SN 2006gy – a point of discussion
Christina Hövel
09.06.2008
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
1 / 27
Supernova 2006gy
Huge luminosity (-22 mag)
Time of peak luminosity
(≈ 70 days)
Hydrogen in spectrum
Low expansion speed of ejecta
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
2 / 27
Contents
1
General features of Supernovae
1.1 Classification
1.2 Light Curve
1.3 Physical Mechanisms
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
3 / 27
Contents
1
General features of Supernovae
1.1 Classification
1.2 Light Curve
1.3 Physical Mechanisms
2
Explanations for SN2006gy
2.1 A runaway collision in a young star cluster
2.2 Pulsational pair instability Supernova
2.3 Other attempted explanations
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
3 / 27
Contents
1
General features of Supernovae
1.1 Classification
1.2 Light Curve
1.3 Physical Mechanisms
2
Explanations for SN2006gy
2.1 A runaway collision in a young star cluster
2.2 Pulsational pair instability Supernova
2.3 Other attempted explanations
3
Conclusion
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
3 / 27
General features of Supernovae
1.1 Classification
Contents
1
General features of Supernovae
1.1 Classification
1.2 Light Curve
1.3 Physical Mechanisms
2
Explanations for SN2006gy
2.1 A runaway collision in a young star cluster
2.2 Pulsational pair instability Supernova
2.3 Other attempted explanations
3
Conclusion
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
4 / 27
General features of Supernovae
1.1 Classification
Absorption spectra
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
5 / 27
General features of Supernovae
1.1 Classification
Absorption spectra
Type I
H - lines absent
Type Ia
deep Si II absorption line
strong blends of Fe emission lines (late time spectra)
Si II absorption line absent
He I absorption lines (early time spectra)
Si II absorption line absent
He I absorption line weak or absent
Type Ib
Type Ic
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
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General features of Supernovae
1.1 Classification
Absorption spectra
Type I
H - lines absent
Type Ia
deep Si II absorption line
strong blends of Fe emission lines (late time spectra)
Si II absorption line absent
He I absorption lines (early time spectra)
Si II absorption line absent
He I absorption line weak or absent
Type Ib
Type Ic
Type II
H - lines present
Type IIb
Type II-L
Type II-P
Type IIn
He - lines dominant
linear decrease in its light curve
plateau in its light curve
narrow emission lines ⇔ low expansion velocity
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
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General features of Supernovae
1.1 Classification
Classification of SN 2006gy
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
6 / 27
General features of Supernovae
1.1 Classification
Classification of SN 2006gy
Hα emission lines ⇒ Type II
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
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General features of Supernovae
1.1 Classification
Classification of SN 2006gy
Hα emission lines ⇒ Type II
absorption features that may be Si II lines at low expansion
velocity ⇒ Type Ia and Type IIn
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
6 / 27
General features of Supernovae
1.1 Classification
Classification of SN 2006gy
Hα emission lines ⇒ Type II
absorption features that may be Si II lines at low expansion
velocity ⇒ Type Ia and Type IIn
hybrid Type IIn/Ia SNe also known as Type IIa
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
6 / 27
General features of Supernovae
1.2 Light Curve
Light Curve
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
7 / 27
General features of Supernovae
1.2 Light Curve
Light Curve
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
7 / 27
General features of Supernovae
1.2 Light Curve
Light Curve
huge luminosity (-22 mag)
long time of peak luminosity (≈ 70 days).
