引力与相对论天体物理

Astrophysical

QuarkMatterRenxin

Xu(徐仁新)School

of

Physics,

Peking

University2005年10月12日，扬州大学“Astrophysical

QM”/rxxu➢imagine,

it

is

stranger

than

we

can

imagin➢——

ArthurEddingtonAstrophysical

laboratory:

to

find

QGP?·Cosmic

QCD

phase

separation:

consequence?·Compact

pulsar-like

stars:

quark

stars?·Cosmic

rays:

quark

nuggets?“Astrophysical

QM”/rxxuSUMMARYIntroduction:

quark

&

quark

matteQM

in

the

earlyUniverseQM

in

pulsar-like

compact

starsQM

as

cosmic

raysConclusions“Astrophysical

QM”/rxxuQuark?

A

historical

note

…M.

Gell-Mann

(1969)Quarks?1950s~1960s:

A

success

inthe

classification

of

hadrondiscovered

in

cosmic

rays

andin

acceleratorsM.

Gell-Mann

(1964):Quarks?

----

in

mathematicaldescription,

rather

than

inreality.Zweig,

Chinese

group(1960s):

in

reality?1973:

SU(3)

non-Abelianasymptoticgauge

theoryfreedomExperimental

evidence

forthe

last

flavor

of

quark

(topquark)

in

1990sIntroduction:

Quark

matteruThe

standard

model

ofparticle

physicsInteraction

via

gauge

bosQCD“Astrophysical

QM”/rxxuuExperimental

evidence

for

asymptotic

freedIntroduction:

Quark

matter“Astrophysical

QM”/rxxuM.

R.

Pennington

(University

of

Durham)

in:

QCD

aHadronic

Physics

(Held

in

PKU,

Beijing,

June

20,The

Nobel

prize

in

Physics

(2004)David

J.

Gross

(L)

of

theUniversityof

Californiaat

Santa

Barbara

and

hiswife

(R)Frank

Wilczekof

theMassachusettsInstitute

ofTechnology.H.

DavidPolitzer

of

theCaliforniaInstitute

ofTechnology,Pasadena,California.uWhat

is

Quark

Matter?ÞExpectedin

QCDIntroduction:

Quark

matter(Hadron

gas)To

be

a

direct

consequence

ofaympt.

freedomA

simple

QCD

phase

diagram(QGP)“Astrophysical

QM”/rxxuCan

we

find

quark

matter?·Terrestrial

experimentsÞRelativistic

heavy

ion

collide·Astrophysical

observationsÞT-dominated

QM:

earlyUniverseÞD-dominated

QM:

compact

starsIntroduction:

Quark

matter“Astrophysical

QM”/rxxuuSolid

Quark

Matter?Introduction:

Quark

matterBSolid?Liquid?Gas?HadronQGP0QCD

phase?TPhase

diagram

for

CO2“Astrophysical

QM”/rxxuuTwo

kinds

of

Quark

Matter.Solid

QM?T-dom.D-dom.Introduction:

Quark

matterXu

2005“APAPsusutltlrsrsoaoarprphshsyasnidcQaulaQrMk”Starhst”tp:h/t/tvpe:g/a/.vbeagac.pbkauc.epdku.cend/ur.xcxnu/rxSUMMARYIntroduction:

quark

&

quark

matte√

QM

in

the

early

UniverseQM

in

pulsar-like

compact

starsQM

as

cosmic

raysConclusions“Astrophysical

QM”/rxxuEdward

Witten

(1984):1,

cosmic

QCD

phase;

2,

strange

stars;

3,

cosmicrayQM

in

the

early

Universe“Astrophysical

QM”/rxxuuBodmer-Witten’sconjectureeumu

~

5umd

~

10ums

~150u

=1.5Nu

F

~

400uFarhi

&u

Jaffeu

(1984)Greiner

et

al

1998Introduction:

Quark

matter“Astrophysical

QM”/rxxuCome

back

whenwe

discuss

p-pdot

diagramB

critical

=

4.4x10^13

GQM

in

the

early

UniverseSchwarzastro-ph/0303574Quark-hadron

phasetransitiont

~

10-5

s,

Tc

~

300

MeVFirstorderS.

Banerjee,

et

al.hep-ph/0307366reheating“Astrophysical

QM”/rxxuCome

back

whenwe

discuss

p-pdot

diagramB

critical

=

4.4x10^13

GQM

in

the

early

UniverseMotivations

to

study

quark-hadron

transit“Astrophysical

QM”/rxxuto

know

“What

happened

at

thetransition?”to

set

initial

physical

conditions

for

Binhomogeneous

distribution

abundanceto

generate

relics

of

cosmic

QCD

transitstrange

quark

nuggets?

