O. Benhar, V. Ferrari, L. Gualtieri, S. Marassi, astro-ph/0603464
If the quark phese is describedwithIn the bag model,the frequency of the fundamental mode depends on the value of the bag constant B
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Summary of the analysison quark NS content
1. The transition to quark matter in NS looks likely, but the amount of quark matter and the transition density depend on the quark matter model.
2. If the “observed” high NS masses (about 2 solar mass) have to be reproduced, additional repulsion is needed with respect to “naive” quark models .
3. Further constraints can come from other observationaldata (cooling, glitches …….)
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Schematic cross section of a Neutron Star
outer crust nuclei, e-
inner crust nuclei, n, e-
Nuclear matter layer n, p, e- , -
exotic core (a) hyperonic matter (b) kaon condensate (c) quark matter
drip = 4.3 1011 g/cm3
~1.5 1014 g/cm3
M 1.4 M R 10 km
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Superfluidity (homogeneous matter)
In most calculations, 1S0 pairing is neutron matter Is strongly suppressed by medium effects
A recent calculation based on Quantum Montecarlo yields a nuch smaller reduction of the gaps
A. Fabrocini, S. Fantoni, A. Yu Ilarionov,K.E: Schmidt, PRL 95(2005)192501
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nn
p
nn
nn
n
nnnn
density exc spin exc
isospin exc spin-isospin exc
p
n
p
Pairing interaction in neutron and nuclear matter and exchange of p.h. excitations
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antiscreening Vind >> Vdir
screeningVind << Vdir
L.G. Cao, U. Lombardo, P. Schuck, nucl-th/0608005
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Z
k
nk
Z=1 free Fermi gasZ<1 correlated Fermi system
' '3 ''2 2
' '
1
2 ( )
p pp pp p
p F p
Z V Zd p
Gap Equation
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Comparison with finite nuclei: attractive contributions from surface vibrations prevail
120Sn
Pairing gap due to exchange of density+spin fluctuations
Pairing gap due to exchange of of density density fluctuations only
G. Gori, F. Ramponi, F. Barranco,R.A. Broglia,P.F. Bortignon ,G. Colo, E. Vigezzi, PRC72(2005)11302
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The inner crust: coexistence of finite nuclei with a sea of free neutrons
J. Negele, D. VautherinNucl. Phys. A207 (1974) 298
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F=13.5MeV
Uniform Matter
Pairing gap in the Wigner cell
Potential in the Wigner cell Pairing gap in uniform neutron matter
Finite size effects on the pairing field
F=13.5MeV
P.M. Pizzochero, F. Barranco,E. Vigezzi, R.A. Broglia, APJ 569(2002)381
The difference is smallbut affects specific heatand the cooling process
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Spatial description of (non-local) pairing gap
The local-density approximation overstimates the decrease of the pairing gap in the interior of the nucleus.
R(fm) R(fm)
R(fm)
The range of the force is small compared to the coherence length, but not compared to the diffusivity of the nuclear potential
K = 0.25 fm -1
K = 2.25 fm -1
kF(R)
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Going beyond mean field: including the effects of polarization (exchange of vibrations) and of finite nuclei at the same time
G. Gori, F. Ramponi, F. Barranco,R.A. Broglia,G. Colo, D. Sarchi,E. Vigezzi, NPA731(2004)401
Spin modes
Density modes
RPA response In
duce
d pa
iring
inte
ract
ion
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However, the presence of the nucleus increases the gap by about 50%
With the adopted interaction,screening suppresses the pairing gap very strongly for kF >0.7 fm-1
Argonne (bare and uniform case)
Gogny (bare and uniform case)
Screening, uniform case
Screening + nucleus
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M. Baldo, U. Lombardo, E.E: Saperstein, S.V. Tolokonnikov, Nucl. Phys. A736(2004)241
New calculation of the optimal properties of the WIgner-Seitz cell including pairing
Without pairing
With pairing:smoothing ofshell effects
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The ‘global’ functional: matching Fayans functional (for finite nuclei) with BBG calculation for neutron matter
Microscopic, ‘exact’descriptionof neutron matter
Phenomenologicalfunctional with gradient terms:‘knows how to dealWit hthe surface’
Matching condition
Simplified pairing description: constant G which reproduces the BCS gap in neutron matter
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Comparison between phenomenological forces andmicroscopic calculations (BBG) at sub-saturationdensities.
