Models of SNe IIn for cosmology:
problems to solve
S.Blinnikov
Sergei.Blinnikov@itep.ru

ITEP, SAI

Kyoto, 31Oct13-Prosp – p. 1

Kyoto, 31st of October 2013
S.I.Blinnikov 1,2
1 Institute for Theoretical andExperimental Physics (ITEP),
Moscow

2 Sternberg AstronomicalInstitute (SAI), Moscow

Kyoto, 31Oct13-Prosp – p. 2

Sources
Work on SN light curves with E.Sorokina, P.Baklanov,
M.Potashov, A.Tolstov, A.Dolgov, K.Nomoto,
N.Tominaga, M.Tanaka, T.Moriya, Y.Kamiya
Observations of SN2006gy, 2009ip, 2010jl...
Theory of SNIIn (Nadyozhin,Grasberg,Chugai,SB,Woosley,Heger...)Recent papers: Blinnikov e’a 2012, Baklanov e’a 2013
(JETPL), Potashov e’a 2013 (MNRAS)

Kyoto, 31Oct13-Prosp – p. 3

SNe as distance indicators
Nobel prize in physics 2011
"for the discovery of theaccelerating expansion of theUniverse through observations ofdistant supernovae"
S.Perlmutter

A.Riess

SecondarySNe IaB.Schmidt

Kyoto, 31Oct13-Prosp – p. 4

Nobel prize in physics 2011
Actually, neither acceleration, nor theexpansion itself of the Universe aredirectly observable!
This is hard because decades of accurate−9observations are ∼ 10

the age of theUniverse. Accuracy of observations for
distances and angles in large scale ismuch much worse.
Kyoto, 31Oct13-Prosp – p. 5

What is measured: distance and redshift
Photometric distance:
d2ph =L(emitted, ergs/s)
4πF (observed, ergs/s/cm2 )Dependence on redshift z
dph (z)(Ωm , ΩDE , w(z))|theory

is determined by cosmology.
Comparison withdph (z)(observed)

allows one to find Ωm , ΩDE , w(z), etc.
There are models without expansion producing similar relations, e.g. Wetterich,arXiv:1303.6878
Kyoto, 31Oct13-Prosp – p. 6

Distance indicators
Primary

SecondarySNe IIPSNe IaKyoto, 31Oct13-Prosp – p. 7

Distance Ladder

Kyoto, 31Oct13-Prosp – p. 8

Distance Ladder - 1Kyoto, 31Oct13-Prosp – p. 9

Distance Ladder - 2

Kyoto, 31Oct13-Prosp – p. 10

Distance indicators
Primary

SN 1999em LC
Plateau phase

SNe IIP
V. Utrobin A&A461, 233 (2007)

Kyoto, 31Oct13-Prosp – p. 11

Distance indicators
Primary

SecondarySNe IIPSNe IaExpanding photosphere method (EPM)
R. P. Kirshner and J. Kwan, Astrophys. J.
193, 27 (1974)
Kyoto, 31Oct13-Prosp – p. 12

Expanding Photosphere Method (EPM)
Cf. Baade(1926)-Wesselink(1946) method for Cepheids .
Measuring color and flux at two different times, t1 and t2 ,one finds the ratio of the star’s radii, R2 /R1 (or frominterferometry).
Using weak lines which are believed to be formed near thephotosphere one can measure the photospheric speed vph .
R t2
Then t1 vph dt would give ∆Rph = R2 − R1 .
Knowing R2 /R1 and R2 − R1 , it is easy to solve for theradii. The ratio of fluxes gives
D2R2=Fν (emitted)
Fν (observed),hence the distance D.
Kyoto, 31Oct13-Prosp – p. 13

Problems with BW
But this idea does not work for supernovae(as a rule)!
Velocity of matter at the photosphere vph isnot at all Ṙph ≡ dRph/dt.
Velocity vph and Ṙph may even have
opposite signs!

Kyoto, 31Oct13-Prosp – p. 14

Kirshner & Kwan, 1974
The main idea of EPM for SNe is different from BW!
(Kirshner & Kwan were the first to point this out.)

Using weak lines one can measure thematter velocity on photospheric level, vph,
and then one finds,
Rph = vpht .
This is based on the assumption of free expansion,v = r/t ∝ r ,– like a Hubble law. Velocity is not assumed to be dRph /dt.
Kyoto, 31Oct13-Prosp – p. 15

Distance from EPM
Now the distance D to the supernova issFν (model)
D = RphFν (observed)
if a reliable model flux Fν (model) at theSN photosphere is compared with thedetected flux Fν (observed).

