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Non-Thermal Emission from Galactic Jets Valent Bosch-Ramon Dublin - - PowerPoint PPT Presentation

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Non-Thermal Emission from Galactic Jets Valent Bosch-Ramon Dublin Institute for Advanced Studies High Energy Phenomena in Relativistic Outflows III Barcelona, Catalonia (Spain) 27/06/2011-01/07/2011 V. Bosch-Ramon (DIAS) Non-Thermal

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Non-Thermal Emission from Galactic Jets

Valentí Bosch-Ramon

Dublin Institute for Advanced Studies High Energy Phenomena in Relativistic Outflows III Barcelona, Catalonia (Spain) 27/06/2011-01/07/2011

  • V. Bosch-Ramon (DIAS)

Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 1 / 32

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SLIDE 2

Outline

1

Introduction

2

Some phenomenology

3

Basic non-thermal physics

4

Emitting sites

5

Final remarks

  • V. Bosch-Ramon (DIAS)

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SLIDE 3

Outline

1

Introduction

2

Some phenomenology

3

Basic non-thermal physics

4

Emitting sites

5

Final remarks

  • V. Bosch-Ramon (DIAS)

Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 3 / 32

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Galactic Jets: microquasars, ...

Microquasars are binary systems harboring a normal star and an accreting compact object, from which jets are produced.

(Mirabel & Rodríguez 1999) Do we include Young Stellar Objects?

  • V. Bosch-Ramon (DIAS)

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SLIDE 5

Outline

1

Introduction

2

Some phenomenology

3

Basic non-thermal physics

4

Emitting sites

5

Final remarks

  • V. Bosch-Ramon (DIAS)

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SLIDE 6

Non-thermal emission from microquasars

Persistent flat radio emission, sometimes extended at mas scales, is detected.

(e.g. Fender 2001, Stirling et al. 2001)

Radio blobs with ∼ 1”-size are observed after X-ray state changes.

(e.g. Mirabel & Rodríguez 1994, Martí et al. 2001, Fender et al. 2004)

  • V. Bosch-Ramon (DIAS)

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Microquasars at radio wavelengths

Compact and continuous jets versus extended transient ejections:

Cyg X-1: Stirling et al. (2001) Cyg X-3: Martí et al. (2001)

See also, e.g., Ribó (2005).

  • V. Bosch-Ramon (DIAS)

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Non-thermal emission from microquasars

Persistent flat radio emission, sometimes extended at mas scales, is detected.

(e.g. Fender 2001, Stirling et al. 2001)

Radio blobs with ∼ 1”-size are observed after X-ray state changes.

(e.g. Mirabel & Rodríguez 1994, Martí et al. 2001, Fender et al. 2004)

X-rays are typically of thermal accretion origin,

(e.g. Shakura & Sunyaev 1973)

although non-thermal radiation may be also contributing.

(e.g. Bisnovatyi-Kogan & Blinnikov 1976, Akharonian et al. 1985, Gierlinski et al. 1999)

  • V. Bosch-Ramon (DIAS)

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X-rays

Power-law tails; e.g. a non-thermal component beyond X-rays in Cyg X-1

(McConnell et al. 2002)

  • V. Bosch-Ramon (DIAS)

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Non-thermal emission from microquasars

Persistent flat radio emission, sometimes extended at mas scales, is detected.

(e.g. Fender 2001, Stirling et al. 2001)

Radio blobs with ∼ 1”-size are observed after X-ray state changes.

(e.g. Mirabel & Rodríguez 1994, Martí et al. 2001, Fender et al. 2004)

X-rays are typically of thermal accretion origin, although non-thermal radiation may be also contributing.

(e.g. Shakura & Sunyaev 1973, Bisnovatyi-Kogan & Blinnikov 1976, Akharonian et al. 1985, Gierlinski et al. 1999)

Gamma rays have been detected from microquasars, likely from the jet at its base (MeV) and at binary scales (GeV–TeV).

(e.g. McConnell et al. 2002, Tavani et al. 2009, Abdo et al. 2009a, Sabatini et al. 2010)

  • V. Bosch-Ramon (DIAS)

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γ-rays from microquasars: Cyg X-3

Multiwavelength behavior of Cyg X-3 when active in GeV

(Abdo et al. 2009a, Aleksic et al. 2010, Williams et al. 2011; see also Tavani et al. 2009)

  • V. Bosch-Ramon (DIAS)

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γ-rays from microquasars: Cyg X-1

Detections at ∼ 4 − 5 σ of Cyg X-1 in GeV-TeV in the hard state

AGILE: MAGIC:

(Sabatini et al. 2010) (Albert et al. 2007)

  • V. Bosch-Ramon (DIAS)

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γ-rays from microquasars: candidates

LS 5039 and LS I +61 303: (Abdo et al. 2009b, 2009c, Aharonian et al. 2006, Albert et al. 2009)

Plus two more sources: HESS J0632+057; 1FGL J1018.6−5856 (Hinton et al. 2009, Falcone et al. 2011; Corbet et al. 2011)

  • V. Bosch-Ramon (DIAS)

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Non-thermal emission from microquasars

Persistent flat radio emission, sometimes extended at mas scales, is detected.

