A numerical simulation of the evolution and fate of a Fanaroff-Riley type I jet. The case of 3C 31

Perucho, M.; Martí, Juan José Ibàñez

doi:10.1111/j.1365-2966.2007.12454.x

Cited by 157 publications

(172 citation statements)

References 43 publications

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“…The code and initial setup is similar to that of Perucho & Martí (2007). We performed two simulations, one with a one-sided jet (M1) and a second one with a two-sided jet (M2), by changing the boundary conditions at the inlet.…”

Section: Discussionmentioning

confidence: 99%

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VLBI-selected sample of compact symmetric object candidates and frequency-dependent position of hotspots

Sokolovsky¹,

Kovalev²,

Pushkarev³

et al. 2011

A&A

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Context. The compact symmetric objects (CSOs) are small (<1 kiloparsec) and powerful extragalactic radio sources showing emission on both sides of an active galactic nucleus and no signs of strong relativistic beaming. They may be young radio sources, progenitors of large FR II radio galaxies. Aims. We aim to study the statistical properties of CSOs by constructing and investigating a new large sample of CSO candidates on the basis of dual-frequency, parsec-scale morphology. Methods. For the candidate selection we utilized VLBI data for 4170 extragalactic objects obtained simultaneously at 2.3 and 8.6 GHz (S and X band) within the VLBA Calibrator Survey 1-6 and the Research and Development -VLBA projects. Properties of their broad-band radio spectra were characterized by using RATAN-600 observations. Numerical modeling was applied in an attempt to explain the observed effects. Results. A sample of 64 candidate CSOs is identified. The median two-point S -X band spectral index of parsec-scale hotspots is found to be −0.52; with the median brightness temperature ∼10 9 K at X band. Statistical analysis reveals a systematic difference between positions of brightest CSO components (associated with hotspots) measured in the S and X bands. The distance between these components is found to be on average 0.32 ± 0.06 mas greater at 8.6 GHz than at 2.3 GHz. Conclusions. This difference in distances cannot be explained by different resolutions at the S and X bands. It is a manifestation of spectral index gradients across CSO components, which may potentially provide important physical information about them. Despite our detailed numerical modeling of a CSO hotspot, the model was not able to reproduce the magnitude of the observed positional difference. A more detailed modeling may shed light on the origin of the effect. Multifrequency follow-up VLBI observations of the selected sample are needed to confirm and study newly identified CSOs from the list presented here.

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Section: Discussionmentioning

confidence: 99%

“…The jet composition is purely leptonic and the external medium is composed of the neutral hydrogen. We assume the profile of the external medium in a typical radio galaxy like 3C 31 (Perucho & Martí 2007;Hardcastle et al 2002).…”

Section: Discussionmentioning

confidence: 99%

VLBI-selected sample of compact symmetric object candidates and frequency-dependent position of hotspots

Sokolovsky¹,

Kovalev²,

Pushkarev³

et al. 2011

A&A

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“…To determine the radius of the bow-shock, r b , we assume a self-similar relationship between its length and width given by R ≡ l b /r b , which can vary from source to source in the range R ∈ [2 − 3] (see Leahy et al 1989;Kaiser et al 2004;Perucho & Martí 2007). Here, we use a fiducial value of R = 3 (similar to the value from our simulations; see Appendix A).…”

Section: Bow-shockmentioning

confidence: 99%

Non-thermal emission from microquasar/ISM interaction

Bordas¹,

Bosch‐Ramon

Paredes³

et al. 2009

A&A

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Context. The interaction of microquasar jets with their environment can produce non-thermal radiation as in the case of extragalactic outflows impacting on their surroundings. Significant observational evidence of jet/medium interaction in galactic microquasars has been collected in the past few years, although little theoretical work has been done regarding the resulting non-thermal emission. Aims. In this work, we investigate the non-thermal emission produced in the interaction between microquasar jets and their environment, and the physical conditions for its production. Methods. We developed an analytical model based on those successfully applied to extragalactic sources. The jet is taken to be a supersonic and mildly relativistic hydrodynamical outflow. We focus on the jet/shocked medium structure in its adiabatic phase, and assume that it grows in a self-similar way. We calculate the fluxes and spectra of the radiation produced via synchrotron, inverse Compton, and relativistic bremsstrahlung processes by electrons accelerated in strong shocks. A hydrodynamical simulation is also performed to investigate further the jet interaction with the environment and check the physical parameters used in the analytical model. Results. For reasonable values of the magnetic field, and using typical values of the external matter density, the non-thermal particles could produce significant amounts of radiation at different wavelengths, although they do not cool primarily radiatively, but by adiabatic losses. The physical conditions of the analytical jet/medium interaction model are consistent with those found in the hydrodynamical simulation. Conclusions. Microquasar jet termination regions could be detectable at radio wavelengths for current instruments sensitive to ∼arcminute scales. At X-ray energies, the expected luminosities are moderate, although the emitter is more compact than the radio one. The source may be detectable by XMM-Newton or Chandra, with 1-10 arcsec of angular resolution. The radiation at gamma-ray energies may be within the detection limits of the next generation of satellite and ground-based instruments.

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“…Since there are no clear signatures of a reverse shock (Bordas et al 2009) in this source and only the shocked ISM thermal radiation is detected, it may be that the Cygnus X-1 jet head is fully disrupted. A shock driven in the ISM can still develop in such a conditions since the disrupted jet region has much higher pressure than the environment, as simulations of jets of FRI radio galaxies show (Perucho & Martí 2007; see also Bordas et al 2011).…”

Section: The Physical Picturementioning

confidence: 99%

The termination region of high-mass microquasar jets

Bosch‐Ramon

Perucho

Bordas

2011

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Context. The environment of high-mass X-ray binaries can be characterized either by the supernova remnant that forms these systems or by the wind from the companion massive star. These regions should be tenuous but very hot and surrounded by a dense and cold shocked ISM shell. The interaction between the jet and such a complex medium, also affected by the system proper motion, can lead to very different jet termination structures. Aims. The evolution of the jet termination regions during the life of a high-mass microquasar is simulated to improve our present understanding of these structures. Also, the evolving emission characteristics are modeled to inform potential observational campaigns of this class of object. Methods. We performed 2D numerical simulations of jets propagating in different scenarios, corresponding to different epochs after the formation of the high-mass X-ray binary, using the code Ratpenat. We also made simple estimates of the nonthermal emission that could be produced in the jet termination regions. Results. We find that, in the way through the hot and tenuous medium of the shocked wind/supernova ejecta, the jet suffers recollimation shocks in which it loses part of its thrust and ends in a strong shock inflating a hot cocoon. The jet head propagates with a speed that is similar to the medium sound speed, until it eventually reaches the denser and colder shocked ISM and the unperturbed ISM later on. In these last stages of evolution, the jet is significantly slowed down and can be disrupted. For relatively old sources, the microquasar peculiar velocity becomes important, leading to complete jet destruction. Extended nonthermal radiation can be generated in the jet termination regions, and hard X-rays and TeV photons are the wavelengths best suited for observing these structures.

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A numerical simulation of the evolution and fate of a Fanaroff-Riley type I jet. The case of 3C 31

Cited by 157 publications

References 43 publications

VLBI-selected sample of compact symmetric object candidates and frequency-dependent position of hotspots

VLBI-selected sample of compact symmetric object candidates and frequency-dependent position of hotspots

Non-thermal emission from microquasar/ISM interaction

The termination region of high-mass microquasar jets

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