A New Window on Radio and X-ray emission from Strongly Interacting Supernovae Poonam Chandra Royal Military College of Canada Collaborators: Roger Chevalier, Alicia Soderberg, Claes Fransson, Nikolai Chugai Poonam Chandra Royal Military College of Canada Collaborators: Roger Chevalier, Alicia Soderberg, Claes Fransson, Nikolai Chugai Supernovae Core collapse supernovae: explosion of a massive star in a red supergiant phase. Progenitor star > 8 M sun. Thermonuclear supernovae: explosion of a carbon-oxygen white dwarf in a binary system. Progenitor star 4-8 M sun in a binary. SN/GRB explosion centre Photosphere Outgoing ejecta Reverse shock shell Contact discontinuity Forward shock shell SN/GRB explosion centre Photosphere Outgoing ejecta Reverse shock shell Contact discontinuity Forward shock shell Circumstellar environment 10 5 K 10 9 K 10 7 K Radio emission from Supernovae: Synchrotron non-thermal emission of relativistic electrons in the presence of high magnetic field. X-ray emission from Supernovae: Both thermal and non-thermal emission from the region lying between optical and radio photospheres. Interaction of SN ejecta with CSM gives rise to radio and X-ray emission Examples of CS interaction Chandra et al. 2009, to appear in ApJ Chandra et al. 2009, ApJ, Nymark, Chandra, Franssion 2009, A&A Chandra et al Chandra et al. 2005, ApJ With Chris Stockdale, Alak Ray, Claes Fransson, Eric Schlegel, Kurt Weiler, Roger Chevalier, Tanja Nymark and more Radio light curves of SN 1995N How fast ejecta is decelerating? R~t -0.8, this also implies n=8 (m=(n-3)/(n-2) in R~t -m ) What is the mass loss rate of the progenitor star? Mass loss rate = ~10 -4 M sun yr -1 Red supergiant star on M sun in a superwind phase Density and temperature of the shocked shells Forward shock: T=2.4 x 10 8 K, Density=3.3 x 10 5 cm -3 Reverse shock: T=0.9 x 10 7 K, Density= 2 x 10 6 cm -3 How fast ejecta is decelerating? R~t -0.8, this also implies n=8 (m=(n-3)/(n-2) in R~t -m ) What is the mass loss rate of the progenitor star? Mass loss rate = ~10 -4 M sun yr -1 Red supergiant star on M sun in a superwind phase Density and temperature of the shocked shells Forward shock: T=2.4 x 10 8 K, Density=3.3 x 10 5 cm -3 Reverse shock: T=0.9 x 10 7 K, Density= 2 x 10 6 cm -3 SN 1995N NeX NeIX Mass of the progenitor For f = 0.1, n e = 2 x 10 6 cm -3, n Ne = 600 cm -3 Corresponding Neon mass ~ M sun. Compatible with M sun progenitor star. X-ray studies of SN 1993J (Chandra et al 2009; Nymark, Chandra, Fransson 2008) X-ray spectrum of SN 1993J ( Nymark, Chandra, Fransson 2008) X-ray emission from reverse shock in the CNO zone Multiwaveband campaign for Type IIn supernovae Very Large Array: hours of time every cycle Swift XRT: 3 SNe every cycle ChandraXO: 45 ks time XMM-Newton: 86 ks time More than 24 supernovae with the VLA. Best detection SN 2006jd and SN 2005kd. 2.5 Frequency Flux density Luminosity ratio 2005kd 2006jd Chevalier 2006 Conclusions Type IIn supernovae, revealing a new population of supernovae. SN 2006jd indicate bizarre light curve and spectrum, probably indicating increased CS interaction. More observations underway, which will give a better picture of this unique class of supernovae. Free-free absorption: absorption by external medium Information about mass loss rate. Synchrotron self absorption: absorption by internal medium Information about magnetic field and the size. Poonam Chandra Forand Break frequency (Fransson & Bjornsson, 1998, ApJ, 509, 861) GMRT VLA Synchrotron cooling break at 4 GHz Frequency FluxFlux Synchrotron cooling break at ~ 5.5 GHz GMRT VLA Frequency FluxFlux Day 3200Day 3770 SN 1993J On day 3200 B=330 mG On day 3770 B=280 mG Diffusion acceleration coefficient =(5.3 +/- 3.0) x cm 2 s -1 Diffusion acceleration coefficient =(5.3 +/- 3.0) x cm 2 s -1