1 / 20

Day 8550: 23.41 years since outburst

How old were you when this issue appeared ?. Day 8550: 23.41 years since outburst. NASA/ADS: 2435 (~2 /week) refereed papers, 24875 c. (since 1987) Crab : 2511 (23658 c.) since 1892 Cass A: 239 (2596 c.) since 1948. Collaborators : mid -IR: Eli Dwek , Rick Arendt, James de Buizer

marcus
Download Presentation

Day 8550: 23.41 years since outburst

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. How oldwereyouwhenthis issue appeared? Day 8550: 23.41 years since outburst • NASA/ADS: 2435 (~2 /week) refereed papers, 24875 c. (since 1987) • Crab : 2511 (23658 c.) since 1892 • Cass A: 239 (2596 c.) since 1948

  2. Collaborators: • mid-IR: Eli Dwek, Rick Arendt, James de Buizer • X-rays : Sangwook Park • HST : SAINTS Team (R. Kirshner, PI) • CSM : Ben Sugerman, ArlinCrotts, Steve Lawrence Supernova SN 1987A - The birth of a Remnant –P. Bouchet & J. Danziger • 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

  3. Imaging with the Hubble Space Telescope (HST) SAINTSCollaboration CSM : EQ ring 1.34 lt-yr; i = 45°, produced by a mass loss event that occurred ~ 20,000 before explosion

  4. X-ray Imaging N ROSAT/HRI (5” pixels) HEASARC/SkyView E ACIS (1999-10): Burrows et al. 2000 Green-Blue: ACIS Red: HST Contour: ATCA 1 arcsecond Park, 2007

  5. mid-IR Imaging

  6. ATNF, Gaensler, 2007 • Limb brightened • Bright lobes to • east and west • Eastern lobe • brighter than • western lobe, • & brightening • faster •  Same as X-rays Radio Imaging ATCA 9 GHz diffraction limited (0.9 arcsec) ATCA 9 GHz super-resolved (0.5 arcsec)

  7. Park et al., 2006; Zhekov et al., 2009  2-shocks model • Soft X-Ray = Decelerated, slow (300-1700 kms-1); kT= 0.3 – 0.6 keV • Hard X-Ray = High-speed (3700±900 kms-1); kT= 2 – 5 keV X-ray and Radio Light Curves 0.5-2 keV 3-10 keV Chandra (0.5 – 2 keV) Density and Temperature of the soft X-ray emitting gas have not significantly changed during the > 5 years period. 0.5-2 keV fractional flux “Fast” shock d ~ 6200 ATCA X-ray Flux (10-13 ergs/cm2/s) Chandra/ACIS X-ray Flux (10-13 ergs/cm2/s) ROSAT Chandra (3 – 10 keV) ROSAT (Hasinger et al. 1996) Similar rates of hard X-ray and radio X-ray (2005-7) vs. Optical (2005-4) Radio: Gaensler & Staveley-Smith, 2007 ACIS 3-8 keV Contours: ATCA 9GHz ACIS 0.4-0.5 keV Contours: ATCA 9GHz ACIS 0.5-2 keV: Park et al., 2008 Contours: HST (Peter Challis)

  8. 11.7μm(Bouchet et al., 2006)and HST(Challis, 2006) EQUATORIAL RING McCray, 2007 HOT « FINGERS » Optical/Soft X-rays IR?? SHOCK WAVE ? NS/BH HOT GAS Hard X-rays REVERSE SW Radio COOL EJECTA Low speed oblique radiative shock: optical/UV Slower shock in high-density knot: soft X-rays High speed shock: radio, hard X-ray Cf. Michael et al. 1998

  9. Mid-IR observations of the Circumstellar Dust VISIR, VLT T-ReCS, Gemini T-ReCS, Gemini T-ReCS, Gemini 6526 7241 7569 6067 ~ ~ ~ 6526, Qa 7241/6067, N 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).

  10. HST vs VISIR (VLT) Overlay of HST (Dec2006) (black) with VISIR (red-yellow) shows correlation far from 100 percent! Other comparisons show dust annulus possibly (?) thicker than visual HST annulus. • Whatheats the dust? • Collisionalheating? • Radiative heating? • Whereis the dust? • In the X-ray emittinggas? • In the denser UVO emittingknots?

  11. Origin of the mid-IR emission? T-ReCS/HST ACIS/11.7 mm ACIS/18.3 mm ATNF/18.3 mm ATNF/11.7 mm

  12. Observations with SPITZER Silicates Silicates + Black body Grain absorption coeffs.  ne = (2 – 4) x 104 cm-3 ne (cm-3) Dwek et al., 2010 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 ?

  13. IRX: the IR to X-ray Flux ratio  Dust cooling dominates the cooling via atomic transitions at T ≥ 106 K L(Te): Equilibrium atomic cooling rate for a plasma with ER abundances L(Te) erg cm3 s-1 Ld(T): Gas cooling rate via dust –gas collisions SN 1987A Te (K) 1987, ApJ 320 Dwek et al., 2010 L(T) Cooling rate via atomic processes ≈ 2.5  a ≥ 0.30 mm IRX = = Ld(T) Cooling rate via dust-gas collisions The cooling of the shocked gas is dominated by IR emission from the collisionally-heated dust with radii > 0.3 mm, and a significant fraction of the refractory elements in the ER is depleted onto dust (Dwek et al., 2010)

  14. IRX vs. Dust Destruction No obvious dust destruction yet No cooling of the shocked gas yet IRX Constant  • t(Si grains) = 4 – 15 yr, t(C dust) = 0.4 – 1 yr • Gas cooling time for the shocked gas = 12 – 20 yr • grain destruction may become important only at day ≈ 9200 •  the X-ray emission may not be affected until t ≈ 30 yr IRX IRX  a ≥ 0.30 mm Te (K) Dwek et al., 2008 Mass of radiating dust in ring = ~10-6 MSun

  15. Observations with the Hubble Space Telescope The SAINTS team (PI: R.P. Kirshner) monitors SN 1987A with HST since it was launched. The recent repair of STIS allows us to compare observations in 2004, just before its demise, with those in 2010. The young remnant of supernova 1987A (SN 1987A) offers an unprecedented glimpse into the hydrodynamics and kinetics of fast astrophysical shocks • 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 France et al., 2010

  16. Central part (debris) shows blue (approaching) extends to ~4000 – 6000 km/s. Red extension not apparent because dust in ejecta blocks far side receding (France et al., 2010).

  17. Lya 2010 – 2004 difference image (black indicatessimilarintensities): Lyaemission has increased in brightness by factor 1.6 – 2.4 increased flux of H atomsinto the shockregion The maximum Doppler shift in the northernblueshiftedemissionisdecreasing as a function of time (France et al., 2010) Lya:Ha ~ 80 (5:1 for a Balmer-dominatedshock) If the Lya photons produced by the samemechanism as the Ha photons Lya:Hashouldbe the same for all velocities a sufficientnumber of Lya photons are emitted by the hotspotsand the neutral H layer in the expandingenvelopescattersLya photons by ~ 6000 kms-1

  18. 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(?) Slit in geocoronal Lya  N V emission provides a unique probe of the isotropization zone of the collisionless shock (France et al., 2010) • H atoms are excited by collisions withoutsignificantdeflection • N atomsbecomeionized and gyrate about a magneticfieldthatisparallel to the shock and movingwith the fluidvelocity of the shocked plasma.

  19. G54.1+0.3 IR shell – gas and dust condensed from SN debris and then heated by stars in cluster. Expanding pulsar wind also heats dust.

  20. THE END….. (Thankyou!)

More Related