Astrophysical Quark Matter Renxin Xu ( 徐仁新 ) School of Physics, Peking University...

Astrophysical Quark Matter

Renxin Xu ( 徐仁新 )School of Physics, Peking University

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

2005 年 10 月 12 日，扬州大学

Not only is the Universe stranger than we

imagine, it is stranger than we can imagine.

—— Arthur Eddington

Astrophysical laboratory: to find QGP?

Cosmic QCD phase separation: consequence?

Compact pulsar-like stars: quark stars?

Cosmic rays: quark nuggets?

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

SUMMARYSUMMARY Introduction: Introduction: quarkquark && quark matterquark matter

QM in the early UniverseQM in the early Universe

QM in pulsar-like compact starsQM in pulsar-like compact stars

QM as cosmic raysQM as cosmic rays

ConclusionsConclusions

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Quark? A historical note …

M. Gell-Mann (1969)

Quarks?

1950s~1960s: A success in the classification of hadrons discovered in cosmic rays and in accelerators M. Gell-Mann (1964): Quarks? ---- in mathematical description, rather than in reality. Zweig, Chinese group (1960s): in reality? 1973: SU(3) non-Abelian gauge theory asymptotic freedom Experimental evidence for the last flavor of quark (top quark) in 1990s

Introduction: Quark matterIntroduction: Quark matterThe standard model of particle physics

Interaction via gauge bosons

QCDQCD

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Experimental evidence for asymptotic freedom

Introduction: Quark matterIntroduction: Quark matter

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

M. R. Pennington (University of Durham) in: QCD and Hadronic Physics (Held in PKU, Beijing, June 20, 2005)

The Nobel prize in Physics (2004)

David J. Gross (L) of the University of California at Santa Barbara and his wife (R)

Frank Wilczek of the Massachusetts Institute of Technology.

H. David Politzer of the California Institute of Technology, Pasadena, California.

What is Quark Matter?

Expected in QCD

To be a direct consequence of aympt. freedom

T

A simple QCD phase diagram

Introduction: Quark matterIntroduction: Quark matter

(Hadron gas)

(QGP)

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Can we find quark matter?Can we find quark matter?

Terrestrial experimentsRelativistic heavy ion colliders

Astrophysical observationsT-dominated QM: early UniverseD-dominated QM: compact stars

Introduction: Quark matterIntroduction: Quark matter

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Solid Quark Matter?Introduction: Quark matterIntroduction: Quark matter

B

T0 QCD phase?Phase diagram for CO2

Solid?Liquid?

Gas?Hadron

QGP

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

T deconfinement

chiral sym. restor.

Two kinds of Quark Matter.

Solid QM?

T-dom.

D-dom.

Introduction: Quark matterIntroduction: Quark matter

Xu 2005

“Pulsars and Quark Stars” http://vega.bac.pku.edu.cn/rxxu R. X. Xu“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

SUMMARYSUMMARY Introduction: Introduction: quarkquark && quark matterquark matter

QM in the early UniverseQM in the early Universe

QM in pulsar-like compact starsQM in pulsar-like compact stars

QM as cosmic raysQM as cosmic rays

ConclusionsConclusions

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Edward Witten (1984):1, cosmic QCD phase; 2, strange stars; 3, cosmic rays.

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

QM in the early UniverseQM in the early Universe

Bodmer-Witten’s conjecture

mu ~ 5

md ~ 10

ms ~150

=1.5N

F ~ 400

Farhi & Jaffe (1984) Greiner et al 1998

Introduction: Quark matterIntroduction: Quark matter

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

QM in the early UniverseQM in the early Universe

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

S. Banerjee, et al.hep-ph/0307366

Schwarzastro-ph/0303574Quark-hadron phase

transitiont ~ 10-5 s, Tc ~ 300 MeVFirst order reheating

QM in the early UniverseQM in the early Universe

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Motivations to study quark-hadron transitionto know “What happened at the transition?”to set initial physical conditions for BBN

•inhomogeneous distribution abundancesto generate relics of cosmic QCD transition

•strange quark nuggets? (MACHOs?)•gravitational waves from colliding bubbles?•magnetic fields with ~ 100 kpc correlations?•QCD balls as a new CDM candidate?•black holes formation during the transition?

