iau symposium 279 death(s ) of massive stars
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IAU Symposium 279 Death(s ) of Massive Stars. S R Kulkarni Caltech Optical Observatories. A magnificent & elegant Setting. But NIPPON is also … ( a personal perspective). Nippon is also …. Nippon is also … . Very clever … . . Nippon is also …. Nippon is also…. - PowerPoint PPT PresentationTRANSCRIPT
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IAU Symposium 279Death(s) of Massive Stars
S R KulkarniCaltech Optical Observatories
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A MAGNIFICENT & ELEGANT SETTING
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BUT NIPPON IS ALSO …(a personal perspective)
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Nippon is also …
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Nippon is also …
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Very clever ….
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Nippon is also …
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Nippon is also…
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NIPPON IS INDOMITABLE SPIRIT我慢
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Many thanks• The LOC
– Great choice of location– Impeccable arrangements– Firm Bell Person
• The SOC– Excellent choice of speakers– Giving young people opportunities
• The Speakers– Keeping to time – High quality
• Funding agencies– IAU, MEXT, Tokodai, IPMU, SWRI, JSPS, ASJ
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NOW TO SERIOUS BUSINESS
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Palomar Sky SurveyThe Beginning of Supernovae Research
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Fritz Zwicky at P18
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The Core-Collapse SpectrumLower mass limit unclear: <7..11 solar; stable C/O core
M: 7-11
RSG=II-P
M: 8-16 M: 17-25
W-R = Ib/c?
M: 25-30
GRB
M: 40-50
NS BH
SN IIn
M: 50-150
PI SNe
M> 150
BH No remnantNS NS
EC SN?
AIC
BSG
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• The WD-NS boundary is well determined
• For massive stars mass loss determines destiy
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Progenitors: Progress
• Type IIP progenitors now well established (RSG)• Progenitors of Ic are compact objects (not more
than 1011 cm)• Progenitors for long duration GRBs are massive stars• Progenitors of Super-luminous SN are massive stars
and very large R0
• Progenitors of Pair Instability SN are very massive stars
• Type IIn and LBVs are linked
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Open questions & controversies
• What (rare) type of massive stars end as GRBs?• What is the mass spectrum of Population III stars?
(40 versus 400 Mo!)• What factors determine NS versus BH outcome?• What factors determine NS versus magnetar?• Is stellar collisions important for certain outcomes?• Are there some LGRBs without SNe?• Is there a fundamental difference between
GRB890425 and classical GRBs?
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Obvious questions but likely messy answers
• What factors determines mass loss rates? • How does the environment shape the IMF?• What is the role of metallicity?
– Determining IMF– Retaining (or radiating) angular momentum
• Do (slowly rotating) BH outcomes produce detectable SN?• Explosion Mechanism for CC SNe:
– Are there many cases which require bipolar explosion mechanism? • LGRB:
– How is energy carried? (relativistic jets versus Poynting vector)– What determines jet opening angles?
• Are Ultra-high energy Cosmic Rays produced by stellar death?• What re-ionizes the early Universe?
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Stellar Deaths: Not an Unfinished Chapter but an Unfinished Book
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Angular momentum budget
rotating wave + advected vorticity = 0
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Constraints: progenitors of GRBs
Fruchter et al. 2006; Svensson et al. 2010; Fong et al. 2010
LGRB
CCSN
SGRB
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1. LGRBs are extremely rare explosions
2. LGRBs are produced in copiously star forming regions
3. Be more common at low metallicity but not precluded in high metalicity regions
4. GRB explosions are strongly collimated (``jetted’’)
Long Duration GRBs (LGRBs)
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EITHER GREAT BEGINNINGS OR MERE CURIOSITIES
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Massive Stars Exist Locally
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SN2010jp: A Truly Bipolar Supernovae
MMT
Palomar
Keck
MMT
Keck
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Blackbody Component in LGRBsGRB-SN z Epk Eiso T90 kT FBB/Ftot LBB RBB keV erg s keV % erg/s cm
060218 0.033 403 4x1049 2100 0.220.14 50+ -- 5x1011
100316D 0.059 4014 >4x1049 >1300 0.14 30 3x1046 8x1011
090618 0.54 13 2.5x1053 113 0.90.3 20 1x1049 6x1012
101219B 0.55 70 4x1051 51 0.2 11 1x1047 --
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“WILL NOT SHY AWAY FROM TOUGH ISSUES”
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Metalicity
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THERE IS PLENTY OF ROOM TO GROW SIDEWAYS …
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41 43
Ancient (Impressive)
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Cathedrals (->Bankruptcy)
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Kasli
wal
201
1 (P
hDT)
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Parameter space
LGRBsSGRBs
SGRs
?
TDEs?
Galactic sources (SGR, LMXB, HMXB, microquasar, gamma-ray pulsars etc)
LLGRBs
060218100316D030329
AGN031203
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Inverted (Pretty)
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Inverted (The Exciting Future)
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Bibliography
• Speakers who freely gave me their talks• xkcd (geeky cartoons)• Google (for images)• Rabbits of the Okunoshima Island
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Results | three light curve families
Plateau
Slow Decline
Rapid DeclineSN1993J – Richmond et al. 1994SN1999em – Leonard et al. 2002SN2004fx – Hamuy et al. 2006 (preliminary)
SN2005cs – Pastorello et al. 2009SN2011dh – Arcavi et al. 2011