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
7 / 27
General features of Supernovae
1.3 Physical Mechanisms
Physical Mechanisms
i) Core collapse supernova
possible progenitor: Mstar = 10 − 95Msun
possible SN Types: Ic/b IIb/L/P
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
8 / 27
General features of Supernovae
1.3 Physical Mechanisms
Physical Mechanisms
i) Core collapse supernova
possible progenitor: Mstar = 10 − 95Msun
possible SN Types: Ic/b IIb/L/P
ii) Pair (e − /e + ) instabillity supernova (PISN)
possible progenitor: Mstar = 130 − 260Msun ,
moderate metallicity,
low abundance of other elements than H & He
possible SN Types: IIa
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
8 / 27
General features of Supernovae
1.3 Physical Mechanisms
Physical Mechanisms
i) Core collapse supernova
possible progenitor: Mstar = 10 − 95Msun
possible SN Types: Ic/b IIb/L/P
ii) Pair (e − /e + ) instabillity supernova (PISN)
possible progenitor: Mstar = 130 − 260Msun ,
moderate metallicity,
low abundance of other elements than H & He
possible SN Types: IIa
iii) Thermonuclear supernova
possible progenitor: Binary System
possible SN Types: Ia
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
8 / 27
General features of Supernovae
1.3 Physical Mechanisms
i) Core collapse
onion-layered shells of
elements with an iron
core
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
9 / 27
General features of Supernovae
1.3 Physical Mechanisms
i) Core collapse
onion-layered shells of
elements with an iron
core
Christina Hövel
collapse over
Chandrasekhar-mass
SN 2006gy – a point of discussion
09. 06. 2008
9 / 27
General features of Supernovae
1.3 Physical Mechanisms
i) Core collapse
onion-layered shells of
elements with an iron
core
Christina Hövel
collapse over
Chandrasekhar-mass
SN 2006gy – a point of discussion
core is compressed into
neutrons
09. 06. 2008
9 / 27
General features of Supernovae
1.3 Physical Mechanisms
i) Core collapse
infalling material
bounces →
outward-propagating
shock front
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
10 / 27
General features of Supernovae
1.3 Physical Mechanisms
i) Core collapse
infalling material
bounces →
outward-propagating
shock front
Christina Hövel
shock front starts to
stall, but it is
reinvigorated by
neutrino interaction
SN 2006gy – a point of discussion
09. 06. 2008
10 / 27
General features of Supernovae
1.3 Physical Mechanisms
i) Core collapse
infalling material
bounces →
outward-propagating
shock front
Christina Hövel
shock front starts to
stall, but it is
reinvigorated by
neutrino interaction
SN 2006gy – a point of discussion
surrounding material is
blasted away →
degenerated remnant
09. 06. 2008
10 / 27
General features of Supernovae
1.3 Physical Mechanisms
ii) Pair instabillity
Preassure ⇔ Gravitation
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
11 / 27
General features of Supernovae
1.3 Physical Mechanisms
ii) Pair instabillity
collision between atomic
nuclei and energetic gamma
rays produces free electrons
and positrons
Preassure ⇔ Gravitation
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
11 / 27
General features of Supernovae
1.3 Physical Mechanisms
ii) Pair instabillity
collision between atomic
nuclei and energetic gamma
rays produces free electrons
and positrons
reduction of the thermal
pressure inside the core
Preassure ⇔ Gravitation
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
11 / 27
General features of Supernovae
1.3 Physical Mechanisms
ii) Pair instabillity
collision between atomic
nuclei and energetic gamma
rays produces free electrons
and positrons
reduction of the thermal
pressure inside the core
partial collapse
Preassure ⇔ Gravitation
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
11 / 27
General features of Supernovae
1.3 Physical Mechanisms
ii) Pair instabillity
collision between atomic
nuclei and energetic gamma
rays produces free electrons
and positrons
reduction of the thermal
pressure inside the core
partial collapse
accelerated burning
Preassure ⇔ Gravitation
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
11 / 27
General features of Supernovae
1.3 Physical Mechanisms
ii) Pair instabillity
Preassure ⇔ Gravitation
Christina Hövel
collision between atomic
nuclei and energetic gamma
rays produces free electrons
and positrons
reduction of the thermal
pressure inside the core
partial collapse
accelerated burning
runaway thermonuclear
explosion blows the star
completely apart
SN 2006gy – a point of discussion
09. 06. 2008
11 / 27
General features of Supernovae
1.3 Physical Mechanisms
iii) Thermonuclear supernova
binary
system
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
12 / 27
General features of Supernovae
1.3 Physical Mechanisms
iii) Thermonuclear supernova
binary
system
Christina Hövel
more
massive
→ giant
SN 2006gy – a point of discussion
09. 06. 2008
12 / 27
General features of Supernovae
1.3 Physical Mechanisms
iii) Thermonuclear supernova
