Thermal non thermal plasma interactions in clusters
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Thermal / Non-thermal plasma Interactions in Clusters. The Good, the Bad & the Puzzling. L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100. The BIG Questions. • How can relativistic plasmas, seen through synchrotron radiation, reveal the dynamics and evolution of clusters?

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Thermal / Non-thermal plasma Interactions in Clusters

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Thermal non thermal plasma interactions in clusters

Thermal / Non-thermal plasmaInteractions in Clusters

The Good, the Bad & the Puzzling

L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100


The big questions

The BIG Questions

• How can relativistic plasmas, seen through synchrotron radiation, reveal the dynamics and evolution of clusters?

SYNCHROTRON, clues to  DYNAMICS ?

• How does the dynamics of the thermal plasma affect the growth of the magnetic field and the acceleration of relativistic particles?

DYNAMICS causes  B field and CRs ?

L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100


Key messages

GOOD NEWS: хорошие новости

• AGN influences on thermal X-ray plasma are well

documented (heating, cavities, etc)

• Shocks seen in radio, sometimes in X-ray & S-Z, are consistent

with expectations from theory, connected to cluster mergers

• Radio halos likely result from expected turbulence in mergers

Key Messages

ЮрийНикулин

BAD NEWS:плохиеновости

• Mach numbers expected from simulations and measured in X-ray inconsistent with spectral index of radio emission.

• Missing shocks, either radio or X-ray

PUZZLING NEWS: головоломки

• Mild mergers with no shocks also produce giant radio halos.

• 3D structure of giant shock in Abell 2256 is not simple to explain

• Radio galaxies sometimes seen at edge of shocks – why?

Max Otto von Stierlitz

Максим Максимович Исаев

L. Rudnick MN Inst. for Astrophysics Zeldovich 100

with support from U.S. NSF, AST112195


The good news

The GOOD News

PASSIVE

ACTIVE

Radio galaxy  ICM interactions

L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100


The good news1

The GOOD News

Vazza et al. 2012, MNRAS 421 1868

• Merger shocks:

simulations and observed relics

L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100


The good news2

Keeping electrons energized: CRe lifetimes ~ 108 yCRediffusion times ~ 1010 y

The GOOD News

Merger-driven turbulence

W. Couch

M. Owers

L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100


The good news3

Halos

DISTURBED

The GOOD News

Cassano+ 2011

• Radio halos 

mergers

RELAXED

L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100


The good news4

Consistent shock story - Radio, X-ray, S-Z

X-RAY

A. Simionescu et al. 2013 ApJ 775 4

The GOOD News

RADIO

S-Z

Brown & Rudnick, 2011

Planck intermediate results. X. Physics of

the hot gas in the Coma cluster, 2013

L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100


Thermal non thermal plasma interactions in clusters

The BAD News

Mismatched Mach numbers ?

X-ray shock

Ogrean+2013

ainj=

-0.6 to -0.7

X-ray shock

radio spectrum

M < 2

3.3 < M < 4.6

van Weeren+ 12

radio spectrum


Thermal non thermal plasma interactions in clusters

The BAD News

Do shocks look too efficient?

Tension with g-ray limits?


Thermal non thermal plasma interactions in clusters

The BAD News

X-ray shock

Radio shock

Why the

offset?

Where’s the

radio shock?


The puzzling news

The PUZZLING News

Exploring

low surface brightness

radio emission

PUZZLING

головоломки

Farnsworth+2013

L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100


Can mild mergers giant radio halos

The PUZZLING News

Can MILD mergers  Giant Radio Halos?

X-Ray

RADIO

Rossetti+ 2013

Abell 2142

Farnsworth+ 2013


Abell 2256 where s the shock

The PUZZLING News

Abell 2256 – where’s the shock?

Radio

X-ray

with F. Owen, NRAO & J. Eilek, NMIMT


Abell 2256 where s the shock1

The PUZZLING News

Abell 2256 – where’s the shock?

Flat spectrum

Steep spectrum

with F. Owen, NRAO & J. Eilek, NMIMT


Thermal non thermal plasma interactions in clusters

The PUZZLING News

Radio Galaxy – relic/shock connection?

van Weeren+ 2010

Bonafede+14

Pizzo+2010


Key messages1

GOOD NEWS: хорошие новости

• AGN influences on thermal X-ray plasma are well

documented (heating, cavities, etc)

• Shocks seen in radio, sometimes in X-ray & S-Z, are consistent

with expectations from theory, connected to cluster mergers

• Radio halos likely result from expected turbulence in mergers

Key Messages

ЮрийНикулин

BAD NEWS:плохиеновости

• Mach numbers expected from simulations and measured in X-ray inconsistent with spectral index of radio emission.

• Missing shocks, either radio or X-ray

PUZZLING NEWS: головоломки

• Mild mergers with no shocks also produce giant radio halos.

• 3D structure of giant shock in Abell 2256 is not simple to explain

• Radio galaxies sometimes seen at edge of shocks – why?

Max Otto von Stierlitz

Максим Максимович Исаев

L. Rudnick MN Inst. for Astrophysics Zeldovich 100

with support from U.S. NSF, AST112195


Thermal non thermal plasma interactions in clusters

radio.galaxyzoo.org


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