Temporal evolution of the shock wave and hot core air in laser induced plasma

Sobral, H.; Villagrán-Munı́z, M.; Navarro‐González, Rafael; Raga, A. C.

doi:10.1063/1.1324986

Cited by 161 publications

(84 citation statements)

References 10 publications

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“…This code has been tested with laser laboratory explosions (Sobral et al 2000;Velázquez et al 2001a) and jets (Raga et al 2001), giving confidence in the accuracy of the results obtained when computing SNR models (Velázquez et al 2001b).…”

Section: The Yguazú-a Codementioning

confidence: 99%

Effects of Thermal Conduction on the X‐Ray and Synchrotron Emission from Supernova Remnants

Velázquez

Martinell

Raga

et al. 2004

ApJ

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Several physical mechanisms have been studied in order to explain why composite supernova remnants (SNRs) have shell-like morphologies in the radio continuum while their X-ray emission is centrally peaked. One of the proposed mechanisms has been the presence of thermal conduction, which can raise the density at the center of SNRs, increasing the X-ray emission from these regions. In this work, we have carried out axisymmetric numerical simulations with the adaptive grid Yguazú-a code, which includes advection of the magnetic field and thermal conduction. We have considered cases with anisotropic and isotropic thermal conduction, as well as with no conduction. We have simulated X-ray (as well as radio synchrotron) emission maps from our numerical simulations, which can be directly compared with observations.

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Section: The Yguazú-a Codementioning

confidence: 99%

Effects of Thermal Conduction on the X‐Ray and Synchrotron Emission from Supernova Remnants

Velázquez

Martinell

Raga

et al. 2004

ApJ

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“…Within the following 10 −9 -10 −8 s, Tm rapidly ascents through energy transfer due to elastic and inelastic collision between hot electrons and the surrounding air molecules (nitrogen and oxygen), until thermal equilibrium appears [19,20]. This sudden increase of localized gas temperature gives rise to a shock wave that persists for a short distance, then relaxing into acoustic wave [21,22].…”

Section: Experimental Details and Resultsmentioning

confidence: 99%

Acoustic Measurement of the Length of Air-plasma Filament Induced by an Intense Femtosecond Laser Pulse

Dai

Xiong

2017

ITM Web Conf.

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Abstract:The paper studies acoustic emission from air-plasma filament induced by a strong femtosecond laser pulse. Acoustic signal is detected with a sensitive directional microphone. Acoustic measurement provides a new method to determine the length of a filament. Compared with other methods, acoustic measurement is simpler, more sensitive, and with higher spatial resolution. Information of filament length is experimentally acquired through measuring acoustic pressure at different position of filament. On the basis of the relationship between acoustic signal and free-electron density in filament, profile of free-electron density is demonstrated

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“…(Cerqueira et al 2006b) and supernova remnants (Velázquez et al 2001a). It was also tested with laser generated plasma laboratory experiments (Sobral et al 2000;Raga et al 2001;Velázquez et al 2001b). In this work, instead of solving an energy equation, we prescribe a temperature law, given by…”

Section: The Numerical Method the Numerical Setup And The Simulatedmentioning

confidence: 99%

3D numerical simulations of photodissociated and photoionized disks

Vasconcelos¹,

Cerqueira²,

Raga³

2011

A&A

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Aims. In this work we study the influence of the UV radiation field of a massive star on the evolution of a disklike mass of gas and dust around a nearby star. This system has similarities with the proplyds seen in Orion. Methods. We study disks with different inclinations and distances from the source, performing fully 3D numerical simulations. We use the YGUAZÚ-A adaptative grid code modified to account for EUV/FUV fluxes and non-spherical mass distributions. We treat H and C photoionization in order to reproduce the ionization fronts and photodissociation regions observed in proplyds. We also incorporate a wind from the ionizing source, in order to investigate the formation of the bow shock observed in several proplyds. We examine density and Hα maps, as well as the mass loss rates in the photoevaporated winds. Results. Our results show that a photoevaporated wind propagates from the disk surface and becomes ionized after an ionization front (IF) seen as a bright peak in the Hα maps. We follow the development of an HI region inside the photoevaporated wind which corresponds to a photodissociated region (PDR) for most of our models, except those without a FUV flux. For disks that are at a distance from the source d ≥ 0.1 pc, the PDR is thick and the IF is detached from the disk surface. In contrast, for disks that are closer to the source, the PDR is thin and not resolved in our simulations. The IF then coincides with the first grid points of the disk that are facing the ionizing photon source. In both cases, the photoevaporated wind shocks (after the IF) with the wind that comes from the ionizing source, and this interaction region is bright in Hα. Conclusions. Our 3D models produce two emission features: a hemispherically shaped structure (associated with the IF) and a detached bow shock where both winds collide. A photodissociated region develops in all of the models exposed to the FUV flux. More importantly, disks with different inclinations with respect to the ionizating source have relatively similar photodissociation regions. If the disk axis is not aligned with the direction of the ionizing photon flux, the IF displays moderate side-to-side asymmetries, in qualitative agreement with images of proplyds, which also show such asymmetries. The mass loss rates are ∼10 −7 M yr −1 for face-on disks, and 5 × 10 −8 M yr −1 for inclined disks at distances from 0.1 to 0.2 pc from the ionizing photon sources.

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Temporal evolution of the shock wave and hot core air in laser induced plasma

Cited by 161 publications

References 10 publications

Effects of Thermal Conduction on the X‐Ray and Synchrotron Emission from Supernova Remnants

Effects of Thermal Conduction on the X‐Ray and Synchrotron Emission from Supernova Remnants

Acoustic Measurement of the Length of Air-plasma Filament Induced by an Intense Femtosecond Laser Pulse

3D numerical simulations of photodissociated and photoionized disks

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