View
215
Download
1
Category
Preview:
Citation preview
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
e
Day 8550: 23.41 years since outburst
How old were you
How old were you when this issue when this issue appeared?
appeared?
NASA/ADS: 2435 (~2 /week) refereed papers, 24875 c. (since 1987)Crab : 2511 (23658 c.) since 1892Cass A: 239 (2596 c.) since 1948
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
eSupernova SN 1987A Supernova SN 1987A
- The birth of a Remnant –- The birth of a Remnant –P. Bouchet & J. Danziger P. Bouchet & J. Danziger
Collaborators: Collaborators: • mid-IR: Eli Dwek, Rick Arendt, James de Buizermid-IR: Eli Dwek, Rick Arendt, James de Buizer• X-rays : Sangwook ParkX-rays : Sangwook Park• HST : SAINTS Team (R. Kirshner, PI)HST : SAINTS Team (R. Kirshner, PI)• CSM : Ben Sugerman, Arlin Crotts, Steve Lawrence CSM : Ben Sugerman, Arlin Crotts, Steve Lawrence
• Five Years of Mid-Infrared Evolution of the Remnant of SN 1987A: The Encounter Between the Blast Wave and the Dusty Equatorial Ring: Dwek, E. et al., 2010, ApJ in press• Observing Supernova 1987A with the Refurbished Hubble Space Telescope, France, K., et al., 2010, Science, in press• Infrared and X-Ray Evidence for Circumstellar Grain Destruction by the Blast Wave of Supernova 1987A: Dwek, E., et al., 2008, ApJ, 676, 1029 • SN 1987A after 18 Years: Mid-Infrared Gemini and Spitzer Observations of the Remnant: Bouchet, P., et al., 2006, ApJ, 650, 212 • High-Resolution Mid-infrared Imaging of SN 1987A: Bouchet, P., et al., 2004, ApJ, 611, 394 • Evolution and Geometry of Hot Spots in Supernova Remnant 1987A: Sugerman, B., et al., 2002, ApJ, 572, 209
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
e
Imaging with the Hubble Space Telescope
(HST)
CSM : EQ ring 1.34 lt-yr; i = 45°, produced by a mass loss event that occurred ~ 20,000 before explosion
SAINTSCollaboration
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
e
X-ray Imaging
N
EROSAT/HRI (5” pixels)
HEASARC/SkyView
1 arcsecond
ACIS (1999-10): Burrows et al. 2000
Green-Blue: ACIS
Red: HST
Contour: ATCA
Park, 2007
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
e
mid-IR Imaging
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
e
ATCA 9 GHz super-resolved (0.5 arcsec)
Radio Imaging
• Limb brightened
• Bright lobes to east and west
• Eastern lobe brighter than western lobe, & brightening faster
Same as X-raysSame as X-rays
ATCA 9 GHz diffraction limited (0.9 arcsec)
ATNF, Gaensler, 2007ATNF, Gaensler, 2007
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
e
Chandra
(0.5 – 2 keV)
Chandra
(3 – 10 keV)
ATCA
ROSAT
Similar rates of hard X-ray and radio
ACIS 3-8 keVACIS 3-8 keV
Contours: ATCA 9GHzContours: ATCA 9GHz
X-r
ay
Flu
x (1
0-1
3 e
rgs/
cm2 /
s)
X-r
ay F
lux (
10
-13
erg
s/cm
2/s
)
0.5-2 keV
3-10 keV
“Fast” shock0.5-2 keV fractional flux
ROSAT
(Hasinger et al. 1996) Chand
ra/A
CIS
X-ray (2005-7) vs. Optical (2005-4)
d ~
620
0
ACIS 0.5-2 keV: Park et al., 2008
Contours: HST (Peter Challis)
Radio: Gaensler & Staveley-Smith, 2007
Park et al., 2006; Zhekov et al., 2009 2-shocks model1. Soft X-Ray = Decelerated, slow (300-1700 kms-1); kT= 0.3 – 0.6 keV
2. Hard X-Ray = High-speed (3700±900 kms-1); kT= 2 – 5 keV
X-ray and Radio Light Curves
Density and Density and Temperature of Temperature of the soft X-ray the soft X-ray
emitting gas have emitting gas have not significantly not significantly changed during changed during the > 5 years the > 5 years
period. period.
ACIS 0.4-0.5 keV
Contours: ATCA 9GHzContours: ATCA 9GHz
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
e
Cf. Michael et al. 1998
EQUATORIAL RING
HOT « FINGERS »
SHOCK WAVE
HOT GAS
REVERSE SW
COOL EJECTA
NS/BH ?
Optical/Soft X-raysOptical/Soft X-rays
IR??IR??
Hard X-raysRadioRadio
11.7μm (Bouchet et al., 2006)(Bouchet et al., 2006) and HST (Challis, (Challis, 20062006)
McCray, 2007McCray, 2007
Low speed oblique radiative shock: optical/UV
Slower shock in high-density knot: soft X-rays
High speed shock: radio, hard X-ray
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
eMid-IR observations of the
Circumstellar Dust
6067
6526 7241
7569
6526, Qa
7241/6067, N
T-ReCS, Gemini T-ReCS, GeminiT-ReCS, Gemini VISIR, VLT
~~
~
The silicate emission increased as t0.87, consistent with X-ray observations, suggesting the blast wave has transitioned from a free expansion to the Sedov phase (now
expanding into the main body of the ER).
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
e
Overlay of HST (Dec2006)(black) with VISIR (red-yellow)
shows correlation far from100 percent!
Other comparisons showdust annulus possibly (?) thicker
than visual HST annulus.