SUMMARYSUMMARY Introduction: Introduction: quarkquark && quark matterquark matter

QM in the early UniverseQM in the early Universe

QM in pulsar-like compact starsQM in pulsar-like compact stars

QM as cosmic raysQM as cosmic rays

ConclusionsConclusions

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

L. Landau (1962)S. Chandrasekhar (1983)

Maybe there are stars with

nuclear density after collapse?

Degenerate pressure is not omnipotent in standing against the gravitational collapse

A historical note of pulsars

“Neutron” star

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Walter Baade and Fritz Zwickyproposed in 1934 that supernovaecould produce cosmic rays andneutron stars …

A historical note of pulsars

Pulsars (discovered in

1967) could be neutron

stars?

A. Hewish (1974)

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Pulsars in conventional scenarioPulsars in conventional scenario

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Radio pulsars: cosmological lighthouse ...Pulse sequences from a radio pulsar

Pulsar is pulsing …

Neutron Stars

or

Quark stars?

Pulsars in conventional scenarioPulsars in conventional scenario

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Pulsars in conventional scenarioPulsars in conventional scenarioDistribution of radio pulsars in the Galaxy

Radio pulsars

Accretion-powered X-ray pulsarsX-ray bursts

AXP/SGRDim thermal “Neutron” stars

Compact center objects

Members of the family of pulsar-like stars …

What’s really the nature of pulsars?

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

The structure of normal Neutron stars

Heiselberg 2002

Atmosphere

Outer crust

Inner crust

Neutron matter

Core ？

QM in pulsar-like compact starsQM in pulsar-like compact stars

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Pulsars: quark stars?Ivanenko & Hurdgelaidze (1969)

Itoh (1970)

Bodmer (1971)

Asymptotic freedom

Witten (1984)

1986: Haensel et al.; Alcock et al.

QM in pulsar-like compact starsQM in pulsar-like compact stars

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

http://chandra.harvard.edu/photo/2002/0211/0211_illustration.pdf

Neutron Stars

v.s.

Quark Stars

QM in pulsar-like compact starsQM in pulsar-like compact stars

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Two requirements for forming quark starQuark de-confinement can occur

•An estimate of c ： (4R3/3)-1 ~ 1.5 N

Strange matter in bulk is absolutely stable __(Bodmer-Witten’s conjecture)

•Note: Strangelet in RHIC could be unstable!

Unfortunately, one can not know if these two are satisfied from the first principles (QCD). But the requirements seem ok …

QM in pulsar-like compact starsQM in pulsar-like compact stars

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Structure of strange star: bare or crusted

Electric field:

E ~ 1017V/cm

QM in pulsar-like compact starsQM in pulsar-like compact stars

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

How to form a quark star?

QM in pulsar-like compact starsQM in pulsar-like compact stars

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

What if to form a quark star, rather than a neutron stars, in a CC-process?

This idea is attractive since more energy and radiation (, ) are released …

It is still a challenge for astrophysicists to reproduce a successful core-collapse supernova!

Note: quark stars formed in this way should be bare!

QM in pulsar-like compact starsQM in pulsar-like compact stars

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

A summary of our work only …

QM in pulsar-like compact starsQM in pulsar-like compact stars

Evidence for quark stars?Evidence for quark stars?

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

To solve the binding energy problem (1999)Observations: drifting subpulses of PSRs

To expect non-atomic spectra (2002)Observations: thermal & non-thermal

To explain discrepancy between … (2004)Observations: free prec. & glitch of PSRs

To understand others …Observations: superE SGR, -profile (AG)

QM in pulsar-like compact starsQM in pulsar-like compact stars

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

NASA News release (2002/4/10): RX J1856 a strange star?