M. Baldo, C. Maieron, P.Schuck, X. Vinas, Nucl. Phys. A736(2004)241
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Making the connection with finite nuclei:Microscopic functionals in neutron matter with gradient terms
Micr.Correl.term
Phen.gradient.term
+ Spin Orbit, Coulomb
A related but different approach: constraining the parameters of Skyrme interaction with the results of Brueckner calculations in homogeneous matter
L.G. Cao, U. Lombardo, C.W. Shen, N.Van Giai, PRC73(2006)14313
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peri
od
time
2.5year
As a rule, rotational period of a neutron star slowly increases because the system loses energy emitting electromagnetic radiation.
Glitches
One of the accredited explanations
Superfuid nature of nucleons in the inner crust
Sudden spin ups are measured, at regular intervals
glitch
P.W. Anderson and N.Itoh, Nature 256(1975)25
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A superfluid in a rotating container develops an array of microscopic linear vortices
Vortices may pin to container impurities, what may modify their dynamics. Sudden unpinning at critical period difference, due to Magnus force, would cause the glitch.
P.W. Anderson and N.Itoh, Nature 256(1975)25
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Calculations of pinned vortices:
-R. Epstein and G. Baym, Astrophys. J. 328(1988)680 Analytic treatment based on the Ginzburg-Landau equation
-F. De Blasio and O. Elgaroy, Astr. Astroph. 370,939(2001)Numerical solution of De Gennes equations with a fixed nuclear mean field and imposing cylindrical symmetry (spaghetti phase)
-P.M. Pizzochero and P. Donati, Nucl. Phys. A742,363(2004)Semiclassical model with spherical nuclei and fixed nuclear mean field.
HFB calculation of vortex in uniform neutron matter
Y. Yu and A. Bulgac, PRL 90, 161101 (2003)
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HFB
Semiclassical
(Avogadro)
P. Avogadro, F. Barranco, R.A. Broglia. E. Vigezzi, nucl-th/0602028
Importance of finite size effects
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BBG : PRC 69 , 018801 (20HHJ : Astrophys. J. 525, L45
(1999AP : PRC 58, 1804 (1998)
The baryonic Equations of State
BBG:
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density (fm-3)
E/A(MeV))
Comparison between BBG (solid line) Phys. Lett. B 473,1(2000)and variational calculations (diamonds) Phys. Rev. C58,1804(1998)
Pure neutron matterTwo-body forces only.
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Kh. Gad Nucl. Phys. 747 (2005) 655
Phenomenolocical area from Danielewicz et al.,Science 298 (2002) 1592
Nonostante le incertezzedell’ analisi sembra esserci unaben definita discriminazionetra le diverse EOS
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Schematic cross section of a Neutron Star
outer crust nuclei, e-
inner crust nuclei, n, e-
Nuclear matter layer n, p, e- , -
exotic core (a) hyperonic matter (b) kaon condensate (c) quark matter
drip = 4.3 1011 g/cm3
~1.5 1014 g/cm3
M 1.4 M R 10 km
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Composition of asymmetric and beta-stable matter
•Parabolic approximation
),0,(),1,(),(
),(),0,(),,(
2x-1parameter Asymmetry
2
p
YYYsym
YsymYY
pn
xA
Bx
A
BxE
xExA
Bx
A
B
•Composition of stellar matter
i) Chemical equilibrium among the
different baryonic species
ii) Charge neutrality
iii) Baryon number conservation
np
ep
e
epn
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Composition of asymmetric and beta-stable matterincluding hyperons
•Parabolic approximation
),0,(),1,(),(
),(),0,(),,(
2x-1parameter Asymmetry
2
p
YYYsym
YsymYY
pn
xA
Bx
A
BxE
xExA
Bx
A
B
•Composition of stellar matter
i) Chemical equilibrium among the
different baryonic species
ii) Charge neutrality
iii) Baryon number conservation
np
ep
n
pn
e
epn
2
extended to hyperons
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Composition of hyperonic beta-stable matter
I. Vidaña, I. Bombaci, A. Polls, A. Ramos, Astron. and Astrophys. 399 (2003) 687
Hyperonic Star
MB = 1.34 M
Baryon number density b [fm-3]
Radial coordinate [km ]
Par
ticl
e fr
acti
ons
Hyperonic core NM shell
cru
st
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Hyperon influence on hadronic EOS
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Composition of asymmetric and beta-stable matter
•Parabolic approximation
),0,(),1,(),(
),(),0,(),,(
2x-1parameter Asymmetry
2
p
YYYsym
YsymYY
pn
xA
Bx
A
BxE
xExA
Bx
A
B
•Composition of stellar matter
i) Chemical equilibrium among the
different baryonic species
ii) Charge neutrality
iii) Baryon number conservation
np
ep
e
epn
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•Shift of the hyperon onset points
down to 2-3 times saturation density
•At high densities N and Y present almost in the same percentage.
