cooling of compact stars - institute of nuclear...
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Structure and Cooling of Compact Stars obeying Modern Constraints David Blaschke (Wroclaw University, JINR Dubna)
Facets of Strong Interaction Physics, Hirschegg, January 17, 2012
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Structure and Cooling of Compact Stars obeying Modern Constraints David Blaschke (Wroclaw University, JINR Dubna)
Facets of Strong Interaction Physics, Hirschegg, January 17, 2012
PSR J16142230 M=(1.97+/0.04) M_sun
Demorest et al., Nature (2010)
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Structure and Cooling of Compact Stars obeying Modern Constraints David Blaschke (Wroclaw University, JINR Dubna)
Facets of Strong Interaction Physics, Hirschegg, January 17, 2012
Neutron star in SNR Cas AFast cooling directly observed
Ho & Heinke, Nature (2009)
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Structure and Cooling of Compact Stars obeying Modern Constraints
Thanks to ‘cool’ coauthors: Hovik Grigorian, Fridolin Weber, Dima Voskresensky and ‘dense’ ones: Thomas Klaehn, Rafal Lastowiecki, Fredrik Sandin, Daniel Zablocki
David Blaschke (Wroclaw University, JINR Dubna)
Facets of Strong Interaction Physics, Hirschegg, January 17, 2012
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Recent systematic studies: S. Weissenborn et al., ApJ Lett. 740 (2011)L. Bonanno & A. Sedrakian, 1108.0559 (2011)
T. Klahn et al., 1111.6889; R. Lastowiecki et al. (in preparation)
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Acta Phys. Pol. Suppl. 3, 641 (2010); arxiv:1004.4375 [hepph]
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Fischer et al., arxiv: 1103.3004
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Implications from PSR J16142230 within 3fCS NJL – DBHF model
HIC: n_c ~ 4n_0
2SC QM
If hybrid star,Then:
Vector MF
If no hybrid star, then:
small (<0.85)diquark coupl.
HIC: n_c > 4.5 n_0
T. Klahn et al., Acta Phys. Pol. (to appear); arxiv: 1111.6889
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Same hybrid model (3fCS NJL – DBHF) , smaller chiral condensate (quark mass)
HIC: n_c ~23 n_0
2SC QM
If hybrid star,Then:
Vector MF
If no hybrid star, then:
small (<0.85)diquark coupl.
HIC: n_c > 2 n_0
R. Lastowiecki et al., in preparation
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The question of hyperons … … and quarkhyperon hybrids
Hyperonic matter without strange vector meson Repulsion too soft; Demorest constraint failed→ Inclusion of phimeson repulsion OK→ Phase transition: “masquerade” problem … Density dependence of gluon sector (bag) !
Lastowiecki et al., 1112.6430 [nuclth]
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Exploring hybrid star matter at NICA & FAIRT.Klähn (1), D.Blaschke (1,2), F.Weber (3)(1) Institute for Theoretical Physics, University of Wroclaw, Poland
(2) Joint Institute for Nuclear Research, Dubna(3) Department of Physics, San Diego State University, USA
HeavyIon Collisions Compact Stars
„The CBM Physics Book“, Springer LNP 841 (2011), pp.158181; arxiv:1101.6061
Proposal: 1. Measure transverse and elliptic flow for a wide range of energies (densities) at NICA and perform Danielewicz's flow data analysis > constrain stiffness of high density EoS2. Provide lower bound for onset of mixed phase > constrain QM onset in hybrid stars
stiff EoS(at flow limit)
low ncrit
(at NICA fixT)
soft EoS (dashed line)
high Mmax
(J16142230)
low Monset (all NS hybrid)
excluded(J16142230)
NICA White Paper
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Conclusions I PSR 1614-2230 (“Demorest-pulsar”) puts
strong constraints to dense matter EoS Both alternatives for the inner structure,
hadronic and hybrid star, are viable for the Demorest pulsar; HIC favors hybrid model
If Demorest pulsar has a quark matter (QM)core, then QM must:- be color superconducting– - have a strong (vector-field) repulsion
– - occur at >2 n0 in HIC, depending on <qq>
Discriminating test? Measure M-R relation !!