HST vs VISIR (VLT)
Where is the dust?Where is the dust?1.1. In the X-ray emitting gas?In the X-ray emitting gas?2.2. In the denser UVO emitting knots?In the denser UVO emitting knots?
What heats the dust?What heats the dust?1.1. Collisional heating?Collisional heating?2.2. Radiative heating?Radiative heating?
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
e
Origin of the mid-IR emission?Origin of the mid-IR emission?
T-ReCS/HST
ACIS/11.7m ACIS/18.3m
ATNF/11.7m ATNF/18.3m
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
eObservations with SPITZER
Silicates Silicates + Black body
Mystery contributor: much higher T, grain radii or IR emissivity smaller, significantly shorter sputtering time, distinct evolution: No temporal change of spectral shape
and in the mass ratio?: A clue to binarity of progenitor ?A clue to binarity of progenitor ?
Grain absorption coeffs.
ne = (2 – 4) x 104 cm-3
n e (
cm-3)
Dwek et al., 2010
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
e
IRX: the IR to X-ray Flux ratio
(T
e) e
rg c
m3
s-1
Te (K)
(Te): Equilibrium atomic cooling rate
for a plasma with ER abundances
d(T): Gas
cooling rate via dust –gas
collisions
Dust cooling dominates the cooling via atomic transitions at T ≥ 106 K
IRX = =
(T) Cooling rate via atomic processes
d(T) Cooling rate via dust-gas collisions≈ ≈ 2.5 2.5 a a ≥ 0.30 ≥ 0.30 m m
Dwek et al., 2010 1987, ApJ 320
SN 1987A
The cooling of the shocked gas is dominated by IR emission from the collisionally-heated dust with radii > 0.3 m, and a significant fraction of the
refractory elements in the ER is depleted onto dust (Dwek et al., 2010)
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
e
Mass of radiating dust in ring = ~10-6 MSun
No obvious dust destruction yetNo obvious dust destruction yetNo cooling of the shocked gas yetNo cooling of the shocked gas yet
IRX vs. Dust Destruction
Te (K)
IRX
IRX Constant
IRX IRX a a ≥ 0.30 ≥ 0.30 m m
Dwek et al., 2008
(Si grains) = 4 – 15 yr, (C dust) = 0.4 – 1 yr Gas cooling time for the shocked gas = 12 – 20 yr
grain destruction may become important grain destruction may become important only at day only at day ≈ 9200 ≈ 9200
the X-ray emission may not be affected until the X-ray emission may not be affected until t ≈ 30 yr t ≈ 30 yr
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
e
Last Results (January 31st., 2010): • Ly and H lines from shock emission continue to brighten, while their maximum velocities continue to decrease. • Evidence for resonant scattering (within the source) of Ly photons from hotspots on the equatorial ring (to blueshifts −12,000 km s∼ −1) . • Emission to the red of Ly attributed to N V 1239,1243Å
Observations with the Hubble Space Telescope
The SAINTS team The SAINTS team (PI: R.P. Kirshner) (PI: R.P. Kirshner) monitors SN 1987A with monitors SN 1987A with HSTHST since it since it was launched. was launched. The recent repair of The recent repair of STIS allows us to compare observations STIS allows us to compare observations
in 2004, just before its in 2004, just before its demise, with those in 2010.demise, with those in 2010.
The young remnant of supernova 1987A (SN 1987A) The young remnant of supernova 1987A (SN 1987A) offers an unprecedented glimpse into the hydrodynamics offers an unprecedented glimpse into the hydrodynamics
and kinetics of fast astrophysical shocksand kinetics of fast astrophysical shocks
France et al., 2010
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
e
Central part (debris) shows blue (approaching) extends to ~4000 – 6000 km/s. Red extension not apparent because dust in ejecta dust in ejecta blocks far side receding blocks far side receding (France et al., 2010).(France et al., 2010).
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
eLy 2010 – 2004 difference image (black
indicates similar intensities):
1.Lyemission has increased in
brightness by factor 1.6 – 2.4 increased flux of H atoms into the shock region2.The maximum Doppler shift in the northern blueshifted emission is decreasing as a function of time
If the Ly photons produced by the same mechanism as the H photons Ly:H should be the same for all velocities a sufficient number of Ly photons are emitted by the hotspots emitted by the hotspots and the neutral H layer in the expanding envelope scatters Ly photons by ~ 6000 kms-1
LyLy:H:Hfor a Balmer-for a Balmer-
dominated shockdominated shock
(France et al., 2010)(France et al., 2010)
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
e
Slit in geocoronal Ly
N V lines are detectable because, unlike hydrogen atoms, N4+ ions emit hundreds of photons before they are ionized. The profiles of the N V lines differ markedly from that of H scattering of N4+ ions by magnetic fields in the ionized plasma(?)
N V emission provides a N V emission provides a unique probe of the unique probe of the
isotropization zone of the isotropization zone of the collisionless shockcollisionless shock
H atoms are excited by collisions without H atoms are excited by collisions without significant deflectionsignificant deflection N atoms become ionized and gyrate about a N atoms become ionized and gyrate about a magnetic field that is parallel to the shock and magnetic field that is parallel to the shock and moving with the fluid velocity of the shocked moving with the fluid velocity of the shocked plasma. plasma.
(France et al., 2010)(France et al., 2010)
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
eG54.1+0.3
IR shell – gas and dust condensed from SN debris and then heated by stars in cluster. Expanding pulsar wind also heats dust.
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRF
U/
Ser
vice
d
’Ast
rop
hys
iqu
e
THE END….. (Thank you!)THE END….. (Thank you!)
Recommended