(e.g. Fender 2001, Stirling et al. 2001)

Radio blobs with ∼ 1”-size are observed after X-ray state changes.

(e.g. Mirabel & Rodríguez 1994, Martí et al. 2001, Fender et al. 2004)

X-rays are typically of thermal accretion origin, although non-thermal radiation may be also contributing.

(e.g. Shakura & Sunyaev 1973, Bisnovatyi-Kogan & Blinnikov 1976, Akharonian et al. 1985, Gierlinski et al. 1999)

Gamma rays have been detected from microquasars, likely from the jet at its base (MeV) and at binary scales (GeV–TeV).

(e.g. McConnell et al. 2002, Tavani et al. 2009, Abdo et al. 2009a, Sabatini et al. 2010)

The jet termination region is also a non-thermal emitter.

(e.g. Mirabel et al. 1992, Safi-Harb & Petre 1999, Corbel et al. 2002, Tudose et al. 2006)

  • V. Bosch-Ramon (DIAS)

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Jet medium interactions

Cyg X-1 interacting with the ISM(Gallo et al. 2005) Jet/SNR interactions in SS 433(Dubner et al. 1998) Ejecta/medium shocks in XTE J1550−564(Corbel et al. 2002)

  • V. Bosch-Ramon (DIAS)

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Outline

1

Introduction

2

Some phenomenology

3

Basic non-thermal physics

4

Emitting sites

5

Final remarks

  • V. Bosch-Ramon (DIAS)

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Basics: acceleration, transport and work

Particle transport due to jet advection and particle diffusion takes place.

Diffusion time: tBohm ≈ 15 R2

j 10 B10 G E−1 TeV s

Advection time: tadv = 10 zj 11/vj 10 s

Adiabatic cooling is likely relevant, and can dominate the whole NT population.

Adiabatic cooling: tad ∼ 10 (Rj 10/vexp 9) s

The timescale of the acceleration process can be roughly characterized through ηacc rg/c with ηacc > 1.

Acceleration time: tacc ≈ 10−2 ηacc ETeV B−1

10 G s

(Protheroe 1999) (Fermi processes: e.g. Bell 1978a, 1978b; Drury 1983; see also Rieger et al. 2007) (Perucho et al. 2010)

  • V. Bosch-Ramon (DIAS)

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Basics: radiation processes

Relativistic particles cool through synchrotron and IC emission.

Stellar IC scattering: tcool ≥ 12 u−1

100 E−1 10 GeV s

Synchrotron emission: tsync ≈ 400 B−2

10 G E−1 10 GeV s

Relativistic Bremsstrahlung and coulombian cooling could be relevant in the jet base.

Relativistic Bremsstrahlung: tbr ∼ 106 n−1

9

s Ionization cooling: tion ∼ 3 × 104 E10 MeV n−1

9

s

Hadronic processes:

pp interactions: tpp ≈ 106 n−1

9

s

Photomeson production, and even photodisintegration, cannot be discarded, but require more extreme conditions: very dense radiation and matter fields, and very high p/nuclei energies. (see Bosch-Ramon & Khangulyan 2009 and references therein)

  • V. Bosch-Ramon (DIAS)

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Basics: Non-thermal modeling

Complex sources: particle transport, orbital motion, geometrical effects in IC and gamma-ray absorption, modulated adiabatic losses... Modeling hints at B, emitter location, Lnt, ηacc, adiabatic losses... But, the detailed physics and even the engines are yet unknown. →

High-quality data+simulations

e.g. LS 5039: Takahashi et al. (2009)

  • V. Bosch-Ramon (DIAS)

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Basics: Gamma-ray absorption and reprocessing

In systems with τγγ ∼ 0.5 L∗38 d−1

∗12.5 1,

> 30 GeV gamma rays will be absorbed. Energy can end up as secondary synchrotron radio and X-ray radiation, or IC gamma rays.

(e.g. B.-R. et al. 2008; B.-R. & Khangulyan 2011) E-M cascades in binary systems: Bednarek 2000; Aharonian et

  • al. (2006); Orellana et al. (2007); Khangulyan et al. (2008);

Sierpowska-Bartosik & Torres (2008); Cerutti et al. (2010)

  • V. Bosch-Ramon (DIAS)

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Outline

1

Introduction

2

Some phenomenology

3

Basic non-thermal physics

4

Emitting sites

5

Final remarks

  • V. Bosch-Ramon (DIAS)

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Accretion and jet formation

In the jet base/corona, B-reconnection, recollimation and internal shocks can take place.

