long-grbs and hypernovae
DESCRIPTION
Long-GRBs and Hypernovae. Paolo A. Mazzali Max-Planck Institut f ϋ r Astrophysik, Garching Istituto Naz. di Astrofisica, Oss. Astron. Trieste Astronomy Department and RESearch Centre for the Early Universe, University of Tokyo. The Type Ic SN 1998bw. SN1998bw was a very bright - PowerPoint PPT PresentationTRANSCRIPT
Long-GRBs and Hypernovae
Paolo A. Mazzali
Max-Planck Institut fϋr Astrophysik, Garching
Istituto Naz. di Astrofisica, Oss. Astron. Trieste
Astronomy Department and RESearch Centre for the Early Universe,
University of Tokyo
17.5.2006 Swift Meeting, Venice, 7.6.06 4
The Type Ic SN 1998bw
SN1998bw was a very bright
Type Ic SN, with very broad
absorption lines, indicative of
high-velocity ejecta (~0.1c),
and of
a very energetic explosion
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Type Ic SNe / Hypernovae
Broad lines
Large Kinetic Energy
“Hypernovae”
(only SN1998bw was associated with a GRB)
Narrow lines
“normal” KE (1 foe)
Normal SN Ic
Mazzali et al. 2002
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GRB/SN LCs are brightestOther broad-lined SNeIc w/o GRB are dimmer
Narrow-lined, non-GRB SNeIc are dimmest
Mazzali et al. 2002
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Light curves can be degenerate
if both M and E are allowed to vary
4/1
4/32/1
E
MLC
Iwamoto et al. 1998
SN 1998bw
LC
Determining the properties of SN 1998bw
17.5.2006 Swift Meeting, Venice, 7.6.06 9Iwamoto et al. 1998
SN 1998bw
Early-time spectra
Model CO138
ergKE 52105
17.5.2006 Swift Meeting, Venice, 7.6.06 10Mazzali et al. 2001
SN 1998bw
Late-time spectra
`Broad-line’ models
v~10,000 km/s
Fits FeII lines
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56Fe
16O
Spherical
Aspherical
FeII] 5200A
[OI] 6300A
Observed
Interpretation as an Aspherical explosion
Orientation 15 deg
Maeda et al. 2002
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SN2003dh: the nebular phase
The nebular spectrum shows a strong but narrow [O I]6300 line, like SN1998bw.
Model:
v = 5000 km/s
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A non-GRB HN: SN2002ap
KE = 4 foe
Mazzali et al.2002
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SN 2002ap: nebular models
Foley et al. 2003[O I] line is sharp: no asphericity?
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Non-GRB, broad lined SN Ic: 1997dq (= SN1997ef)
M(56Ni) = 0.15M⊙.
[OI] profile rounded: no asphericity?
(Mazzali et al. 2004)
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SN 83N 94I 02ap 97ef/dq 98bw
type Ib Ic Ic (Hypernovae)
MZAMS 15 15 21 34 40
MHe 4 4 6.6 13 16
MCO 2 2 4.5 11 14
MExpl 4 2.1 4.6 11.1 13.8
MRem 1.25 1.2 2.1 1.6 2.9
MEj 2.75 0.9 2.5 9.5 10.9
MHe 2.0 --- 0.1 --- ---
MCO 0.5 0.6 1.8 5.3 8
MIME(Si,S) 0.1 0.2 0.5 4 2
MNi 0.15 0.07 0.1 0.13 0.7
E51 1 1 5 19 50
GRB X X X X
Properties of Type Ib/c Super/Hypernovae
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?56MSMNiM
`bright’ branch:
Hypernovae
`faint’ branch:
SN1997D etc.
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?MSMKE
Again two branches
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Properties of GRB/HNe: Photospheric velocities
• Velocity also seems to be proportional to global properties: GRB/SNe have the highest velocities
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3 HNe/GRB
Same SN properties,
but very different
X-ray light curves
(and radio properties)
What is the diagnostic value?
