Transcript 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.

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
Part II: Jan Staff
Part III: Brian Niebergal
R. Ouyed (U. Calgary)
Type II Supernovae
(Core-collapse
Supernovae)
Mass > 8 Msun
Core-Collapse
Supernovae
Hydrogen present when they explode!
Mass-shedding
Stars
Black Holes
Neutron Stars
White Dwarfs
May or may not have
hydrogen when they explode!
Energy release
GRAVITY → RADIATION !!!
NS
1%
Grav. Energy
(1053
erg)
1%
Kinetic Energy
(1051
ergs)
Radiation (1049 ergs)
The
Quark-Nova
Compact 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
Lead to Black Holes
Lead to Neutron Stars
Heavy NSs
(HS candidates)
Neutron star to Quark star Transition
The QUARK-NOVA !
The quark matter
core becomes
unstable and
shrinks faster
than
the envelope
response time!
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
Quark Nova
and
Super-luminous Supernovae
"This was a truly monstrous explosion,
a hundred times more energetic than a typical supernova,"
1051 ergs in Radiation !
100 times a normal Supernova !
3 Possible Mechanisms
(1) interaction of the supernova
Need too much surrounding blast wave with circumstellar
Ejecta !
material (CSM)
Need too much Nicke !
(2) energy from radioactive
decay of 56Ni
(3) Oscillating PISN
Very massive progenitor !
Artificial energy input!
Standard picture stretched to the extreme !
Ekinetic = 6.4x1052 erg; Mejecta = 53Msun; M(Ni+CO) = 15Msun
Neutron
Star
What does the
Quark-Nova
has to offer
in this context?
Dual
Explosion!
Quark
Star
QuarkNova
Ejecta
Application
SN2006gy
Mejec = 40Msun
Rstar = 10 Rsun
2000 < VSN (km/s) < 4800
tdelay = 15 days
Light-Curves of
SN2005gj
and
SN2005ap
Keep same parameters
as for SN2006gy except
SN2005gj
tdelay = 10 days
SN2005ap
tdelay = 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 receeds
deeper, one would start seeing
heavy elements processed
during the QN. These lines
should look narrow since the
QN ejecta is slowed down by
interaction with the preceeding
SN ejecta …
The Photosphere
OCCURRENCE RATE
Lead to Black Holes
Lead to Neutron Stars
Heavy NSs
(QS candidates)
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
Follow-up talk by Jan Staff: implications to GRBs ……
Quark-Novae
and
Reionization Era
?
HII
(Hydrogen
“fully” ionized)
?
HI
z
9
8
7
6
5
4
3
2
1
0
reionization
The
Source(s) of
reionizatio?
Fan et al. 2006
2 Key Constraints:
1. WMAP: zstart= 20 (tau_e~0.11)
2. WMAP: zend ~ 6
From Avi Loeb
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 !
6<z<8
If GRBs are indeed quark-novae (see Staff’s talk)
then
high-z GRBs should cluster around z~6-8
FIN …
or is it may be
just … the beginning
FIN …
or is it may be
just … the beginning
Takeaway message:
Photon-driven (instead of traditional neutrino-driven) explosions
Dual-explosions
Dual-explosion
Target or seed
nuclei
(neutron star crust)
v
Neutrons
r-process nucleo-synthesis
Collapsing
core
R-process Elements from the Quark Nova
Light element (Ge, Ti) production by alpha-burning
132Xe
44Ti 79Se
195Pt
U island
152Eu
73Ge
Observations of Gamma-rays from 44Ti (half-life=90 years
could in principle confirm the Quark-Nova Scenario
The Nature of the Beast
Spectrum
2006gy
Ia
QN inside
a SN
Hot SN ejecta cools slowly
by adiabatic expansion
QN shock/chunks wave
moves through entire
Supernova ejecta
SN ejecta becomes fully
shocked by QN chunks
Shocks/chunks breakout