Chandra

QM in pulsar-like compact starsQM in pulsar-like compact stars

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Submillisecond radio pulsar: FAST?

Low-mass & small-radius pulsar-like stars: X-ray interference telescopes MAXIM?

Gravitational wave observations: LIGO?

Dust emission from ms-pulsars: Spitzer?

How to identify clearly a quark star?

QM in pulsar-like compact starsQM in pulsar-like compact stars

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Five hundred meter Aperture Spherical Telescope

QM in pulsar-like compact starsQM in pulsar-like compact stars

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

SUMMARYSUMMARY Introduction: Introduction: quarkquark && quark matterquark matter

QM in the early UniverseQM in the early Universe

QM in pulsar-like compact starsQM in pulsar-like compact stars

QM as cosmic raysQM as cosmic rays

ConclusionsConclusions

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

QM as cosmic raysQM as cosmic rays

The higher the particle energy attained, the smaller __the scale of physics which can be probed.Cosmic rays vs. Particle physics

1937 (Anderson & Neddermeyer): 1947 (Powell): 1947(Rochester & Butler): strange part. 0, K, ...

Cosmic rays vs. AstrophysicsGenerally, astrophysics studies “cosmic rays”Astrophysics offers extreme environments

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

UHECRs:>~1019eV

The highest!

Within the Galaxy

QM as cosmic raysQM as cosmic rays

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

GZK cutoff: estimations

Ep ~ 1019 eV, ~ Ep/1GeV ~ 1010

ECB ~ 3 K ~ 10-4 eV

Proton rest frameE’CB ~ ECB ~ MeV

Greisen PRL (1966); Zatsepin & Kuzmin JETP (1966)

QM as cosmic raysQM as cosmic rays

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

The GZK cutoff'p p s

196 10 eVthE

with threshold

Other particles

Photon, Iron

QM as cosmic raysQM as cosmic rays

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

No clear GZK cutoff observed Stecker 2003

QM as cosmic raysQM as cosmic rays

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

ML03

UHECRs: quark nuggets (strangelets)?

What is Strangelet?=>A lump of strange matter

Advantages if UHECRs are strangelets:

Larger mass Beyond GZK cutoff

Higher electricity Easier to accelerate

Be not point-like No collapse to BHs(Xu & Wu 2003)

QM as cosmic raysQM as cosmic rays

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

What is the astrophysical origin of strangelets?during the early Universe?

during the formation of quark stars!Acceleration in induced electric field ~ 1017/P10eV

Formation by stellar processes

1, Evaporation during SNEs

2, Collision of (low-mass) strange QSsGRBs

QM as cosmic raysQM as cosmic rays

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

T deconfinement

chiral sym. restor.

How do strangelets evolve in the atmosphere?Solid strangelets

Fluid strangelets

Evaporating hadrons: n, p, ...

QM as cosmic raysQM as cosmic rays

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

How can we detect strangelets?

Atmospheric Cerenkov radiation?

Atmospheric fluorescence radiation?

ESA: in YBJ?

Neutron detection in YBJ?

…?

QM as cosmic raysQM as cosmic rays

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Cosmic raydetectionin YBJ

SUMMARYSUMMARY Introduction: Introduction: quarkquark && quark matterquark matter

QM in the early UniverseQM in the early Universe

QM in pulsar-like compact starsQM in pulsar-like compact stars

QM as cosmic raysQM as cosmic rays

ConclusionsConclusions

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

ConclusionsConclusionsAstrophysical quark matter are reviewed. In addition to test GR, pulsars are also useful to test and to improve the fundamental strong interaction.

Possible evidence for quark stars are proposed.

The physics relevant to the elementary chromatic interaction could be improved if pulsar-like stars are quark stars.

A solid state of quark matter is suggested.

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

Thank you ！

“Astrophysical QM” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

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