binary
system
Christina Hövel
more
massive
→ giant
giant spills
gas onto
companion
SN 2006gy – a point of discussion
09. 06. 2008
12 / 27
General features of Supernovae
1.3 Physical Mechanisms
iii) Thermonuclear supernova
binary
system
Christina Hövel
more
massive
→ giant
giant spills
gas onto
companion
lighter star
and giant
core spiral
SN 2006gy – a point of discussion
09. 06. 2008
12 / 27
General features of Supernovae
1.3 Physical Mechanisms
iii) Thermonuclear supernova
binary
system
Christina Hövel
more
massive
→ giant
giant spills
gas onto
companion
lighter star
and giant
core spiral
SN 2006gy – a point of discussion
ejected
envelope,
separation
decreases
09. 06. 2008
12 / 27
General features of Supernovae
1.3 Physical Mechanisms
iii) Thermonuclear supernova
binary
system
more
massive
→ giant
giant spills
gas onto
companion
lighter star
and giant
core spiral
ejected
envelope,
separation
decreases
giant core
→ white
dwarf (wd)
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
12 / 27
General features of Supernovae
1.3 Physical Mechanisms
iii) Thermonuclear supernova
binary
system
giant core
→ white
dwarf (wd)
Christina Hövel
more
massive
→ giant
giant spills
gas onto
companion
lighter star
and giant
core spiral
ejected
envelope,
separation
decreases
companion
spills gas
onto wd
SN 2006gy – a point of discussion
09. 06. 2008
12 / 27
General features of Supernovae
1.3 Physical Mechanisms
iii) Thermonuclear supernova
binary
system
giant core
→ white
dwarf (wd)
Christina Hövel
more
massive
→ giant
giant spills
gas onto
companion
companion
spills gas
onto wd
lighter star
and giant
core spiral
ejected
envelope,
separation
decreases
wd reaches
crit. mass
& explodes
SN 2006gy – a point of discussion
09. 06. 2008
12 / 27
General features of Supernovae
1.3 Physical Mechanisms
iii) Thermonuclear supernova
binary
system
giant core
→ white
dwarf (wd)
Christina Hövel
more
massive
→ giant
giant spills
gas onto
companion
companion
spills gas
onto wd
lighter star
and giant
core spiral
wd reaches
crit. mass
& explodes
SN 2006gy – a point of discussion
ejected
envelope,
separation
decreases
ejects
companion
star
09. 06. 2008
12 / 27
Explanations for SN2006gy
2.1 A runaway collision in a young star cluster
Contents
1
General features of Supernovae
1.1 Classification
1.2 Light Curve
1.3 Physical Mechanisms
2
Explanations for SN2006gy
2.1 A runaway collision in a young star cluster
2.2 Pulsational pair instability Supernova
2.3 Other attempted explanations
3
Conclusion
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
13 / 27
Explanations for SN2006gy
2.1 A runaway collision in a young star cluster
Portegies Zwart et al.
Simon F. Portegies Zwart & Edward P. J. van Heuvel , A runaway collision
in a young star cluster as the origin of the brightest supernova, Nature
450, 388-389 (15.11.2007)
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
14 / 27
Explanations for SN2006gy
2.1 A runaway collision in a young star cluster
Portegies Zwart et al.
Simon F. Portegies Zwart & Edward P. J. van Heuvel , A runaway collision
in a young star cluster as the origin of the brightest supernova, Nature
450, 388-389 (15.11.2007)
Problem: Only a very massive star will end up in such a bright SN,
but Mstar ≥ 40Msun loses H-rich envelope hundred
thousands of years before the star explodes.
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
14 / 27
Explanations for SN2006gy
2.1 A runaway collision in a young star cluster
Portegies Zwart et al.
Simon F. Portegies Zwart & Edward P. J. van Heuvel , A runaway collision
in a young star cluster as the origin of the brightest supernova, Nature
450, 388-389 (15.11.2007)
Problem: Only a very massive star will end up in such a bright SN,
but Mstar ≥ 40Msun loses H-rich envelope hundred
thousands of years before the star explodes.
Explanation: 104 − 105 years before Supernova: Merger of
M1 ≥ 100Msun (H-depleted) and M2 ≥ 20 − 40Msun
(H-rich).
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
14 / 27
Explanations for SN2006gy
2.1 A runaway collision in a young star cluster
Portegies Zwart et al.
Simon F. Portegies Zwart & Edward P. J. van Heuvel , A runaway collision
in a young star cluster as the origin of the brightest supernova, Nature
450, 388-389 (15.11.2007)
Problem: Only a very massive star will end up in such a bright SN,
but Mstar ≥ 40Msun loses H-rich envelope hundred
thousands of years before the star explodes.
Explanation: 104 − 105 years before Supernova: Merger of
M1 ≥ 100Msun (H-depleted) and M2 ≥ 20 − 40Msun
(H-rich).
Verification: The collision frequency of massive stars in a dense and
young cluster is sufficient to provide a reasonable chance
for this scenario. (King model)
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
14 / 27
Explanations for SN2006gy
2.1 A runaway collision in a young star cluster
Results
Mass of the collision runaway star as a function of cluster mass and
its distance to the center of NGC 1260.