Kyoto, 31Oct13-Prosp – p. 16

Great Success of EPM
B.Schmidt et al.(1994), R.Eastmanet al.(1996) found H0 = 73 ± 6
based on EPM for a set of SNe II.

Kyoto, 31Oct13-Prosp – p. 17

Distance indicators
Primary

SecondarySNe IIPSNe IaEPM
Spectral-fitting expanding
atmosphere method (SEAM)
E. Baron, et al. Astrophys. J. Lett. 616, L91 (2004)
Kyoto, 31Oct13-Prosp – p. 18

Distance indicators
Primary

SecondarySNe IIPSNe IaEPMSEAMr
Free expansion v =is assumed!
tKyoto, 31Oct13-Prosp – p. 19Distance indicators
Primary

SNe IIP

EPM

SecondarySNe IInSNe IaSEAM

Kyoto, 31Oct13-Prosp – p. 20

Distance indicators
Primary

SNe IIP

SecondarySNe IInSNe IaDense Shell Method (DSM)
No free expansion, back to Baade!
S. Blinnikov, et al. JETP Letters 96, 153 (2012); M. Potashov, et al. MNRAS 431, 98 (2013)

Kyoto, 31Oct13-Prosp – p. 21

Why we need this?
Nick Suntzeff:

Forget it, when using SNe Ia. Othertools may help.
Kyoto, 31Oct13-Prosp – p. 22

SN Light Curves A.Filippenko in ARAA

Kyoto, 31Oct13-Prosp – p. 23

Most Luminous SNe N.Smith ea’07

Kyoto, 31Oct13-Prosp – p. 24

Extremely luminous Type IIn SNeV-band(Drake et al. 2010)

Kyoto, 31Oct13-Prosp – p. 25

SN 2006gy, type IIn
Ofek et al.
2007, ApJL,astroph/0612408)
Smith et al.
2007, Sep. 10
ApJ, astroph/0612617)

Kyoto, 31Oct13-Prosp – p. 26

Smith et al. SN 2006gy, Hα profile

Narrow component ∼ 200 km/s, wide ∼ 5000 km/s.
Kyoto, 31Oct13-Prosp – p. 27

SN IIn structure, Chugai, SB ea’04(photosphere)

Kyoto, 31Oct13-Prosp – p. 28

Two mass ejections Woosley e’a 2007

Kyoto, 31Oct13-Prosp – p. 29

Double explosion: old idea
Grasberg & Nadyozhin (1986)

Kyoto, 31Oct13-Prosp – p. 30

Light curve for SN2006gy
from Woosley, SB, Heger (2007)

Kyoto, 31Oct13-Prosp – p. 31

Smith,Chornock ea cartoon, 06tf

Kyoto, 31Oct13-Prosp – p. 32

Cold Dense Shell

Kyoto, 31Oct13-Prosp – p. 33

Long Living Dense shells-1

Sorokina et al.

See Poster 16Kyoto, 31Oct13-Prosp – p. 34

Long Living Dense shells-2

Sorokina et al.

See Poster 16
Kyoto, 31Oct13-Prosp – p. 35

Long Living Dense shells-3

Sorokina et al.

See Poster 16
Kyoto, 31Oct13-Prosp – p. 36

Long Living Dense shells-4

Sorokina et al.

See Poster 16
Kyoto, 31Oct13-Prosp – p. 37

Shocks in SNe IIn
Alongliving
shock:
anexample
for
SN1994wof type
IIn.
Density as afunction of theradiusrin
two models atday 30.
Thestructure tends
to an isothermal
shock wave.

Where are forward and reverese shocks?
Kyoto, 31Oct13-Prosp – p. 38

SN06gy Hydro structure 120 d

X-rays from the shock cannot go out yet, the matter is too dense.

Kyoto, 31Oct13-Prosp – p. 39

SN06gy 120 d, mass coordinate

Kyoto, 31Oct13-Prosp – p. 40

Observed L, T, R(t) of SN2006gy

Kyoto, 31Oct13-Prosp – p. 41

‘Visible’ disk of SN 2006gy

Kyoto, 31Oct13-Prosp – p. 42

New DSM for SNe IIn
Measure narrow line components to estimate theproperties of CS envelope (may be done crudely).
Measure wide line components to find the photosphericspeed vph (as accurately as possible).
Build a best fitting model for broad band photometryand the speed vph .

