Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010 IRFU/ Service d’Astrophysiqu e Day 8550: 23.41 years since outburst How old were you when this

Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010

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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


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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


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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


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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


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mid-IR Imaging


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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


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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


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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


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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).


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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?


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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


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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


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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)


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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


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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


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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).


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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)


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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)


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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.


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THE END….. (Thank you!)THE END….. (Thank you!)

Documents

Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010 IRFU/ Service d’Astrophysiqu e Day 8550: 23.41 years since outburst How old were you when this