The most massive object that can form is 920Msun .
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
15 / 27
Explanations for SN2006gy
2.2 Pulsational pair instability Supernova
Woosley et al.
S. E. Woosley, S. Blinnikov & alexander Heger, Pulsational pair instability
as an explanation for the most luminous supernovae, Nature 450, 388-389
(15.11.2007)
Problem: Luminosity and H-lines.
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
16 / 27
Explanations for SN2006gy
2.2 Pulsational pair instability Supernova
Woosley et al.
S. E. Woosley, S. Blinnikov & alexander Heger, Pulsational pair instability
as an explanation for the most luminous supernovae, Nature 450, 388-389
(15.11.2007)
Problem: Luminosity and H-lines.
Explanation: The explosive burning of a PISN of a red supergiant is
inadequate to unbind the entire star and ejects only
many solar masses of surface material. Depending on the
temperature a second explosion can occur and the
ejected material can collide with the earlier ejecta. This
collision can radiate 1050 erg light, about a factor of ten
more than an ordinary SN.
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
16 / 27
Explanations for SN2006gy
2.2 Pulsational pair instability Supernova
Woosley et al.
S. E. Woosley, S. Blinnikov & alexander Heger, Pulsational pair instability
as an explanation for the most luminous supernovae, Nature 450, 388-389
(15.11.2007)
Problem: Luminosity and H-lines.
Explanation: The explosive burning of a PISN of a red supergiant is
inadequate to unbind the entire star and ejects only
many solar masses of surface material. Depending on the
temperature a second explosion can occur and the
ejected material can collide with the earlier ejecta. This
collision can radiate 1050 erg light, about a factor of ten
more than an ordinary SN.
Verification: Calculation of the evolution of a star of 110 solar
masses and solar composition. (Kepler code)
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
16 / 27
Explanations for SN2006gy
2.2 Pulsational pair instability Supernova
Results
The pre-supernova star
red supergiant
radius 1.6Rsun (Rsun = 695 700km)
luminosity 2.4 · 106 Lsun (Lsun = 4 · 1033 erg/s)
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
17 / 27
Explanations for SN2006gy
2.2 Pulsational pair instability Supernova
Results
The pre-supernova star
red supergiant
radius 1.6Rsun (Rsun = 695 700km)
luminosity 2.4 · 106 Lsun (Lsun = 4 · 1033 erg/s)
The first explosion
after burning He and C: T = 109 K ⇒ pair instability
He core collapses T = 3 · 109 K
the star explodes, burning 1.4Msun O & 1.6Msun C
releasing 1051 erg
10% goes into driving off 25Msun (He & some H)
speed 100 − 1000km s −1 , luminosity 108 Lsun for 200 days
Mremnant = 50Msun
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
17 / 27
Explanations for SN2006gy
2.2 Pulsational pair instability Supernova
Results
Cumulative light curve for the 110-solar-mass model
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
18 / 27
Explanations for SN2006gy
2.2 Pulsational pair instability Supernova
Results
6.8 years after the first explosion
the second explosion
stronger pulse from pair instability (1017 Lsun )
smaller ejected mass (5Msun )
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
19 / 27
Explanations for SN2006gy
2.2 Pulsational pair instability Supernova
Results
The first explosion
luminosity 108 Lsun
ejected mass 25Msun
6.8 years after the first explosion
the second explosion
stronger pulse from pair instability (1017 Lsun )
smaller ejected mass (5Msun )
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
19 / 27
Explanations for SN2006gy
2.2 Pulsational pair instability Supernova
Results
6.8 years after the first explosion
the second explosion
stronger pulse from pair instability (1017 Lsun )
smaller ejected mass (5Msun )
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
19 / 27
Explanations for SN2006gy
2.2 Pulsational pair instability Supernova
Results
6.8 years after the first explosion
the second explosion
stronger pulse from pair instability (1017 Lsun )
smaller ejected mass (5Msun )
6.9 years after the first explosion
the collision takes place
radiates 1050 erg of light
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
19 / 27
Explanations for SN2006gy
2.2 Pulsational pair instability Supernova
Results
6.8 years after the first explosion
the second explosion
stronger pulse from pair instability (1017 Lsun )
smaller ejected mass (5Msun )
6.9 years after the first explosion
the collision takes place
radiates 1050 erg of light
9 years after the first explosion
the remnant forms a M = 2.2Msun iron core
the core collapses into a rapidly rotating
neutron star or black hole
maybe a third bright event (gamma-ray burst)
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
19 / 27
Explanations for SN2006gy
2.2 Pulsational pair instability Supernova
Velocity structure
The collision between the first and second outburst starts at 1015 cm
(67AU).
