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

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

Outline Introduction 1 Some phenomenology 2 Basic non-thermal physics 3 Emitting sites 4 Final remarks 5 V. Bosch-Ramon (DIAS) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 2 / 32

Outline Introduction 1 Some phenomenology 2 Basic non-thermal physics 3 Emitting sites 4 Final remarks 5 V. Bosch-Ramon (DIAS) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 3 / 32

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) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 4 / 32

Outline Introduction 1 Some phenomenology 2 Basic non-thermal physics 3 Emitting sites 4 Final remarks 5 V. Bosch-Ramon (DIAS) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 5 / 32

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) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 6 / 32

Microquasars at radio wavelengths Compact and continuous jets versus extended transient ejections: Cyg X-3: Martí et al. (2001) Cyg X-1: Stirling et al. (2001) See also, e.g., Ribó (2005). V. Bosch-Ramon (DIAS) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 7 / 32

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) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 8 / 32

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) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 9 / 32

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) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 10 / 32

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) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 11 / 32

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) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 12 / 32

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) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 13 / 32

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) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 14 / 32

Jet medium interactions Jet/SNR interactions in SS 433(Dubner et al. 1998) Ejecta/medium shocks in XTE J1550 − 564(Corbel et al. 2002) Cyg X-1 interacting with the ISM(Gallo et al. 2005) V. Bosch-Ramon (DIAS) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 15 / 32

Outline Introduction 1 Some phenomenology 2 Basic non-thermal physics 3 Emitting sites 4 Final remarks 5 V. Bosch-Ramon (DIAS) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 16 / 32

Basics: acceleration, transport and work Particle transport due to jet advection and particle diffusion takes place. j 10 B 10 G E − 1 Diffusion time: t Bohm ≈ 15 R 2 TeV s Advection time: t adv = 10 z j 11 / v j 10 s Adiabatic cooling is likely relevant, and can dominate the whole NT population. Adiabatic cooling: t ad ∼ 10 ( R j 10 / v exp 9 ) s The timescale of the acceleration process can be roughly characterized through η acc r g / c with η acc > 1. Acceleration time: t acc ≈ 10 − 2 η acc E TeV B − 1 10 G s (Protheroe 1999) (Perucho et al. 2010) (Fermi processes: e.g. Bell 1978a, 1978b; Drury 1983; see also Rieger et al. 2007) V. Bosch-Ramon (DIAS) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 17 / 32

Basics: radiation processes Relativistic particles cool through synchrotron and IC emission. Stellar IC scattering: t cool ≥ 12 u − 1 100 E − 1 10 GeV s Synchrotron emission: t sync ≈ 400 B − 2 10 G E − 1 10 GeV s Relativistic Bremsstrahlung and coulombian cooling could be relevant in the jet base. Relativistic Bremsstrahlung: t br ∼ 10 6 n − 1 s 9 Ionization cooling: t ion ∼ 3 × 10 4 E 10 MeV n − 1 s 9 Hadronic processes: pp interactions: t pp ≈ 10 6 n − 1 s 9 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) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 18 / 32

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, L nt , η acc , 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) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 19 / 32

Basics: Gamma-ray absorption and reprocessing In systems with τ γγ ∼ 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) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 20 / 32

Outline Introduction 1 Some phenomenology 2 Basic non-thermal physics 3 Emitting sites 4 Final remarks 5 V. Bosch-Ramon (DIAS) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 21 / 32

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) Non-Thermal Emission from Galactic Jets 27/06/2011-01/07/2011 22 / 32