Kyoto, 31Oct13-Prosp – p. 43

New DSM for SNe IIn
Although the “Hubble”-law v = r/t is not applicable,
vph now measures true velocity of the photosphericradius (not only the matter flow speed, as in type II-P).
Now the original Baade’s idea works for measuring theradius by integrating vph (of course, with due accountof scattering, limb darkening/brightnening etc in atime-dependent spectral modeling of emerging light).
This must be used when iterating the best fitting model.
The observed flux then gives the distance.

Kyoto, 31Oct13-Prosp – p. 44

Dense Shell Method, DSM

dR = vphdt
R0 = Initial shell radius, unknown!
Ri ≡ R0 + ∆Ri
i = 1, 2, 3 . . .
Kyoto, 31Oct13-Prosp – p. 45

Dense Shell Method, DSM
pp
0.2Aν
D Fνi
ζνi(R0 + ∆Ri) πBν (Tνi ) = 10
Model: ζνi – correction factor

Observations+model: Tνi , ∆Ri
Observations: Fνi, Aν – extinction
All quantities are defined for the frequency ν.

And finally, D is the sought-for distance tothe star.
Kyoto, 31Oct13-Prosp – p. 46

‘Visible’ disk of SN 2006gy for ζKyoto, 31Oct13-Prosp – p. 47

MC probable D to SN 2006gy

Kyoto, 31Oct13-Prosp – p. 48

D to SN 2006gy+19
D ≈ 68−15 (68% CL) Mpc

Large error due touncertainty in extinction

Kyoto, 31Oct13-Prosp – p. 49

A better example of SN 2009ip– almost no extinction.
Real explosion September 2012
Kyoto, 31Oct13-Prosp – p. 50

D to SN 2006gy and SN 2009ip+19
D ≈ 68−15 (68% CL) Mpc

for SN 2006gy
Standard value around 71 Mpc

D ≈ 20.1 ± 0.8 (68% CL) Mpc
for SN 2009ip
Standard value around 20.4 Mpc
Kyoto, 31Oct13-Prosp – p. 51

Hubble parameter
SN 2006gy gives+23
H0 ≈ 79−17 km/s/Mpc.

Recent SNIa result
A. Riess, et al. ApJ 730, 119 (2011)

H0 ≈ 73 ± 2.4 km/s/Mpc.
Latest PLANCK value
H0 ≈ 67.3 ± 1.2 km/s/Mpc.
Kyoto, 31Oct13-Prosp – p. 52

Problems to Solve

Extracting vph from spectra
NLTE effects
Multi-D

Kyoto, 31Oct13-Prosp – p. 53

Extracting vph from spectra
Observed lines of SN2006gy

Care of widewings
duetoscattering(Chugai;Dessart&Hillier)

Kyoto, 31Oct13-Prosp – p. 54

NLTE effects Baklanov et al. 2013
Evolution of model sn09ipbp3 inLTE

Using
approach similar
to Lucy, Mazzali,
Sim...,
but for hydrosimulations

Kyoto, 31Oct13-Prosp – p. 55

LTE(solid) vs Non-LTE(dashed)

Kyoto, 31Oct13-Prosp – p. 56

Next step will be Multi-D
in theoretical modeling

Kyoto, 31Oct13-Prosp – p. 57

Multi-D
Chevalier & Blondin 1995
We
begin
with
our open source
code
FRONT3D
dau.itep.ru/sn(Semyon Glazyrin)
andadopting
SHDOM
radiativetransfer(NozomuTominaga)

Kyoto, 31Oct13-Prosp – p. 58

A. J. van Marle et al. MN 2010

23 days
Kyoto, 31Oct13-Prosp – p. 59

A. J. van Marle et al. MN 201087 days
Kyoto, 31Oct13-Prosp – p. 60

Conclusions
EPM is based not on Baade-Wesselink, but on
Kirshner-Kwan (KK) idea
Radiating shocks are most probable sources of light inmost luminous supernovae of type IIn like SN2006gy
Most luminous SN IIn events may be observed at high z[for years due to (1 + z)] and may be useful as direct,primary, distance indicators in cosmology
The new DSM is based on original Baade idea whichreally works now
The shock model requires NLTE and multi-D
development
Accurate observations of spectra must be used
together with detailed models to extract velocities
Kyoto, 31Oct13-Prosp – p. 61