particle acceleration and magnetic fields:looking at the nw rim of rcw 86 withchandrasne-grb workshop
kyoto
oct 2013

daniel castro - mitcollaboratorslaura lopez – mit
pat slane – cfa
hiroya yamaguchi – cfa*
enrico ramirez-ruiz – ucsc
enectali figueroa-feliciano – mit
special credit to joe depasquale at cxc for
imaging help

outline
what evidence is there that SNRs acceleratecosmic rays?
how does the magnetic field get amplified? andhow do we know it does?
what have we learnt studying rcw 86 withchandra?

0. primer: what are snrs?
• explosive end of a star
• two types:ocore-collapse
othermonuclear• material ejected with~1051 erg kinetic
energy• shock wave forms &sweeps up ISM/CSM
warren+ 2005

0. primer: what are snrs?

e.g. caprioli 2012

i.

evidence

what evidence is there that SNRs acceleratecosmic rays?

i.

evidence••••

non-thermal X-rays
ɣ-ray emission
dynamical properties
structure

koyama+ 1995

keVi.

TeV

evidencevela jr.

••••

non-thermal X-rays
ɣ-ray emission
dynamical properties
structurerx j1713.7-3936

rcw 86hinton & hofmann 2009uchiyama+ 2002
aschenbach 1998
vink+ 2006
aharonian+ 2006, 2007,2008
naumann-godo+ 2006

sn 1006

i.

evidence••••

non-thermal X-rays
ɣ-ray emission
dynamical properties
structure

LAT SNR catalog (sometime in the next 12 months)

i.

evidence••••

non-thermal X-rays
ɣ-ray emission
dynamical properties
structurehughes+ 2000

evidence••••

non-thermal X-rays
ɣ-ray emission 1 10
dynamical properties
structuredensity (g.cm-3)

x1

age = 1000 yr

-24

0.1

1x10-250.01
1x10-26
4

56

radius (pc)

78

number density (cm-3)

i.

i.

evidence••••

non-thermal X-rays
ɣ-ray emission
dynamical properties
structure

warren+ 2005

i.

evidence••••

non-thermal X-rays
ɣ-ray emission
dynamical properties
structure

warren+ 2005
warren+ 2005

i.

evidence

•
•
•
•
•

non-thermal X-rays
ɣ-ray emission
dynamical properties
structure
non-thermal X-rays

uchiyama+ 2007

ii. magnetic field amplification
how does the magnetic field get amplified? andhow do we know it does?

ii. magnetic field amplification
how.resonant cosmic ray streaming instability e.g.
zirakashvili 2000

.bell’s non-resonant instability bell 2004
.non-resonant long-wavelength instability bykov & toptygin
2005.others…

ii. magnetic field amplification
evidence.spectral curvature in radio emission (a littleiffy).broad-band fits of synchrotron emission
between radio and non-thermal X-rays.rapid variability of nonthermal X-ray
emission from bright filaments in SNRs
.sharp X-ray edges

ii. magnetic field amplification
evidence.spectral curvature in radio emission (a littleiffy).broad-band fits of synchrotron emission
between radio and non-thermal X-rays.rapid variability of nonthermal X-ray
emission from bright filaments in SNRs
.sharp x-ray edges

ii. magnetic field amplification.sharp x-ray edges

bamba et al.
2005

ii. magnetic field amplification.sharp x-ray edges

vink 2006

vink et al. 2006

ii. magnetic field amplification.sharp x-ray edges

vink 2006

actually helder+ 2013 find vs~700-2000 km/s

vink et al. 2006

iii. rcw 86

what have we learnt studying rcw 86 withchandra?

iii. rcw 86

red: spitzer 24 microns(wise 22 microns)chandra and xmm
green:0.5-1.95 keV
blue: 1.95-6.8 keV

x-ray: nasa/cxc/sao & esa; infared: nasa/jpl-caltech/b. williams (ncsu)

iii. rcw 86

chandra and xmm
red: 0.5 - 1 keVgreen: 1.5 - 2 keV
blue: 2 - 8 keV

iii. rcw 86

10´
magenta 0.3 - 0.75 keV
blue
1.5 - 7.0 keV

0.1Flux (counts s-1 keV-1)

0.01

0.001

0.0001
0.5

15Energy (keV)
0.1

Flux (counts s-1 keV-1)

Region B

0.01

0.001

0.0001
0.515

Energy (keV)

Flux (counts s-1 keV-1)

Region C
0.01

0.001

0.0001
0.5

15Energy (keV)

Region D
Flux (counts s-1 keV-1)

iii. rcw 86

Region A

0.1

0.01

0.001

0.00010.5

15Energy (keV)

iii. rcw 86

iii. rcw 86
from Bamba+ 2003

iii. rcw 86
advectiondiffusion

joint

iii. rcw 86

ghavamian et al.
2001iii. rcw 86: next step
chandra obs

chandra obs

chandra obs

the end.thin nonthermal x-ray rims observed in thenw of rcw 86.high magnetic fields derived using filament
widths.shock velocity derived from balmer line
profiles (optical observations) appears toolow