(MACHOs?)gravitational

waves

from

colliding

bubbmagnetic

fields

with

~

100

kpc

correlatiQCD

balls

as

a

new

CDM

candidate?black

holes

formation

during

the

transitSUMMARYIntroduction:

quark

&

quark

matteQM

in

the

earlyUniverse√

QM

in

pulsar-like

compact

starsQM

as

cosmic

raysConclusions“Astrophysical

QM”/rxxuA

historical

note

of

pulsarsDegeneratepressure

is

notomnipotent

instanding

against

thegravitationalcollapseMaybe

thereare

stars

withnucleardensity

aftercollapse?“Neutron”starS.

Chandrasekhar

(1983)L.

Landau

(1962)“Astrophysical

QM”/rxxuWalter

Baade

and

Fritz

Zwickyproposed

in

1934

that

supernovaecould

produce

cosmic

rays

andneutron

stars

…A

historical

note

of

pulsarsPulsars(discoveredin

1967)could

beneutronstars?A.

Hewish

(1974)“Astrophysical

QM”/rxxuPulsars

in

conventional

scenariouRadio

pulsars:

cosmological

lighthousePulse

sequences

from

a

radio

pulsarPulsar

is

pulsing

…“Astrophysical

QM”/rxxuCome

back

whenwe

discuss

p-pdot

diagramB

critical

=

4.4x10^13

GsNeutron

StarorQuark

stars?Pulsars

in

conventional

scenario“Astrophysical

QM”/rxxuPulsars

in

conventional

scenariouDistribution

of

radio

pulsars

in

the

Gal“Astrophysical

QM”/rxxuRadio

pulsarsAccretion-powered

X-raypulsarsX-ray

burstsAXP/SGRDim

thermal

“Neutron”

starsCompact

centerobjectsMembers

of

the

family

of

pulsar-like

stars

…What’s

reallythe

nature

ofpulsars?“Astrophysical

QM”/rxxuHeiselberg

2002uThe

structure

of

normal

Neutron

starsAtmosphereOuter

crustInner

crustNeutron

matterCore？QM

in

pulsar-like

compact

stars“Astrophysical

QM”/rxxuuPul➢sIavrasne:nqkuoa&rHkusrsdtgaerlsa?idze

(1969)Itoh

(1970)Bodmer

(1971)Asymptotic

freedomWitten

(1984)1986:

Haensel

et

al.;

Alcock

etal.QM

in

pulsar-like

compact

stars“Astrophysical

QM”/rxxu/photo/2002/0211/0211_illustration.uNeutronStarsuv.s.uQuarkStarsQM

in

pulsar-like

compact

stars“Astrophysical

QM”/rxxuCome

back

whenwe

discuss

p-pdot

diagramB

critical

=

4.4x10^13

GuTwo

requirements

for

forming

quark

starQuark

de-confinement

can

occurAnestimateof

c：(4 R3/3)-1

~

1.5NStrange

matter

in

bulk

is

absolutely

sta (Bodmer-Witten’s

conjecture)Note:

Strangelet

in

RHIC

could

be

unstable!uUnfortunately,

one

can

not

know

if

thesetwo

are

satisfied

from

the

first

princip(QCD).

But

the

requirements

seem

ok

…QM

in

pulsar-like

compact

stars“Astrophysical

QM”/rxxuuStructure

of

strange

star:

bare

or

crusElectric

field:E

~

1017V/cmQM

in

pulsar-like

compact

stars“Astrophysical

QM”/rxxuHow

to

form

a

quark

star?QM

in

pulsar-like

compact

stars“Astrophysical

QM”/rxxuIt

is

still

a

challenge

for

astrophysicistsreproduce

asuccessful

core-collapse

superWhat

if

to

form

a

quark

star,

rather

tha

a

neutron

stars,

in

a

CC-process?This

idea

is

attractive

since

more

ener

and

radiation

(

,

)

are

released

…Note:

quark

stars

formed

in

this

way

should

be

baQM

in

pulsar-like

compact

stars“Astrophysical

QM”/rxxuCome

back

whenwe

discuss

p-pdot

diagramB

critical

=

4.4x10^13

GQM

in

pulsar-like

compact

starsEvidence

for

quark

stars?A

summary

of

our

work

only

…“Astrophysical

QM”/rxxu·To

solve

the

binding

energy

problem

(199ÞObservations:

drifting

subpulses

of

P·To

expect

non-atomic

spectra

(2002)ÞObservations:

thermal

&

non-thermal·To

explain

discrepancy

between

…

(2004ÞObservations:

free

prec.