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[OI] line profiles as tracers of Asphericity
• GRB/SNe show [O I] line narrower than [Fe II] lines aspherical explosions viewed near the axis of
energy injection (in agreement with presence of GRBs)• Lower energy, non-GRB/SNe do not share this.
• Are GRB/SNe the only aspherical SNe Ic?• No: normal SNe Ic are polarised• GRB/SNe may be the most aspherical SNe• What is the effect of the viewing angle?
looking for asphericity through late-time spectra: a Subaru-VLT campaign
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The bright Type Ic SN 2003jd
• SN 2003jd was as bright at peak as SN1998bw (Mv = -18.7)
• Early-time spectra had broad lines, similar to HN SN2002ap
• No GRB or XRF
Mazzali et al. (2005)
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SN 2003jd:
• The [O I] 6300A line shows a double peak, suggesting an explosion similar to SN1998bw but viewed ~70° from the axis
(Subaru and Keck data, Mazzali et al. 2005)
an aspherical SN viewed off-axis
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What we see depends on where we look…
(von oben Gammablitz, von der Seite
Supernova?)
Mazzali et al. (2005)
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Was SN 2003jd also a GRB/HN?
• X-ray and Early Radio upper limits are not in contradiction with a GRB viewed off-axis
• Later Radio upper limits (Soderberg et al 2005) indicate no jet
Mazzali et al. 2005
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FACTS• GRB/SNe (SNe Ic) are highly energetic (Eiso~50foe,
Etrue~10foe) and aspherical• Less energetic SNe Ic appear less aspherical• XRFs may be connected to less energetic SNe and
to off-axis events RADIO FACTS• HNe in GRBs (and XRFs) have radio • Off-axis HNe (and lower-E SNe Ic) show no radio… QUESTIONS1) Do all HNe make GRBs? (γ- and optical sample ≠)2) Where are the off-axis GRBs?3) What are the jet properties? (is there a jet at all)?
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SN2006aj: Bolometric Light Curve
SN2006aj was dimmer than other GRB/SNe (98bw, 03dh, 03lw)
Light curve similar to non-GRB broad-lined SN Ic 2002ap, but brighter
Estimate ~ 0.2M⊙ of 56Ni
Rapid LC evolution:
Mej3/E is small
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SN2006aj: Spectral modelling
Model similar to that used for SN2002ap, but with smaller Mej, KE, more 56Ni, less O.
O-dominated shell (~0.1Mʘ) at 20-25,000 km/s: shell ejection from progenitor?
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Evolution of photosheric velocity from spectral modelling
• SN2006aj never reached velocities as high as the GRB/SNe
• It is intermediate between non-GRB, broad-lined SNe Ic such as SN2002ap and SN1997ef, and GRB/SNe
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Light Curve model of SN2006aj
Explosion model gives a LC consistent with results of spectral fitting
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Placing SN2006aj in context
A neutron star-making SN
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Conclusions (for now….)
• SN 2006aj exploded as a CO core (a WR star) of ~3.2 Mʘ.
• The ejecta (~2Mʘ) consisted of O (~1.3Mʘ), and heavier elements (~ 0.5Mʘ), incl. ~ 0.2Mʘ of 56Ni.
• A NS (M ~ 1.4 Mʘ) was formed.
The progenitor of SN 2006aj was a small mass star (MZAMS ~ 20 Mʘ).
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Hypotheses, future checks
• Magnetar activity may have been responsible for the high energy transient
possible rebrightenings
• Asymmetries, orientation TBD when nebular spectra available (from July) – expect [O I] 6300,6363Å emission to be weak and broad
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The Grand Scheme• Collapse of very massive (~35-50 M⊙), stripped
stars to Black hole makes GRB-HN (GRB can be very different, HN much less).
• Collapse of less massive star (~ 20 M⊙) to NS
can cause an XRF (via magnetic activity ?). • Some of these NS may later (when spin is lower)
harbour some short-hard GRBs (SGRs).• If system is a close binary (possibly necessary
for mass loss) it may end as a NS-NS merger and again produce a short-hard GRB.