Including hyperons inside the neutron stars
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EOS MG/M R(km) nc / n0
BBB1 1.79 9.66 8.53
BBB2 1.92 9.49 8.45
WFF 2.13 9.40 7.81
BPAL12 1.46 9.04 10.99
BPAL22 1.74 9.83 9.00
BPAL32 1.95 10.54 7.58
Maximum mass configuration of pure nucleonic Neutron Stars for different EOS
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Mass-Radius relationMass-Radius relation
• Inclusion of Y decreases the maximum mass value
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•Shift of the hyperon onset points
down to 2-3 times saturation density
•At high densities N and Y present almost in the same percentage.
Including hyperons inside the neutron stars
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H.J. Schulze et al., PRC 73, 058801 (2006)
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Hyperons in Neutron Stars: implications for the stellar structure
The presence of hyperons reduces the maximum mass of neutron stars: Mmax (0.5 – 0.8) M
Therefore, to neglect hyperons always leads to an overstimate of the maximum mass of neutron stars
Microscopic EOS for hyperonic matter:
“very soft” EOS non compatible with measured NS masses.
Need for extra pressure at high density
Improved NY, YY two-body interaction
Three-body forces: NNY, NYY, YYY
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Quark Matter in Neutron Stars
QCD
Ultra-Relativistic Heavy Ion Collisions
Quark-deconfinement phase transition expected at
c (3 – 5) 0
The core of the most massive Neutron Stars is one of the best candidates in the Universe where such a deconfined phase of quark matter can be found
2SC
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Hybrid StarsHybrid Stars
outer crust
inner crust
Hadronic matter layer . n, p, hyperons, e- , -
Quark matter core
Mixed hadron-quark phase
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Including Quark matter
Since we have no theory which describes both confined and deconfined phases, we uses two separate EOS for baryon and quark matter and assumes a first order phase transition. a) Baryon EOS. BBG AP HHJ
b) Quark matter EOS. MIT bag model Nambu-Jona Lasinio Coloror dielectric model
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Al decrescere del valore della bag constant la massa massimadelle NS tende a crescere. Tuttavia B non puo’ essere troppopiccolo altrimenti lo stato fondamentale della materia nucleareall densita’ di saturazione e’ nella fase deconfinata !
Materia nucleare simmetrica
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1.1Q GeV3fm
Density dependent bag “constant”
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Evidence for “large” mass ?
Nice et al. ApJ 634, 1242 (2005) PSR J0751+1807 M = 2.1 +/- 0.2
Ozel, astro-ph /0605106 EXO 0748 – 676 M > 1.8
Quaintrell et al. A&A 401, 313 (2003) NS in VelaX-1 1.8 < M < 2
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J.M. Lattimer , M. Prakash, Science 304(2004)
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Mass radius relationshipMaximum mass
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Some (tentative) conclusions
1. The transition to quark matter in NS looks likely, but the amount of quark matter depends on the quak matter model.
2. If the “observed” high NS masses (about 2 solar mass) have to be reproduced, additional repulsion is needed with respect to “naive” quark models .
The situation resembles the one at the beginning of NS physics with the TOV solution for the free neutron gas
The confirmation of a mass definitely larger than 2would be a major breakthrough
3. Further constraints can come from other observational
data (cooling, glitches …….)
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Comparison between phenomenological forces andmicroscopic calculations (BBG) at sub-saturationdensities.
M.Baldo et al.. Nucl. Phys. A736, 241 (2004)
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Trying connection with phenomenology : the case.Density functional from microscopic calculations
microscopic functional
The value of r_n - r_p from mic. fun. is consistent with data
rel. mean field
Skyrme and Gogny
Pb208
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Looking for the energyminimum at a fixedbaryon density
Density = 1/30 saturationdensity
Wigner-Seitzapproximation
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In search of theenergy minimum as a function ofthe Z value insidethe WS cell
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Gamma Ray Bursts (GRBs)
Spatial distribution: isotropic
Distance: “cosmological” d = (1 – 10) 10 9 ly
Energy range: 100 keV – a few MeV
Emitted energy: ~ 10 51 erg (beamed / jets) J.S. Bloom, D.A. Frail, S.R. Kulkarni, ApJ 594, 2003
Duration: 1 – 300 s Two different types: short GRBs and long GRBs
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Temporal structure of GRBs
0. Supernova explosion
and then… (delay ? how long?)
