A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.
-
Upload
josephine-balding -
Category
Documents
-
view
215 -
download
0
Transcript of A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.
![Page 1: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/1.jpg)
A Chandra view to Exploding Stars
SN2014J
R. MarguttiHarvard
nothing
![Page 2: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/2.jpg)
Margutti +13, +14; Kamble +13; Soderberg +06, +10
Energy partitioning
SNe are an OPTICAL phenomenon1051 erg OPTICAL
1047 ergX-rays/Radio
![Page 3: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/3.jpg)
RADIATION from the REMNANT
X-rays from Supernovae
Log Time
Log Lx
< hr
SHOCK BREAK OUT(R exploding star)
Δt≈ 2msT≈250 keVE≈3 1041 erg Δt≈ hrs
(@ T0+5hrs)T≈ X-raysE≈1046-47 ergL~1044 erg/s
SHOCK INTERACTIONw. COMPANION
(R and distance of the companion)
Kasen +10
< several hrs
SHOCK/JET INTERACTION w. the MEDIUM
(mass-loss of the progenitor)
> 10 years
MASS-LOSS
PROGENITORS
SOURCE of ENERGY
![Page 4: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/4.jpg)
…BUT…
![Page 5: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/5.jpg)
RADIATION from the REMNANT
X-rays from Supernovae
Log Time
Log Lx
< hr
< several hrs
SHOCK/JET INTERACTION w. the MEDIUM
(mass-loss of the progenitor)
> 10 years
MASS-LOSS
SHOCK BREAK OUT(R exploding star)
Δt≈ 2msT≈250 keVE≈3 1041 erg Δt≈ hrs
(@ T0+5hrs)T≈ X-raysE≈1046-47 ergL~1044 erg/s
SHOCK INTERACTIONw. COMPANION
(R and distance of the companion)
Kasen +10
PROGENITORS SOURCE of ENERGY
![Page 6: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/6.jpg)
MASS-LOSSDirect probe of EVOLUTION,Indirect probe of PROGENITORS
SOURCE of ENERGY
Explosion Mechanism
Type Ia SNe, Type Iax , Type Ibc, Type IIb, Strongly interacting SNe, Relativistic SNe, GRB-SNe, Super-Luminous SNe
Type Ia
Relativistic SNe
![Page 7: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/7.jpg)
The PROBLEM
Progenitor System
“…The end is where we start from…”
The Little Gidding by T. S. Eliot
Type Ia SN explosion
?
![Page 8: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/8.jpg)
WD
Two possible answers
?Double Degenerate
(DD)
Single Degenerate(SD)
Exploding star
HIGH-density environment
DIRTY
LOW-density environment
CLEAN “Tra
ditio
nal”
way
of t
hink
ing
![Page 9: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/9.jpg)
Margutti +14
€
ρ =M•
4πR2vw@ R≈1016 cm
SD systems with STEADY mass-loss
![Page 10: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/10.jpg)
SD systems with STEADY mass-loss
Margutti +14
Ruled O
ut
![Page 11: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/11.jpg)
… “It’s black cats in dark rooms”… (S. Firenstein)
![Page 12: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/12.jpg)
Margutti +12; +14
![Page 13: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/13.jpg)
Mar
gutti
+12
; +14
![Page 14: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/14.jpg)
Mar
gutti
+14
… “Its black cats in dark rooms… and there may be no cat in the room” (S. Firenstein)
Symbiotic systems with stable mass-loss are ruled out
![Page 15: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/15.jpg)
MASS-LOSSType Ia
SOURCE of ENERGY
Relativistic SNe
Symbiotic systems with stable mass-
loss are ruled out
TAKE AWAY MESSAGES:
![Page 16: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/16.jpg)
Margutti+14
Radio
Rel SNe
Faint GRBs
In the Radio/optical relativistic SNe looks the same as faint GRBs
X-rays
Relativistic SNe are an intrinsically different class of explosions
![Page 17: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/17.jpg)
GRB Faint GRB Relativistic SN
Fully successful jet
break out
Barely successful
Barely failed
There is some good in every person
JetSN
![Page 18: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/18.jpg)
MASS-LOSSType Ia Symbiotic
systems with stable mass-
loss are ruled out
TAKE AWAY MESSAGES:
SOURCE of ENERGY
Relativistic SNe Jets might be ubiquitous
![Page 19: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/19.jpg)
X-rays from Supernovae
Log Time< few hr > 10 years
SHOCK BREAK OUT(R exploding star)
SHOCK INTERACTIONw. COMPANION
(R and distance of the companion)
SHOCK/JET INTERACTION w. the MEDIUM(mass-loss of the progenitor)
RADIATION from the REMNANT
(accreting BH, MAGNETAR)
Successful JET
PRESENT PAST FUTURE
Very early observations(DIFFICULT)
Faint(DIFFICULT)
RADIATION from the REMNANT in engine
driven SNe
10-100 days
Log Lx
COOLING ENVELOPE(R envelope)
ACCRETION onto the
progenitor
![Page 20: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/20.jpg)
SN1994I
SN2002ap
GRB/SNe
“Standard”, envelope stripped SN Ibc
Hydrogen-poorSuper Luminous SNe
(M<-21)(e.g. Gal-Yam 2012)
7x1043 erg/s
Super-Luminous SNe
![Page 21: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/21.jpg)
Super-Luminous SNe
![Page 22: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/22.jpg)
MASS-LOSSType Ia
SOURCE of ENERGY
Relativistic SNe
Symbiotic systems with stable mass-
loss are ruled out
TAKE AWAY MESSAGES:
Jets might be ubiquitous
Super-Lum I
![Page 23: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/23.jpg)
X-rays from Supernovae
Log Time< few hr > 10 years
SHOCK BREAK OUT(R exploding star)
SHOCK INTERACTIONw. COMPANION
(R and distance of the companion)
SHOCK/JET INTERACTION w. the MEDIUM(mass-loss of the progenitor)
RADIATION from the REMNANT
(accreting BH, MAGNETAR)
Successful JET
PRESENT PAST FUTURE
Very early observations(DIFFICULT)
Faint(DIFFICULT)
RADIATION from the REMNANT in engine
driven SNe
10-100 days
Log
Lx
COOLING ENVELOPE(R envelope)
ACCRETION onto the
progenitor
FUTURE
Thanks to the Chandra Team!!
MASS-LOSS
PROGENITORS
SOURCE of ENERGY
< hours
![Page 24: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/24.jpg)
BACK UP
![Page 25: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/25.jpg)
There is some good in every person
Barely successful jet break out
Consistent with hydrodynamical explosion (No need for a jet/engine)
Barely failed jet break out
Fully successful jet break out
JetSN
![Page 26: A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.](https://reader030.fdocuments.net/reader030/viewer/2022032702/56649cc05503460f94987904/html5/thumbnails/26.jpg)
Type Ia SN2014JHost Galaxy: M82, D=3.5 Mpc
Explosion image
Margutti +14Chandra X-ray images