-
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Neutron Star in Cassiopeia A (Cas A)• 16.08.1680 John Flamsteed
6m star 3 Cas
• 1947 re-discovery in radio
• 1950 optical counterpart
• T ∼ 30 MK
• V exp ∼ 4000 − 6000 km/s
• distance 11.000 ly = 3.4 kpc
picture: spitzer space telescope
Ho & Heinke, Nature 462 (2009) 71, Heinke & Ho, arxiv:1007.4719
Page, Prakash, Lattimer, Steiner, PRL (2011); arxiv:1011.6142Shternin, Yakovlev, Heinke, Ho, Patnaude, MNRAS (2011); arxiv:1012.0045
D.Blaschke, H. Grigorian, D. Voskresensky, F. Weber, arxiv:1108.4125
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Cas A Cooling Observations Cas A is a rapidly cooling star – Temperature drop ~4% in 10 years
W.C.G. Ho, C.O. Heinke, Nature 462, 71 (2009)
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Cas A Cooling Observations
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The influence of the (core) heat conductivity
Blaschke, Grigorian, Voskresensky, A&A 424, 979 (2004)
oCas A
http://www.nature.com/news/2011/110201/full/news.2011.64.html?s=news_rss#commentid18186
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Phase Diagram & Cooling Simulation
Description of the stellar matter - local propertiesModeling of the self bound compact star - including the gravitational fieldExtrapolations of the energy loss mechanisms to higher densities and temperatures Consistency of the approaches
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Cooling Mechanism
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The energy flux per unit time l(r) through a spherical slice at distance r from the center is:
The equations for energy balance and thermal energy transport are:
where n = n(r) is the baryon number density, NB = NB(r) is the total baryon number in the sphere with radius r
F.Weber: Pulsars as Astro. Labs ... (1999);
D. Blaschke Grigorian, Voskresensky, A& A 368 (2001)561.
Cooling Evolution
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• Quark direct Urca (QDU) the most efficient process
Compression n/n0 ≃ 2, strong coupling αs ≈ 1
• Quark Modified Urca (QMU) and Quark Bremsstrahlung
• Suppression due to the pairing
• Enhanced cooling due to the pairing
Neutrino Emissivities in Quark Matter
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Surface Temperature & Age Data
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Crust Model
Time dependence of the light element contents in the crust
Page,Lattimer,Prakash & Steiner, Astrophys. J. 155, 623 (2004)
Yakovlev, Levenfish, Potekhin, Gnedin & Chabrier , Astron. Astrophys , 417, 169 (2004)
Blaschke, Grigorian, Voskresensky, A& A 424 (2004) 979
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DU constraint
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DU ThresholdsDU critical densities DU critical masses
nc = 2.7 n0 NLW (RMF)
nc = 5.0 n0 HHJ (APR)
Mc = 1.25 Msun – NLW
Mc =1.84 Msun - HHJ
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DU problem & constaint
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SC pairing gaps – hybrid stars2SC phase: 1 color (blue) is unpaired (mixed superconductivity)Ansatz 2SC + X phase:
Grigorian, DB, Voskresensky , PRC 71 (2005) 045801
Pairing gaps for hadronic phase(AV18 Takatsuka et al. (2004))
Blaschke, Grigorian, Voskresensky , A&A 424 (2004) 979
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SC pairing gaps – hybrid stars
Popov, Grigorian, Blaschke, PRC 74 (2006)
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Influence of SC on luminosity
Critical temperature Tc, for the proton 1S0 and neutron 3P2 gaps, used in
Page, Lattimer, Prakash & Steiner, Astrophys. J. 707 (2009) 1131
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Tc ‘measurement’ from Cas A 1.4 M star built from ⊙ the APR EoS Rapid cooling at ages
30100 yrs due to the ∼thermal relaxation of the crust Mass dependence
Page, Lattimer, Prakash & Steiner,Phys. Rev. Lett. 106 (2011) 081101
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Medium effects in cooling of neutron stars Based on Fermi liquid
theory: Landau (1956), Migdal (1967), Migdal et al. (1990)
MMU – instead of MU
PBF – fast cooling process for T<Tc
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AV18 gaps, pi-condensate, without suppression of 3P2 neutron pairing - Enhanced PBF process
Anomalies because of PBF proccessGaps taken from Yakovlev at al. (2003)
Grigorian, Voskresensky Astron.Astrophys. 444 (2005)
n 3P2 gap strongly suppressed: Friman&Schwenk, PRL (2004)
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The influence of the (core) heat conductivity
Blaschke, Grigorian, Voskresensky, A&A 424, 979 (2004)
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The influence of the (core) heat conductivity
Blaschke, Grigorian, Voskresensky, A&A 424, 979 (2004)
oCas A
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Cas A as a Hadronic Star – arxiv:1108.4125Evolution of T profiles
Partial contributions to L
Pion Urca? See in 10 50 years !
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Temperature in the Hybrid Star Interior
Blaschke, Grigorian, Voskresensky, A& A 368 (2001) 561
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Cas A as an Hybrid Star
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Cas A as Hybrid Star: Tprofile evolution
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Conclusions II Cas A rapid cooling consistently described by
the nuclear medium cooling model as a “first drop”, delayed by low conductivity
Both alternatives for the inner structure, hadronic and hybrid star, are viable for Cas A; a higher star mass favors the hybrid model
In contrast to the minimal cooling scenario, our approach is sensitive to the star mass and thermal conductivity of superfluid star core matter
Discriminating test? Log N – Log S !! (?)
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It's cool to be a CompStar member!
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Upcoming School and Conference ...
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Thanks for Your attention!
Research ...
… is gong on!