Quark-Nova: Astrophysical Implications

A primer on Compact Stars and

Type II Super-novae

A primer on Quark Stars and Quark-Novae

Application to brightest Supernovae (SN 2006gy case)

Application to Epoch of Reionization

R. Ouyed (U. Calgary)

Quark-Nova: Astrophysical Implications

A primer on Compact Stars and

Type II Super-novae

A primer on Quark Stars and Quark-Novae

Application to brightest Supernovae (SN 2006gy case)

Application to Epoch of Reionization

R. Ouyed (U. Calgary)

Part II: Jan Staff

Part III: Brian Niebergal

Type II Supernovae

(Core-collapse Supernovae)

Type II Supernovae

(Core-collapse Supernovae)

Mass > 8 Msun

Core-CollapseSupernovae

Hydrogen present when they explode!

Mass-shedding Stars

Mass-shedding Stars

Black Holes

Neutron Stars

White Dwarfs

May or may not have hydrogen when they explode!

Energy releaseEnergy release

GRAVITY → RADIATION !!!GRAVITY → RADIATION !!!

NS

Grav. Energy (1053 erg) Kinetic Energy (1051 ergs) Radiation (1049 ergs)1% 1%

The Quark-Nova

Compact Stars in the QCD Phase DiagramCompact Stars in the QCD Phase Diagram

Hybrid stars

Think of a Quark Star as a nucleon with ~1057 quarks.

The quarks are still confined!

u and d convert to s in order to reduce Pauli repulsion by

increasing flavor degeneracy

?

TG

Upon reaching a critical density (~5 times nuclear density),

the core of the neutron star converts rapidly into (u,d,s)

quark matter

Hybrid Stars (HS) Neutron Stars with Quark

Cores

Hybrid Stars (HS) Neutron Stars with Quark

Cores

Lead to Black Holes

Lead to Neutron Stars

Heavy NSs(HS candidates)

Neutron star to Quark star Transition

The quark matter core becomes

unstable and shrinks faster

than the enveloperesponse time!

The QUARK-NOVA !

ENERGY RELEASE (Huge Energy Reservoir)

Gravitational (~ 1053 ergs) Conversion (~ 50 MeV per baryon ----> 5x1052 ergs)

Core collapse

Neutrino & photon emission

The KEY message to “explosive astrophysics”community:

Quark Matter Photon Fireball !

The KEY message to “explosive astrophysics”community:

Quark Matter Photon Fireball !

CFL

QN key ingredients

Energy Reservoir (more than 1053 erg)

Photon Fireball (up to 1052 ergs in K)

Ultra-relativistic iron-rich ejectum

Heavy-element-rich (A>130) ejecta

+ Massive Progenitor

"This was a truly monstrous explosion, a hundred times more energetic than a typical supernova,"

Quark Nova

and

Super-luminous Supernovae

1051 ergs in Radiation !

100 times a normal Supernova !

3 Possible Mechanisms3 Possible Mechanisms

(1) interaction of the supernova blast wave with circumstellar material (CSM)

(2) energy from radioactive decay of 56Ni

(3) Oscillating PISN

(1) interaction of the supernova blast wave with circumstellar material (CSM)

(2) energy from radioactive decay of 56Ni

(3) Oscillating PISN

Need too much surroundingEjecta !

Need too much Nicke !

Very massive progenitor !Artificial energy input!

Ekinetic = 6.4x1052 erg; Mejecta = 53Msun; M(Ni+CO) = 15Msun

Standard picture stretched to the extreme !

Quark-NovaEjecta

QuarkStar

NeutronStar

What does theQuark-Novahas to offer

in this context?

Dual Explosion!

Application SN2006gy

Application SN2006gy

Mejec = 40Msun

Rstar = 10 Rsun

2000 < VSN (km/s) < 4800 tdelay = 15 days

Light-Curves of SN2005gj

and SN2005ap

Light-Curves of SN2005gj

and SN2005ap

Keep same parametersas for SN2006gy except

SN2005gjtdelay = 10 days

SN2005aptdelay = 40 days

Find the first bump (the SN) before the second bump (the QN)

A double-hump!

Kawabata et al. 2009, ApJ

The Nature of the Beast

As the photosphere receedsdeeper, one would start seeingheavy elements processed during the QN. These linesshould look narrow since theQN ejecta is slowed down byinteraction with the preceedingSN ejecta …

The Photosphere

OCCURRENCE RATEOCCURRENCE RATE

Superluminous supernova are rare events: about 1 out of 1000 supernovae

Dual Shock quark novae are also estimated to occur for about 1 out of 1000 supernovae

Superluminous supernova are rare events: about 1 out of 1000 supernovae

Dual Shock quark novae are also estimated to occur for about 1 out of 1000 supernovae

Lead to Black Holes

Lead to Neutron Stars

Heavy NSs(QS candidates)

Follow-up talk by Jan Staff: implications to GRBs ……

z 123456789

?

?

0

HI

HII(Hydrogen

“fully” ionized)

Quark-Novae and

Reionization Era

Quark-Novae and

Reionization Era

From Avi Loeb

reionization

2 Key Constraints:1. WMAP: zstart= 20 (tau_e~0.11)2. WMAP: zend ~ 6

Fan et al. 2006

The Source(s) of reionizatio?

The Source(s) of reionizatio?

One is left with first stars!

One is left with first stars!

Loeb, Ostriker, Chiu, Fan, Venkatessan, Tegmark, Gnedini, Becker, Carilli, Ferrara, Gallerani, Jiang,

Richards, Choudhury, Strauss, Xu, Walter, White ect…

Pop III stars unlikely !

If GRBs are indeed quark-novae (see Staff’s talk)then

high-z GRBs should cluster around z~6-8

6 < z < 8

FIN …

or is it may be just … the beginning

FIN …

or is it may be just … the beginning

Dual-explosion

Takeaway message:

Photon-driven (instead of traditional neutrino-driven) explosions

Dual-explosions

vv

Neutrons

Target or seednuclei

(neutron star crust)

Collapsing core

r-process nucleo-synthesis

Light element (Ge, Ti) production by alpha-burning

Observations of Gamma-rays from 44Ti (half-life=90 years)could in principle confirm the Quark-Nova Scenario

44Ti

73Ge

79Se

195Pt132Xe U island

152Eu

R-process Elements from the Quark Nova

SpectrumSpectrum

2006gy

Ia

The Nature of the Beast

QN inside a SN

QN inside a SN

QN shock/chunks wave moves through entire

Supernova ejecta

SN ejecta becomes fully shocked by QN chunks

Shocks/chunks breakout

Hot SN ejecta cools slowly by adiabatic expansion