1. Precursor delay…
2. Main event with quiescent times
3. Early X-ray afterglow, plateau and flares
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Temporal structure of GRBsin the quark deconfinement model
0. Supernova explosion neutron-proton starand then… (delay, mass accretion)
1. Precursor (formation of strangeness) delay… 2. Main event (formation of normal quark matter),
quiescent time, then... formation of superconducting quarks No need to inject energy continously during the precursor and the main event!
3. Early X-ray afterglow, plateau and flares (differential rotation, expulsion of the toroidal magnetic field, Haensel et al. in preparation, see previous talk)
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Analysis of time intervals between peaks within each emission episod A.D., G.Pagliara, astro-ph/0512602
Same temporal micro-structurewithin each emission episod
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Main results:
Never a detonation (no mechanical shock)
Always a deflagration with an unstable front
Convection can develop if hyperons are present in the hadronic phase or if diquark can condensate
Detonation or deflagration?A.D., A.Lavagno, I.Parenti, astro-ph/0512652
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Supernova-GRB connection: the Quark-Deconfinement Nova model
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A reaction that can generate gamma-ray is:A reaction that can generate gamma-ray is:
The efficency of this reaction in a strong gravitational field is The efficency of this reaction in a strong gravitational field is up toup to::
[J. D. Salmonson and J. R. Wilson, ApJ 545 (1999) 859][J. D. Salmonson and J. R. Wilson, ApJ 545 (1999) 859]
A reaction that can generate gamma-ray is:A reaction that can generate gamma-ray is:
The efficency of this reaction in a strong gravitational field is The efficency of this reaction in a strong gravitational field is up toup to::
[J. D. Salmonson and J. R. Wilson, ApJ 545 (1999) 859][J. D. Salmonson and J. R. Wilson, ApJ 545 (1999) 859]
How to generate GRBs main emission
2 ee
%10
The energy released (in the The energy released (in the strong deflagrationstrong deflagration) is carried out by ) is carried out by neutrinos and antineutrinos.neutrinos and antineutrinos.The energy released (in the The energy released (in the strong deflagrationstrong deflagration) is carried out by ) is carried out by neutrinos and antineutrinos.neutrinos and antineutrinos.
ergEE conv5251 1010
For bare quark starsdirect photon emissioncan be even more efficent!See previous talk byPawel Haensel
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Production of gamma-rays
Total energy released from the QDN: 1052 – 1053 erg
+ e+ + e- 2
E = Econv
(1) Ignoring strong gravit. effects on the cross section = Newt 0.01
(2) In a strong gravitational field (Salmonson and Wilson, ApJ 517,(1999))
GR = (10 – 30) Newt
at r R R (1.5 – 2.0) 2GM/c2
E = 1051 — 1052 erg
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Total energy released in the stellar conversion
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Finite size effects on the H-Q phase transition
The formation of a critical-size drop of QM is not immediate:
P = P – P0
overpressure with respect
to P0
above P0 hadronic matter is
in a metastable state
Quark matter drops form via a quantum nucleation process
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Energy released in the HSHyS(QS) convertion A.D., A.Lavagno, G.Pagliara, PRD69(2004)057505
Based on the “simple” scheme of Alford and Reddy PRD67(2003)074024
CFL gaps
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Potential energy barrier between the metastable hadronic phase and the quark phase
U(R) = (4/3) R3 nQ* (Q* - H ) + 4 R2 = av(P) R3 + asR2
The nucleation time depends dramaticaly on the value of the Hadronic Star’s central pressure (on the HS mass)
P2 > P1 > P0 log(/
sec)
Pres.
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Quark droplet nucleation time“mass filtering”
Critical mass forB1/4 = 170 MeV
Mass accretion
Critical mass for= 30 MeV/fm2
B1/4 = 170 MeV
Age of the Universe!
Berezhiani, Bombaci, Drago, Frontera, LavagnoApJ 586 (2003) 1250
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Conclusions
• The conversion of an hadronic star into a hybrid or quark star can be at the origine of (at least part of) the long GRBs.
• While in the collapsar model SN explosion and GRB need to be almost simultaneous, in the QM formation model a time delay between SN and GRB can exist, and its duration is regulated by mass accretion.
• The formation of diquark condensate can significantly increase the total energy released. “Evidence” of two active periods in long GRBs. The first transition, from hadronic matter to unpaired (or 2SC) quark matter acts as a “mass filter”. The second transition, producing (g)CFL quark matter can be described as a decay having a life-time of order tens of seconds
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QM formation after deleptonization and cooling
Pons et al. PRL 86 (2001) 5223
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