On the application of Jacobian-free Riemann solvers for relativistic radiation magnetohydrodynamics under M1 closure

López-Miralles, José; Martí, J.; Perucho, M.

doi:10.1016/j.cpc.2022.108630

Cited by 3 publications

(6 citation statements)

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“…Following a number of papers that studied RHD simulations of jet-massive wind interactions (Perucho & Bosch-Ramon 2008;Perucho et al 2010a;Perucho & Bosch-Ramon 2012), we run a set of dedicated three-dimensional numerical simulations using our new code LÓSTREGO, including the dynamical effects of magnetic fields (López-Miralles et al 2022). The results of these simulations showed that the latter could play a stabilizing role -and thus, to provide extra collimation within the binary scalein the jet evolution when the flux of magnetic energy is low compared with the flux of kinetic energy, while a non-negligible magnetic energy flux makes the jet prone to the development of current-driven instabilities within the scale of the binary.…”

Section: The Rmhd Simulations 321 Jet-stellar Wind Interactionsmentioning

confidence: 99%

“…Perucho, Bosch-Ramon & Barkov 2017a), hydrogen ionization and recombination effects (e.g. Vaidya et al (2015), Perucho et al (2021), Perucho et al, in preparation) or radiation feedback (López-Miralles, Martí & Perucho 2023).…”

Section: The Rmhd Equationsmentioning

confidence: 99%

“…In figure 5 we present the resulting configuration of the magnetic field in this simulation by focusing on the field lines. This plot shows relevant information about the field structure in the jet spine, which was hidden by the mixed plasma in the cocoon in our representation in López-Miralles et al (2022). Since the magnetic field within the cocoon is low compared with that in the jet, we have applied a linear transparency to the field lines, weighted by the field vector module.…”

Section: The Rmhd Simulations 321 Jet-stellar Wind Interactionsmentioning

confidence: 99%

“…Mirabel (2010) and Fender (2006), for a review), a large number of unknowns remain about fundamental aspects such as their composition (Migliari, Fender & Méndez 2002), internal dynamics and its relation to the formation mechanism and changes in the accretion flow (Fender, Belloni & Gallo 2004), or the mechanisms that generate the production of high-to very-high-energy radiative output within the binary scales (see, e.g. Perucho & Bosch-Ramon 2008;Bosch-Ramon & Khangulyan 2009a;Perucho, Bosch-Ramon & Khangulyan 2010a;Bosch-Ramon et al 2012a;Perucho & Bosch-Ramon 2012;Bosch-Ramon, Barkov & Perucho 2015;Paredes-Fortuny et al 2015;de la Cita et al 2017;López-Miralles et al 2022), even far from the sub-milliarscsecond resolution achieved by very large baseline interferometry at cm-mm wavelengths in the radio band. Furthermore, the transition of the jet from these compact regions (∼10 10 m) to parsec scales (∼10 16 m) has been barely studied by numerical simulations, and only few works have been devoted to microquasar jet evolution at the largest scales (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Numerical simulations of relativistic jets

Perucho,

López-Miralles

2023

J. Plasma Phys.

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In this paper, we review recent and ongoing work by our group on numerical simulations of relativistic jets. Relativistic outflows in astrophysics are related to dilute, high energy plasmas, with physical conditions out of the reach of current laboratory capabilities. Simulations are thus imperative for the study of these objects. We present a number of such scenarios that have been studied by our group at the Universitat de València. In particular, we have focused on the evolution of extragalactic outflows through galactic and intergalactic environments, deceleration by interaction with stars or clouds or the propagation of jets in X-ray binaries and interaction with stellar winds from massive companions. All also share their role as particle acceleration sites and production of non-thermal radiation throughout the electromagnetic spectrum. Therefore, our work is not only aimed at understanding the impact of outflows on their environments and thus their role in galaxy and cluster evolution, but also the nature and capabilities of these sites as generators of high- and very-high-energy radiation and cosmic rays.

