Multi-wavelength Observations of Composite Supernova Remnan - PowerPoint Presentation

Slide1

Multi-wavelength Observations of Composite Supernova Remnants

Tea

Temim(NASA GSFC/ORAU)

Collaborators:Patrick Slane (CfA)Eli Dwek (GSFC)George Sonneborn (GSFC)Richard Arendt (GSFC)Yosi Gelfand (NYU Abu Dhabi)Paul Plucinsky (CfA)Daniel Castro (MIT)Slide2

Gaensler & Slane 2006

Evolution of PWNe inside SNRs

Early Evolution:

SNR is in the free expansion stage PWN expands supersonically inside the SNR and is bounded by a strong shock

The PWN shocks the inner SN ejecta that have not been re-heated by the reverse shock

Late Evolution:

The reverse shock heats the inner SN ejecta and crushes the expanding PWN

PWN expansion becomes unstable and reverberates

PWN continues to expand

subsonically

through SNRSlide3

Reverse shock encounters one side of PWN first and disrupts the nebula – moving pulsar or a density gradient in the ISM

After passage of the reverse shock

relic

PWN remains (typically observed in the radio) and a new PWN forms around the pulsarvan der

Swaluw

et al.

2004

t

SNR

= 1000 yr

t

SNR

= 1800 yr

t

SNR

= 3000 yr

t

SNR

= 11 400 yr

When pulsar’s motion becomes supersonic, new PWN deforms into a bow shock -

occurs when a pulsar has traveled 0.67R

SNR

(van der Swaluw 2004)

Bow Shock Nebula

NASA/CXC/

M.Weiss

Asymmetric Reverse Shock InteractionSlide4

Herschel

70

m

m,Chandra X-rayVLJHK (Mignani et al. 2012)B0540-69.3Chandra X-ray image

G21.5-0.9

[Fe II]

Zajczyk

et al. 2012

G54.1+0.3

Crab Nebula

Kes

75

Early Evolution – SN Dust and Ejecta

3C 58

Slane

et al. 2004Slide5

Dust

radiatively

heated by the PWN  broadband spectrum of the heating source well known

Hester 2008 Information about grain properties can provide clues on the progenitor type Dust surrounding PWNe is ejecta dust, not mixed with the ISM material Dust not been processed by the reverse shock, no dust destructionDust around PWNeSlide6

Dust formation in SN ejecta: Theoretical Predictions

(

Kozasa et al. 1989, 1991; Clayton et al. 1999, 2001; Todini

and Ferrara 2001; Nozawa et al. 2003; Bianchi and Schneider 2007; Kozasa et al. 2009, Cherchneff and Dwek 2010)Mass dominated by grains:> 0.03 μm in Type IIP SNe< 0.006 μm in Type IIb SNe (Kozasa,Nozawa et al. 2009)

Kozasa

et al. 2009

Type IIP

Type

IIb

High amount of can form in dense cooling SN ejecta within the first 600–1000 days - consists primarily of the most abundant refractory elements (e.g., C, Mg, Si, S, and Fe)

Total dust masses range between

0.1 – 1 M



with

2-20%

surviving the reverse shock

Forms in the He envelope where density is high and velocity low – grain properties depend on mass of the hydrogen envelopeSlide7

H

Heating rate

Cooling rate

Ln  non-thermal spectrum of the PWNHester 2008Temim & Dwek 2013

Crab Nebula: Dust Heating Model

Power-law grain size distributions

F(a

) = a

-

a

a

min

= 0.001

m

m

a

max

= 0.03-5.0

m

m

a

= 0.0-4.0 Distance = 0.5-1.5 pc (location of the ejecta filaments in 3D models of Cadez et al. 2004)Qabs

 silicates, carbon (

Zubko et al. 2004), carbon (

Rouleau & Martin 1991)Slide8

Silicates: Carbon:

a = 3.5 a = 4.0 amax > 0.6 mm amax

> 0.1 mmBest-fit parameters:C2 Contours (amax vs.

a

)

Temim &

Dwek

2013

Size distribution index of 3.5-4.0 and larger grain size cut-offs are favored

Larger grains are consistent with a Type IIP SN

– Mass

dominated by grains with radii larger than 0.03

μm

in Type IIP, and less than 0.006

μm

in Type

IIb

SNe

(

Kozasa,Nozawa

et al. 2009)

Md = 0.13 +/- 0.01 M for silicates

M

d = 0.02 +/- 0.04 M

for carbonSlide9

Late Evolution – Interaction with the Reverse ShockSlide10

Composite SNR with a

shell and an off-center pulsar wind nebula

Complex morphology likely produced by a combination of an asymmetric reverse shock and the pulsar’s motionTemi

m et al. 2009MOST Radio, ATCA Radio, ChandraSNR ShellRadio PWNNeutron Star

X-ray PWN

Outflow – bubble?

Reverse Shock Interaction: G327.1-1.1

Sedov

model (for

d

= 9

kpc

):

R

= 22

pc n

0

= 0.12 cm

-

3

t

= 1.8

x

10

4

yr

M

tot

= 31

M

sol

T

=

0.3

keV

v

s

= 500 km/

sSlide11

A compact

core

is embedded in a cometary PWN Prong-like structures originate from the vicinity of the core and extend to the NW – outflow from the pulsar wind?

350 ks Chandra observationGaensler et al. 2004ProngsCometary PWN

Compact PWN

Trail

Compact PWN is more extended than a point source

G327.1-1.1: X-ray Morphology

Two possible scenarios may give rise to

cometary

structure:

Asymmetric passage of the reverse shock from the NW – PWN expanding

subsonically

Bow shock formation due to pulsar’s motion in the NW direction



p

ulsar velocity ~ 770 km/

s

Temi

m et al. 2009, 2014 (in prep)Slide12

RS Interaction: MSH 15-56

X-ray

,

RadioChandra X-rayXMM3-colorimageTemim et al. 2013Sedov model (for

d

= 4

kpc

):

R

=

21 pc n

0

=

0.1

cm

-

3

t

=

16.5 kyr Mtot

= 100 Msol T =

0.3 keV vs = 500 km/sPulsar velocity = 410 km/

sSlide13

Composite SNRs serve as unique laboratories for the study of SNR/PWN evolution

Interaction of the PWN with the SNR and surroundings Properties of progenitor, pulsar, SN ejecta, freshly formed SN dust Nature and evolution of energetic particles in PWNe Evolution can be divided into three stages Expansion of the PWN into cold SN ejecta (ejecta and dust properties, mass, dynamics, progenitor type)

Interaction with the SNR reverse shock (complex morphologies and mixing of PWN with ejecta) Post-reverse shock, subsonic expansion (bow shock formation if pulsar is moving at a high velocity)SummaryCollaborators: Patrick Slane (CfA) Eli Dwek (GSFC) George Sonneborn (GSFC) Richard Arendt (GSFC)

Yosi

Gelfand

(

NYU Abu Dhabi)

Paul

Plucinsky

(CfA)

Daniel Castro (MIT)Slide14