Study of relativistic magnetized outflows with relativistic equation of state

Singh, Kuldeep; Chattopadhyay, Indranil

doi:10.1093/mnras/stz2101

Cited by 4 publications

(3 citation statements)

References 40 publications

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“…In addition, the Maxwell's equations, the ideal MHD condition and the gas EoS (equation 2.8) were used to solve the above equations of motion. We showed that the solutions depend on a large number of parameters [26]. In Fig.…”

Section: Pos(hepro Vii)007mentioning

confidence: 76%

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Relativistic Jets From Black Hole Accretion Disc

Chattopadhyay¹,

Vyas²,

Singh³

2020

Proceedings of High Energy Phenomena in Relativistic Outflows VII — PoS(HEPRO VII)

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Astrophysical jets from AGNs and microquasars are often relativistic and collimated. We study magnetic and radiative driving of jets to address these issues. The plasma is described by a relativistic equation of state which depends on the composition. We show that the matter content may not affect the streamline of magnetically driven jets, but the poloidal velocity and temperature distribution strongly depend on the composition of the jet. We also discuss the salient features of radiatively driven jets. Although consensus in the community precludes radiation driving to be an effective acceleration mechanism, we show that it is certainly not the case. For black holes surrounded by luminous discs, jets may be accelerated up to Lorentz factors of ∼ a few for baryon dominated jets. Interestingly, the terminal Lorentz factor may reach to a value of a few tens for lepton dominated jets. We also show that internal shocks driven by radiation are also possible in jets. Moreover, a temperature dependent scattering cross-section can produce relativistic jets that are launched with very low speeds and quite moderate temperatures, conditions which are expected in the inner region of the accretion discs. Although we have studied magnetic driving and radiative driving separately, it is apparent that both processes should be incorporated in order to solve the collimation and acceleration enigma of astrophysical jets. High Energy Phenomena in Relativistic Outflows VII -HEPRO VII

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Section: Pos(hepro Vii)007mentioning

confidence: 76%

“…In this case the temperature T and the adiabatic index Γ are similar for both the jets. In Singh & Chattopadhyay 2019b [26] we showed that it is very important to consider the relativistic CR EoS.…”

Section: Pos(hepro Vii)007mentioning

confidence: 98%

Relativistic Jets From Black Hole Accretion Disc

Chattopadhyay¹,

Vyas²,

Singh³

2020

Proceedings of High Energy Phenomena in Relativistic Outflows VII — PoS(HEPRO VII)

Self Cite

View full text Add to dashboard Cite

show abstract

“…This, coupled with the fluid approximation for the jet matter due to the presence of tangled magnetic fields [11,12], allows for magnetohydrodynamic (MHD) approximation for the jets. A toroidal magnetic field component may retain jet collimation over considerable distances along its path [10,13]. Moreover, external confinement from surrounding winds is equally important [6,14].…”

Section: Introductionmentioning

confidence: 99%

Synthetic Neutrino Imaging of a Microquasar

Smponias¹

2021

Galaxies

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Microquasar binary stellar systems emit electromagnetic radiation and high-energy particles over a broad energy spectrum. However, they are so far away that it is hard to observe their details. A simulation offers the link between relatively scarce observational data and the rich theoretical background. In this work, high-energy particle emission from simulated twin microquasar jets is calculated in a unified manner. From the cascade of emission within an element of jet matter to the dynamic and radiative whole jet model, the series of physical processes involved are integrated together. A programme suite assembled around model data produces synthetic images and spectra directly comparable to potential observations by contemporary arrays. The model is capable of describing a multitude of system geometries, incorporating increasing levels of realism depending on need and available computational resources. As an application, the modelling process is applied to a typical microquasar, which is synthetically observed from different angles using various imaging geometries. Furthermore, the resulting intensities are comparable to the sensitivity of existing detectors. The combined background emission from a potential distribution of microquasars is also modelled.

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Exact solution of one-dimensional relativistic jet with relativistic equation of state

Joshi

Chattopadhyay

Ryu

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We study the evolution of one-dimensional relativistic jets, using the exact solution of the Riemann problem for relativistic flows. For this purpose, we solve equations for the ideal special relativistic fluid composed of dissimilar particles in flat space-time and the thermodynamics of fluid is governed by a relativistic equation of state. We obtain the exact solution of jets impinging on denser ambient media. The time variation of the cross-section of the jet-head is modeled and incorporated. We present the initial condition that gives rise to a reverse shock. If the jet-head cross-section increases in time, the jet propagation speed slows down significantly and the reverse-shock may recede opposite to the propagation direction of the jet. We show that the composition of jet and ambient medium can affect the jet solution significantly. For instance, the propagation speed depends on the composition and is maximum for a pair-dominated jet, rather than a pure electron-positron or electron-proton jet. The propagation direction of the reverse-shock may also strongly depend on the composition of the jet.

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Study of relativistic magnetized outflows with relativistic equation of state

Cited by 4 publications

References 40 publications

Relativistic Jets From Black Hole Accretion Disc

Relativistic Jets From Black Hole Accretion Disc

Synthetic Neutrino Imaging of a Microquasar

Exact solution of one-dimensional relativistic jet with relativistic equation of state

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