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Section: The Rmhd Simulations 321 Jet-stellar Wind Interactionsmentioning

confidence: 99%

Section: The Rmhd Equationsmentioning

confidence: 99%

Section: The Rmhd Simulations 321 Jet-stellar Wind Interactionsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Numerical simulations of relativistic jets

Perucho,

López-Miralles

2023

J. Plasma Phys.

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“…well; this is known as the two-moment scheme (Levermore 1984;Dubroca & Feugeas 1999). This approach has been applied in the context of neutron star merger (Wanajo et al 2014;Foucart et al 2015;Foucart et al 2016b;Foucart et al 2016a;Sekiguchi et al 2015;Radice et al 2022; see also the review by Foucart 2023), core-collapse supernovae (O'Connor 2015; Just et al 2015;Roberts et al 2016;Kuroda et al 2016;O'Connor & Couch 2018a;Skinner et al 2019;Laiu et al 2021;Santos-Pérez et al 2023; see also the review Mezzacappa et al 2020), black hole accretions (Zanotti et al 2011;Fragile et al 2012;Sądowski et al 2013;Fragile et al 2014;McKinney et al 2014;Takahashi et al 2016;Fragile et al 2018), and other purposes (González et al 2007;Commerçon et al 2011;Skinner & Ostriker 2013;Takahashi & Ohsuga 2013;Rivera-Paleo & Guzmán 2019;Melon Fuksman & Mignone 2019;Weih et al 2020b;Anninos & Fragile 2020;López-Miralles et al 2023) as well. Despite the recent progress of radiation transport modeling, the implementation of general-relativistic multispecies multigroup radiation magnetohydrodynamics codes, which include fully coupled radiation-matter interactions, is still not very common (but see a notable example Kuroda et al 2016), but is essential for astrophysics modeling.…”

Section: Introductionmentioning

confidence: 99%

General-relativistic Radiation Transport Scheme in Gmunu. I. Implementation of Two-moment-based Multifrequency Radiative Transfer and Code Tests

Cheong

Lam

et al. 2023

ApJS

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We present the implementation of a two-moment-based general-relativistic multigroup radiation transport module in the General-relativistic multigrid numerical (Gmunu) code. On top of solving the general-relativistic magnetohydrodynamics and the Einstein equations with conformally flat approximations, the code solves the evolution equations of the zeroth- and first-order moments of the radiations in the Eulerian-frame. An analytic closure relation is used to obtain the higher order moments and close the system. The finite-volume discretization has been adopted for the radiation moments. The advection in spatial space and frequency-space are handled explicitly. In addition, the radiation–matter interaction terms, which are very stiff in the optically thick region, are solved implicitly. The implicit–explicit Runge–Kutta schemes are adopted for time integration. We test the implementation with a number of numerical benchmarks from frequency-integrated to frequency-dependent cases. Furthermore, we also illustrate the astrophysical applications in hot neutron star and core-collapse supernovae modelings, and compare with other neutrino transport codes.

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On the large scale morphology of Hercules A: destabilized hot jets?

Perucho

López-Miralles

Gizani

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Extragalactic jets are generated as bipolar outflows at the nuclei of active galaxies. Depending on their morphology, they are classified as Fanaroff-Riley type I (centre-brightened) and Fanaroff-Riley type II (edge-brightened) radio jets. However, this division is not sharp and observations of these sources at large scales often show intermediate jet morphologies or even hybrid jet morphologies with a FRI type jet on one side and a FRII type jet on the other. A good example of a radio galaxy that is difficult to classify as FRI or FRII is Hercules A. This source shows jets with bright radio lobes (a common feature of FRII type jets) albeit without the hotspots indicative of the violent interaction between the jet and the ambient medium at the impact region, because the jets seem to be disrupted inside the lobes at a distance from the bow shocks surrounding the lobes. In this paper, we explore the jet physics that could trigger this peculiar morphology by means of three-dimensional relativisitic hydrodynamical simulations. Our results show that the large-scale morphological features of Hercules A jets and lobes can be reproduced by the propagation of a relativistically hot plasma outflow that is disrupted by helical instability modes, and generates a hot lobe that expands isotropically against the pressure-decreasing intergalactic medium. We also discuss the implications that this result may have for the host active nucleus in terms of a possible transition from high-excitation to low-excitation galaxy modes.

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On the application of Jacobian-free Riemann solvers for relativistic radiation magnetohydrodynamics under M1 closure

Cited by 3 publications

References 88 publications

Numerical simulations of relativistic jets

Numerical simulations of relativistic jets

General-relativistic Radiation Transport Scheme in Gmunu. I. Implementation of Two-moment-based Multifrequency Radiative Transfer and Code Tests

On the large scale morphology of Hercules A: destabilized hot jets?

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