Non-Hydrogen Windy Models
for Superluminous Supernovae

Elena Sorokina1 , Sergei Blinnikov2
1

Sternberg Astronomical Institute, Moscow State University, Moscow
2

Institute for Theoretical and Experimental Physics, Moscow

SN-GRB workshop – YITP, Kyoto University – 23 Oct. 2013 – p. 1

Extremely bright Type IIn SNe

V-band(Drake et al.
2010)

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Extremely bright Type IIn SNe

V-band (Drake et al. 2010)
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Extremely bright Type Ic SNe

R-band light curves (Young et al. 2010)-21-2056

Co

Absolute magnitude-19to 56
Fe1994I
1997ef
1998bw
2002ap2003jd2007bg
2007bi-21-20-18-19-17-16-18-15-17-14-13-16
050

100

150

200

250

300

350

-200204060

Epoch (days)

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Observations of the superluminous
SNe

Absolute u−band AB magnitude

Quimby et al. 2011
SCP 06F6
SN 2005ap
PTF09cnd
PTF09cwl
PTF09atu
PTF10cwr−22−20−18−16SS SS−50050
100
Rest−frame phase (days)

150SN-GRB workshop – YITP, Kyoto University – 23 Oct. 2013 – p. 5

More exotic case – High-z SNe

z = 2.05

z = 3.9

Cooke+ 2012

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Very bright Type Ib SNe with narrow
lines
43.5
43
42.5

Type Ibn

42
41.5
41

Quasi-bolometric(optical+NIR)(Pastorello et al.
2008)

40.5
40
SN 2006jc Ibn (opt+NIR)
39.5

SN 2006jc Ibn (opt)
SN 1998bw Ic-hyp

39
38.5
38-20

SN 2006aj Ic-hyp
SN 2002ap Ic-pec
SN 1999dn Ib-nor
SN 1999E IIn

020406080100120140160180200

days from maximum

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Very bright Type Ib SNe with narrowlines

Pastorello et al. 2008
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Possible models for SLSNe•

Pair instability SNe•

Magnetar energy pumping•

Interaction with CSM

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PISN vs. magnetar model
One of the latest and the brightest SLSN PTF 12dam(Nickoll+, Nature, 2013)

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Windy model for core collapse SNe

Ofek et al. 2010
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Windy models for type Ib/c SNeEjecta: polytropic mass distribution
Parameters: Mej , Rej .
Wind: power-law mass distribution ρ ∼ r−p
Parameters: Mw , Rw , p(only 2 of them are independent).
For the nearest future: detouched envelope
Composition: uniform for most of models;
mostly CO in different ratio + 2% of metals;
a few He models;
no 56 Ni in most of models;
CSM velocity: mostly u = 0 or linear increase with R
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Initial models
Samples of the density distribution

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Initial models
Samples of the density distribution

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Code STELLA• time-dependent equations for the angularmoments of intensity (coupled to hydro equations)in fixed frequency bins are solved implicitly

SN-GRB workshop – YITP, Kyoto University – 23 Oct. 2013 – p. 15Code STELLA• time-dependent equations for the angularmoments of intensity (coupled to hydro equations)in fixed frequency bins are solved implicitly• no need to ascribe any temperature to theradiation: the photon energy distribution may bequite arbitrary

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Code STELLA• time-dependent equations for the angularmoments of intensity (coupled to hydro equations)in fixed frequency bins are solved implicitly• no need to ascribe any temperature to theradiation: the photon energy distribution may bequite arbitrary• up to ∼ 400 zones for the Lagrangean coordinate

and up to 200 frequency bins are used

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Code STELLA• heating by decays of 56 Ni → 56 Co → 56 Fe with theγ -ray transfer in a one-group approximation

following Swartz et al. 1995 (with purely absorptiveopacity in the gamma-ray range)

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Code STELLA• heating by decays of 56 Ni → 56 Co → 56 Fe with theγ -ray transfer in a one-group approximation

following Swartz et al. 1995 (with purely absorptive
opacity in the gamma-ray range)• Local Thermodynamic Equilibrium (LTE) for

ionization and atomic level populations is assumed(but radiation is nonequilibrium)

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Code STELLA• heating by decays of 56 Ni → 56 Co → 56 Fe with theγ -ray transfer in a one-group approximation

following Swartz et al. 1995 (with purely absorptive
opacity in the gamma-ray range)• Local Thermodynamic Equilibrium (LTE) for

ionization and atomic level populations is assumed(but radiation is nonequilibrium)• the effect of line opacity is treated as an expansion

opacity according to Eastman & Pinto 1993 (andour new recipes).

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Light curves for different explosion
energies

p = 1.8, Mw = 4.8M⊙

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Different Mej
0.2 Msun and 12.8 Msun

More massive - dimmer and wider
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Different Mej
3.2 Msun and 12.8 Msun

More massive - dimmer and wider
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Light curves
for different wind structurep = 2.5, Mw = 2.9M⊙

p = 2, Mw = 3.5M⊙

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Light curves for different E and ρ(r)out10: Mej = 2M⊙ , pw = 2, E = 3 Bethe
out26: Mej = 0.2M⊙ , pw = 1.8, E = 2 Bethe
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56

Ni vs. Shock wave heating

no 56 Ni
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56

Ni vs. Shock wave heating

M (56 Ni) = 1M⊙ in the ejecta
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56

Ni vs. Shock wave heating

M (56 Ni) = 1M⊙ added to the ejecta
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Metallicity

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Different C/O ratio

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CO vs. He wind

CO wind
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CO vs. He wind

Model with He-wind is more symmetric aroundmaximum light
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CO vs. He wind

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Difficulties in the windy models
Very thin layer contains almost all mass

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Best models for SN 2010gx

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Uncertainty in expansion opacity

Opacity is taken as for dv/dr = 1/t = 1/1day

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Model vs. observations

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BUT

What does it mean
“BOLOMETRIC” forcosmological SNe, when
spectra are redshifted?
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What is bolometric?

SN-GRB workshop – YITP, Kyoto University – 23 Oct. 2013 – p. 35What is bolometric?

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What is bolometric?

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What is bolometric?

Chomiuk et al. 2009

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What is bolometric?

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Conclusions• The shock wave which runs through rather dense

matter surrounding an exploding star can produce
enough light to explain very luminous SN events.
No 56 Ni is needed in this case to explain the light
curve near maximum light (some amount is ofcourse needed to explain light curve tails).
We need the explosion energy of only 2-3 Bethe
for the shell with M = 3 − 5M⊙ and R < 1016 cm.
The brightness and the duration of the light curve
maximum strongly depends on the mass andstructure of the envelope.

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Conclusions• Questions on the latest phases of star evolution

arise:• Is it possible to form so big and denseenvelopes? And how?
• Time scale for such a formation• How far can the envelope extend?
• Density and temperature profiles inside theenvelope right before the explosion• Question to observetions: try to find traces of suchshells for bright explosions.
(There are spectral evidence of circumstellar
shells for type IIn and Ibn SNe. Is it possible to findC–O envelopes as well?)

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Conclusions• Many technical problems in light curve

calculations:• line opacities;• dimensionality: 3D is preferable, since theenvelope can most probably be clumpy;• NLTE spectra

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