dietrich baade (eso) peter hoeflich (fsu) ferdinando patat (eso) lifan wang (lbnl)
DESCRIPTION
The Best SN of 2005?. Dietrich Baade (ESO) Peter Hoeflich (FSU) Ferdinando Patat (ESO) Lifan Wang (LBNL) J. Craig Wheeler (Austin). SN 1006 at Discovery – Historical Image from Song Dynasty. SN 2005df. UV – Swift Optical photometry and spectropolarimetry Mid-IR - PowerPoint PPT PresentationTRANSCRIPT
Dietrich Baade (ESO)Peter Hoeflich (FSU)Ferdinando Patat (ESO)Lifan Wang (LBNL)J. Craig Wheeler (Austin)
The Best SN of 2005?
SN 2005df
• UV – Swift• Optical photometry and spectropolarimetry• Mid-IR
• Structure of the ejecta
Optical Light Curves
Si II line atV~25000 km/sec
Fine structuresare found
Polarizationis strong At blue shiftedabsorptionfeatures
-12
-09
+09
+08
+05
+00
-03
-07
-08
+04
OI CaII
Ca
Example 3: SN 2004dt
A high velocity SN Distorted envelope
HVS NVC
Wavelength
Rel
. Flu
x
SN 2004dt - IME only
Wang et al. 2004
Line/Polarization Profiles
Peak blueshifted by 4000 km/sec
SN 2006X
HVS
NVC
HVS
NVC
O I of SN 2006X
Example 2: SN 2001el
Detached Ca Shell/Clump/RingDay -4 Day 19
SN 2001el
Si II Ca IIDay -4 Day 19 Day -4 Day 19
-2X104 0 2X104
Velocity(km/sec)
-2X104 0 2X104
Velocity(km/sec) -2X104 0 -2X104 0 Velocity(km/sec) Velocity(km/sec)
Q-U diagram for axially symmetric geometry
V1V3
V2
Q
U
Principle axis
V4
Q = (I0-I90)/(I0+I90)U = (I45-I135)/(I45+I135)Theorem: For axially symmetric geometry, the Q-U vectors
form a straight line on the Q-U Diagram
Pf=N1/2p0fi
Brownian Motion
f - total area covering factor of clumps (≤1)fi - area covering factor by a typical clump (~f/N)N - total number of clumps (=f/fi)pifi - polarized flux due to individual clump (~3f i%) P ≈ f N~1/23%/(1-f) ~ 0.5%, N ~ 36 for f ~ 0.5, fi~f/N=0.014dc- diameter of a typical clump ~ 2,400 km/sec
∑pifi fiN1/2 fN-1/2
P = ———— ~ ——p0 = —— p0 1-∑fi 1-f 1-f
Pf=N1/2p0fi
Brownian Motion1) When N is sufficiently large P will be a stable vector that does not show big, random fluctuations with time.
2) In the case of a small number of large clumps, P is again a stable quantity as such clumps will shield the photosphere at all epochs
These vectors/clumpsmoved outside the surfaceof the photosphere at a later epoch.
Polarization position angles: A corkscrew in the ejecta?
U
Q
v1
Q
U
v4
Q
U
v3
Q
U
v2
Polarization position angles: corkscrews in the ejecta?
U
QQLoops/arcs on Q-U diagram
Absorbing clumps at different velocity
In velocity space,the radial elongation of the clumps determines the correlation of theobserved polarization at different velocities.
10,0
00 k
m/s
ec
15,0
00 k
m/s
ec
20,0
00 k
m/s
ec
Each velocity layerintercepts ~16 clumpsif the volume in frontof the photosphereis packed with clumpsof diameter of 5,000 km/sec
The volume in front of thephotosphere is big enoughto hold about 48 clumps of diameter ~5,000 km/secThe radial extension
of typical clumps has tobe ~ 5,000 km/sec toexplain the observedpolarization profile.
Peak blueshifted by 4000 km/sec
Si II 3859 Si II 6355
Mg II 4481
O I 7773
SN 2001elSi II Ca II
Day -4 Day 19 Day -4 Day 19
-2X104 0 2X104
Velocity(km/sec)
-2X104 0 2X104
Velocity(km/sec) -2X104 0 -2X104 0 Velocity(km/sec) Velocity(km/sec)
SN 2005df
08/06/200508/08/200508/09/2005
08/10/200508/14/200508/17/200508/21/200508/22/2005
08/25/200508/26/2005
Chemical Structure
Correlation
Correlation
Summary
1. High velocity component is always asymmetric2. The normal velocity component is symmetric, to a level below 5%3. The chemical burning is different for HV and NV events
1) The HV probably burned C to oxygen2) The NV did not burn C at the outer layer (this is why C is found only in some NV)
4. The core is likely asymmetric
Mid-IR
Mid-IR
Mid-IR – Day 135
SN 2003hv – Day 375
Deflagration Delayed Detonation
Observed
Turbulent/clumpy geometry at all velocities
Significantly reduced asymmetry at the central part of the ejecta
No significant asymmetry below photosphere
Clumpy chemical Layered chemical structure layeredLow energy Sufficient energy High speed layer? The seed for significant asymmetry
At the outermost layer, the turbulent plumes/bubbles generated during the deflagration may survive
Asymmetry in 1) pre-expansion2) Progenitor3) Rotation; magnetic field
No high velocity shell
No high velocity shell High velocity shell withstrong asymmetry
Comparable level of asymmetry at all velocities
Stronger asymmetry at outer layers
1) Asymmetry decreases from 30000 – 8000 km/sec;2) The core is likely asymmetric