How unique are pulsar wind nebulae models? Implementation of a multi-parameter, automatic fitting for time-dependent spectra

Martín, J.; Torres, D. F.

doi:10.1016/j.jheap.2022.09.003

Cited by 9 publications

(1 citation statement)

References 64 publications

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“…So far, PWNe have been mostly described with timedependent one-zone (also named 0+1) models (Gelfand et al 2009;Bucciantini et al 2011;Martín et al 2012;Torres et al 2013Torres et al , 2014Martin & Torres 2022), especially when a large number of systems, a wide parameter space, or an extended evolution is investigated. One-zone models represent the PWN as a uniform bubble interacting with the surrounding supernova remnant (SNR) and subject to energy (adiabatic and radiative) and particles losses (Reynolds & Chevalier 1984).…”

Section: Introductionmentioning

confidence: 99%

Reverberation of pulsar wind nebulae – II. Anatomy of the ‘thin-shell’ evolution

Bandiera

Bucciantini

Martín

et al. 2023

Monthly Notices of the Royal Astronomical Society

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During its early evolution, a pulsar wind nebula (PWN) sweeps the inner part of the supernova ejecta and forms a thin massive shell. Later on, when the shell has been reached by the reverse shock of the supernova remnant, the evolution becomes more complex, in most cases reverting the expansion into a compression: this later phase is called “reverberation”. Computations done so far to understand this phase have been mostly performed in the thin-shell approximation, where the evolution of the PWN radius is assimilated to that of the swept-up shell under the effect of both the inner pressure from the PWN, and the outer pressure from the supernova remnant. Despite the thin-shell approach seems rather justifiable, its implementations have so far been inaccurate, and its correctness, never tested. The outer pressure was naively assumed to be scaled according to the Sedov solution (or a constant fraction of it) along the entire evolution. The thin-shell assumption itself fails along the process, being the shell no longer thin in comparison with the size of the PWN. Here, through a combination of numerical models, dimensional arguments, and analytic approximations, we present a detailed analysis of the interaction of the PWN with the supernova remnant. We provide a new analytic approximation of the outer pressure, beyond the Sedov solution, and a revised “thin-shell” able to reproduce results from numerical simulations. Finally, we compute the efficiency by which the PWN is compressed during reverberation over a wide population of sources.

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Section: Introductionmentioning

confidence: 99%

Reverberation of pulsar wind nebulae – II. Anatomy of the ‘thin-shell’ evolution

Bandiera

Bucciantini

Martín

et al. 2023

Monthly Notices of the Royal Astronomical Society

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LHAASO J2226+6057 as a pulsar wind nebula

Sarkar

Zhang

Martín

et al. 2022

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Context. The Large High Altitude Air Shower Observatory has reported the detection of cosmic-ray sources in Milky Way that can accelerate particles up to PeV (= 10 15 eV) energies. These sources, so called "PeVatrons", are mostly unidentified. Several classes of sources, such as supernova remnants, pulsar wind nebula, or young stellar clusters can potentially be the counterparts of these PeVatrons.Aims. The aim of this work is to study a pulsar wind nebula interpretation of one of these PeVatrons, LHAASO J2226+6057, which has a relatively well covered multi-frequency spectrum. Methods. We have performed a leptonic, time-dependent modeling of the pulsar wind nebula (PWN) associated with PSR J2229+6114 considering a time-energy-dependent diffusion-loss equation. Injection, energy losses, as well as escape of particles were considered to balance the time-dependent lepton population. We have also included the dynamics of the PWN and the associated supernova remnant (SNR) and their interaction via the reverse shock to study the reverberation phase of the system. Results. We have considered different values of braking index (n) and true age (t age ) for the fitting of the multi-wavelength (MWL) spectral energy distribution (SED) of LHAASO J2226+6057. The best-fit PWN model parameters and their 1σ confidence intervals were evaluated. We have also demonstrated the impact of reverberation on the MWL SED with increasing time. Additionally, we have discussed the resultant large radius and low magnetic field associated with the PWN in question, as caveats for the possible physical connection of the pulsar as the origin of this high energy source.

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Analysis of the possible detection of the pulsar wind nebulae of PSR J1208-6238, J1341-6220, J1838-0537, and J1844-0346

Zhang,

Torres,

García

et al. 2024

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Pulsar wind nebulae (PWNe) are a source of very high energy radiation that can reach up to tera-electron volts and even peta-electron volts. Our work uses the pulsar tree, a graph theory tool recently presented to analyze the pulsar population and select candidates of interest. We aim to discover detectable PWNe. We also aim to test to what extent the pulsar tree is able to group detectable PWNe despite only considering the intrinsic properties of pulsars. We selected four pulsars as tera-electron volt PWNe candidates based on their positions in the pulsar tree. Using observed and assumed ranges of values for relevant parameters, we anticipated the possible spectral energy distributions of the PWNe of four pulsars (PSR J1208-6238, J1341-6220, J1838-0537, and J1844-0346) via a detailed time-dependent leptonic model that was already found to be appropriate for describing almost all other detected nebulae. We estimated the likelihood of detection for the four candidates we studied by comparing the TeV fluxes predicted by the possible models with the sensitivities of different observatories. In doing so, we provide context for analyzing the advantages and caveats of using the pulsar tree position as a marker for properties that go beyond the intrinsic features of pulsars that are considered in producing the pulsar tree.

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How unique are pulsar wind nebulae models? Implementation of a multi-parameter, automatic fitting for time-dependent spectra

Cited by 9 publications

References 64 publications

Reverberation of pulsar wind nebulae – II. Anatomy of the ‘thin-shell’ evolution

Reverberation of pulsar wind nebulae – II. Anatomy of the ‘thin-shell’ evolution

LHAASO J2226+6057 as a pulsar wind nebula

Analysis of the possible detection of the pulsar wind nebulae of PSR J1208-6238, J1341-6220, J1838-0537, and J1844-0346

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