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
20 / 27
Explanations for SN2006gy
2.2 Pulsational pair instability Supernova
Absolute R-band magnitudes
(calculated by using the radiation-hydrodynamics code Stella)
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
21 / 27
Explanations for SN2006gy
2.3 Other attempted explanations
Other attempted explanations
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
22 / 27
Explanations for SN2006gy
2.3 Other attempted explanations
Other attempted explanations
Ia SN
white dwarf merger
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
22 / 27
Explanations for SN2006gy
2.3 Other attempted explanations
Other attempted explanations
Ia SN
white dwarf merger
Birth of a quark star
progenitor: a massive star which collapses to become a
neutron star
magnetic properties cause their spin rates
to a drastical slow down
centrifugal force can no longer support the neutron
star’s core
the core collapses transforming into strange matter
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
22 / 27
Explanations for SN2006gy
2.3 Other attempted explanations
Other attempted explanations
Ia SN
white dwarf merger
Birth of a quark star
progenitor: a massive star which collapses to become a
neutron star
magnetic properties cause their spin rates
to a drastical slow down
centrifugal force can no longer support the neutron
star’s core
the core collapses transforming into strange matter
...
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
22 / 27
Conclusion
Contents
1
General features of Supernovae
1.1 Classification
1.2 Light Curve
1.3 Physical Mechanisms
2
Explanations for SN2006gy
2.1 A runaway collision in a young star cluster
2.2 Pulsational pair instability Supernova
2.3 Other attempted explanations
3
Conclusion
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
23 / 27
Conclusion
What is SN 2006gy not?
No late time observations of a young star cluster, but the
existence of young star clusters beeing in a state of dynamical
core collapse is crucial for the runaway collision scenario
(Portegies Zwart et al.).
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
24 / 27
Conclusion
What is SN 2006gy not?
No late time observations of a young star cluster, but the
existence of young star clusters beeing in a state of dynamical
core collapse is crucial for the runaway collision scenario
(Portegies Zwart et al.).
The calculation of white dwarf mergers suggests that such
catastrophic event would would lead to the creation of a black
hole or a neutron star rather than a type Ia supernova.
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
24 / 27
Conclusion
What is SN 2006gy not?
No late time observations of a young star cluster, but the
existence of young star clusters beeing in a state of dynamical
core collapse is crucial for the runaway collision scenario
(Portegies Zwart et al.).
The calculation of white dwarf mergers suggests that such
catastrophic event would would lead to the creation of a black
hole or a neutron star rather than a type Ia supernova.
The quark nova explanation is a really exotic model.
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
24 / 27
Conclusion
What is SN 2006gy not?
No late time observations of a young star cluster, but the
existence of young star clusters beeing in a state of dynamical
core collapse is crucial for the runaway collision scenario
(Portegies Zwart et al.).
The calculation of white dwarf mergers suggests that such
catastrophic event would would lead to the creation of a black
hole or a neutron star rather than a type Ia supernova.
The quark nova explanation is a really exotic model.
⇒ We probably have a pulsational pair instability Supernova
(Woosley et al.)
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
24 / 27
Conclusion
Late time observations
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
25 / 27
Conclusion
Late time observations
⇒ Late time observations do not solve the problem and they cause
new mysteries.
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
25 / 27
Sources
Sources
Woosley, S. E., Blinnikov, S., & Heger, A. 2007, Nature, 450, 390
Portegies Zwart, S. F., & van den Heuvel, E. P. J. 2007, Nature, 450,
388
Smith, N., et al. 2008, ArXiv e-prints, 802, arXiv:0802.1743
Smith, N., et al. 2007, Astrophysical Journal, 666, 1116
New Scientist Space Shiga, D. 03.01.2007, Brightest supernova
disvovery hints at stellar collision
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
26 / 27
Sources
Sources - Images
Core collapse illustration after Modelling Supernovae with
PHOENIX - Author R.J. Hall
PISN ilustration: NASA/CXC/ M. Weiss http://
chandra.harvard.edu/ photo/ 2007/ sn2006gy/ sn2006gy_ill.tif
Thermonuclear SN illustration: Nasa, www.hubblesite.org
Christina Hövel
SN 2006gy – a point of discussion
09. 06. 2008
27 / 27