&

glitch

of

P·To

understand

others

…ÞObservations:

superE

SGR,-profile(AG)QM

in

pulsar-like

compact

stars“Astrophysical

QM”/rxxuCome

back

whenwe

discuss

p-pdot

diagramB

critical

=

4.4x10^13

GNASA

News

release

(2002/4/10):

RX

J1856

a

strange

stChandraQM

in

pulsar-like

compact

stars“Astrophysical

QM”/rxxuCome

back

whenwe

discuss

p-pdot

diagramB

critical

=

4.4x10^13

GHow

to

identify

clearly

aquark

st·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:

SpitzeQM

in

pulsar-like

compact

stars“Astrophysical

QM”/rxxuI

amintroducing

youFive

hundred

meter

Aperture

Spherical

TelescQM

in

pulsar-like

compact

starsI

amintroducing

you“Astrophysical

QM”/rxxuSUMMARYIntroduction:

quark

&

quark

matteQM

in

the

earlyUniverseQM

in

pulsar-like

compact

stars√

QM

as

cosmic

raysConclusions“Astrophysical

QM”/rxxuQM

as

cosmic

raysThe

higher

the

particle

energy

attained,

thethe

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.

Astrophysics√Generally,

astrophysics

studies

“cosmic√Astrophysics

offers

extreme

environments“Astrophysical

QM”/rxxuUHECRs:>~1019eVuThe

highesWithin

theGalaxyQM

as

cosmic

rays“Astrophysical

QM”/rxxuuGZK

cutoff:

estimationsuEp

~

Ep/1GeV

~~

1019

eV,1010uECB

~

3

K

~

10-4

eVProton

rest

frameE’CB

~ ECB

~

MeVGreisen

PRL

(1966);

Zatsepin

&

Kuzmin

JETP

(19QM

as

cosmic

rays“Astrophysical

QM”/rxxuCome

back

whenwe

discuss

p-pdot

diagramB

critical

=

4.4x10^13

GuThe

GZK

cutoffwith

thresholduOther

particlesPhoton,IronQM

as

cosmic

rays“Astrophysical

QM”/rxxuStecker2003QM

as

cosmic

raysuNo

clear

GZK

cutoff

observed“Astrophysical

QM”/rxxuCome

back

whenwe

discuss

p-pdot

diagramB

critical

=

4.4x10^13

GuUHECRs:

quark

nuggets

(strangelets)?uWhat

is

Strangelet?=>A

lump

of

strange

mattuAdvantages

if

UHECRs

are

strangelets:Larger

mass Beyond

GZK

cutoffML03Higher

electricityBe

not

point-likeEasier

to

accelNo

collapse

to

B(Xu

&

Wu

2003)“Astrophysical

QM”/rxxuQM

as

cosmic

raysCome

back

whenwe

discuss

p-pdot

diagramB

critical

=

4.4x10^13

GuWhat

is

the

astrophysical

origin

of

stranduring

the

early

Universe?during

the

formation

of

quark

stars!√Acceleration

in

induced

electric

field

~

1017/P1√Formation

by

stellar

processes1,

Evaporation

during

SNEs2,

Collision

of

(low-mass)

strange

QSGRBsQM

as

cosmic

rays“Astrophysical

QM”/rxxuCome

back

whenwe

discuss

p-pdot

diagramB

critical

=

4.4x10^13

GuHow

do

strangelets

evolve

in

the

atmospheSolid

strangeletFluid

strangeletEvaporatinghadrons:

n,

p,

..QM

as

cosmic

rays“Astrophysical

QM”/rxxuCome

back

whenwe

discuss

p-pdot

diagramB

critical

=

4.4x10^13

GuHow

can

we

detect

strangelets?Atmospheric

Cerenkov

radiation?Atmospheric

fluorescence

radiation?ESA:

in

YBJ?Neutron

detection

in

YBJ?…?QM

as

cosmic

rays“Astrophysical

QM”/rxxuCosmic

raydetectionin

YBJSUMMARYIntroduction:

quark

&

quark

matteQM

in

the

earlyUniverseQM

in

pulsar-like

compact

starsQM

as

cosmic

rays√

Conclusions“Astrophysical

QM”/rxxuConclusions·Astrophysical

quark

matter

are

reviewed.

Inadditio