(Komissarov et al. 2007, Barkov & Komissarov 2008)

  • V. Bosch-Ramon (DIAS)

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Non-thermal emission

Reconnection or shocks can accelerate particles.

(e.g. Pineault 1982; Spruit 1988; Gouveia dal Pino & Lazarian 2005; Polko et al. 2010)

Different leptonic (rel. Bremss., synchrotron, IC) and hadronic (pp, pγ) models for non-thermal emission have been proposed. The role of pair creation cannot be neglected.

See, e.g.: Akharonian et al. (1985), Levinson et al. (2001); Markoff et al. (2001); Georganopoulos et al. (2002);; Romero & Vila (2008); Belmont (2008); Vurm & Poutanen (2009); Vieyro et al. 2010 (Bosch-Ramon et al. 2006)

  • V. Bosch-Ramon (DIAS)

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Binary system scales: stellar wind-jet hydrodynamics

The jet interacts with the dense (inhomogeneous) stellar wind suffering a strong (asymmetric) recollimation shock, turbulence, and possibly disruption.

(Perucho & Bosch-Ramon, in prep) (Perucho et al. 2010)

  • V. Bosch-Ramon (DIAS)

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Non-thermal emission

Synchrotron and inverse are the most efficient processes, although in dense wind sources pp may be efficient. Free-free and photo-electric absorption of radio and X-rays in the wind. γγ → e± emission

See also, e.g.: Paredes et al. (2000); Romero et

  • al. (2003); Bosch-Ramon & Paredes (2004);

Aharonian et al. (2006); Orellana et al. (2007); Bednarek & Giovannelli (2007); Perucho & Bosch-Ramon (2008); Khangulyan et al. (2008); Bosch-Ramon (2009,2010); Dubus et al. (2010) (Paredes et al. 2006)

Very inhomogeneous winds imply a specific phenomenology and physical processes.

(Owocki et al. 2009; Araudo, Bosch-Ramon & Romero 2009)

  • V. Bosch-Ramon (DIAS)

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Jet intermediate scales...

Powerful ejections can produce non-thermal emission far from the binary. Instabilities, weak shocks

  • r shear layers can lead to

extended non-thermal emission.

(e.g. Aharonian & Atoyan 1999; Rieger et al. 2007) (Martí et al. 2001)

  • V. Bosch-Ramon (DIAS)

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The jet termination

Low-mass microquasars likely propagate in hot diluted media.

(e.g. Heinz 2002)

High-mass microquasars have to cross the SNR or the stellar wind blown structure.

(Bosch-Ramon et al. 2011; regarding SS 433, see, e.g., Velázquez & Raga 2000)

The jet/ISM shock goes through free propagation, adiabatic and radiative phases. The jet can suffer a strong recollimation shock. Recollimation, reverse, and forward shock: possible accelerators. Non-thermal and thermal emission is produced in the termination region.

(e.g. Bordas et al. 2009)

  • V. Bosch-Ramon (DIAS)

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The jet termination dynamics

Depending on the source age, the environment can differ strongly, and so the impact on the jet.

HMMQ with proper motion: Bosch-Ramon et al. (2011) ISM: Bordas et al. (2009)

  • V. Bosch-Ramon (DIAS)

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Non-thermal emission

Recollimation, reverse and forward shocks can be effective high energy emitters. Radio-to-gamma ray emission may be eventually detected.

See also, e.g.: Kaiser et al 2000; Heinz & Sunyaev (2002); Wang et al. (2003); Bosch-Ramon et al. (2005) (Bordas et al. 2009)

  • V. Bosch-Ramon (DIAS)

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Other galactic jets: young stellar objects

Non-thermal radio emission have been detected from MYSO. Jets and their termination regions may produce high-energy emission.

(e.g. Crusius-Watzel 1990; Henriksen et al. 1991; Araudo et al. 2007, 2008; Romero et al. 2010; Parkin et

  • al. 2010; Bosch-Ramon et al. 2010)

e.g. IRAS 16547−4247:

(Carrasco-González et al. 2010)

  • V. Bosch-Ramon (DIAS)

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Outline

1

Introduction

2

Some phenomenology

3

Basic non-thermal physics

4

Emitting sites

5

Final remarks

  • V. Bosch-Ramon (DIAS)

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Concluding...

The corona and the jet base can be an efficient gamma-ray emitter (attenuation!). At binary scales (HMMQ), the jet and its environment is an efficient radio-to-gamma ray emitter (attenuation!). Large scale jets can still produce radiation, but new ejections are more efficient particle accelerators. Jet termination regions are non-thermal emitters and may be eventually detected in gamma-rays (like Cen A radio lobes!).

Keep an eye on Massive YSOs jets as potential high-energy sources.

  • V. Bosch-Ramon (DIAS)

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