Laboratory formation of a scaled protostellar jet by coaligned poloidal magnetic field

Albertazzi, B.; Ciardi, A.; Nakatsutsumi, M.; Vinci, T.; Béard, J.; Bonito, R.; Billette, J.; Borghesi, M.; Burkley, Z.; Chen, S. N.; Cowan, T. E.; Herrmannsdörfer, T.; Higginson, D. P.; Kroll, Florian; Pikuz, S. A.; Naughton, K.; Romagnani, L.; Riconda, C.; Revet, G.; Riquier, R.; Schlenvoigt, Hans-Peter; Skobelev, I. Yu.; Faenov, A. Ya.; Soloviev, A. A.; Huarte-Espinosa, M.; Frank, Adam; Portugall, O.; Pépin, H.; Fuchs, Julien

doi:10.1126/science.1259694

Cited by 200 publications

(129 citation statements)

References 31 publications

(45 reference statements)

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“…The dynamics of the laboratory-produced jets was shown to be scalable to YSOs jets [1,2] as both systems are to a first approximation well described by magnetohydrodynamics (MHD) [12,13]. The laboratory evidence for the poloidal collimation of jets thus offers an explanation of the observed long range collimation of young stellar jets [14].…”

Section: Recent Work and Astrophysical Implicationsmentioning

confidence: 98%

“…Recent laboratory studies [1,2,3] and pertinent astrophysical simulations [4,5,6] have shown the viability of poloidal (i.e. axial) magnetic fields to directly result in the collimation of wide-angle outflows and the formation of jets in astrophysical accreting systems [7,8], such as young stellar objects (YSO).…”

Section: Recent Work and Astrophysical Implicationsmentioning

confidence: 99%

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Detailed characterization of laser-produced astrophysically-relevant jets formed via a poloidal magnetic nozzle

Higginson

Revet

Khiar

et al. 2017

High Energy Density Physics

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This manuscript is distributed under a Creative Commons Attribution-NonCommercial-NoDerivs License (https://creativecommons.org/licenses/by-nc-nd/4.0/), which permits distribution and reproduction for non-commercial purposes, provided the author and source are cited. General rightsCopyright for the publications made accessible via the Queen's University Belfast Research Portal is retained by the author(s) and / or other copyright owners and it is a condition of accessing these publications that users recognise and abide by the legal requirements associated with these rights. AbstractThe collimation of astrophysically-relevant plasma ejecta in the form of narrow jets via a poloidal magnetic field is studied experimentally by irradiating a target situated in a 20 T axial magnetic field with a 40 J, 0.6 ns, 0.7 mm diameter, high-power laser. The dynamics of the plasma shaping by the magnetic field are studied over 70 ns and up to 20 mm from the source by diagnosing the electron density, temperature and optical self-emission. These show that the initial expansion of the plasma is highly magnetized, which leads to the formation of a cavity structure when the kinetic plasma pressure compresses the magnetic field resulting in an oblique shock [A. Ciardi et al., Phys. Rev. Lett. 110, 025002 (2013)]. The resulting poloidal magnetic nozzle generates a standing conical shock that collimates the plasma into a narrow jet [B. Albertazzi et al., Science 346, 325 (2014).]. At distances far from the target, the jet is only marginally magnetized and maintains a high aspect ratio due to its high Mach-number (M ∼ 20) and not due to external magnetic pressure. The formation of the jet is evaluated over a range of laser intensities (10 12 -10 13 W/cm 2 ), target materials and orientations of the magnetic field. Plasma cavity formation is observed in all cases and the viability of long-range jet formation is found to be dependent on the orientation of the magnetic field.

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Section: Recent Work and Astrophysical Implicationsmentioning

confidence: 98%

Section: Recent Work and Astrophysical Implicationsmentioning

confidence: 99%

Detailed characterization of laser-produced astrophysically-relevant jets formed via a poloidal magnetic nozzle

Higginson

Revet

Khiar

et al. 2017

High Energy Density Physics

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“…The other explanation is that dust is genuinely destroyed in a narrow annulus around the inner shell. Other more exotic causes not involving dust destruction could also be considered, such as magneto-hydrodynamic interactions between the wind and large-scale magnetic fields, as explored by van Marle et al (2014) and Albertazzi et al (2014).…”

Section: Possible Modelmentioning

confidence: 99%

The extinction and dust-to-gas structure of the planetary nebula NGC 7009 observed with MUSE

Walsh

Monreal-Ibero

Barlow

et al. 2016

A&A

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Context. Dust plays a significant role in planetary nebulae. Dust ejected with the gas in the asymptotic giant branch (AGB) phase is subject to the harsh environment of the planetary nebula (PN) while the star is evolving towards a white dwarf. Dust surviving the PN phase contributes to the dust content of the interstellar medium. Aims. The morphology of the internal dust extinction has been mapped for the first time in a PN, the bright nearby Galactic nebula NGC 7009. The morphologies of the gas, dust extinction and dust-to-gas ratio are compared to the structural features of the nebula. Methods. Emission line maps in H Balmer and Paschen lines were formed from analysis of MUSE cubes of NGC 7009 observed during science verification of the instrument. The measured electron temperature and density from the same cube were employed to predict the theoretical H line ratios and derive the extinction distribution across the nebula. After correction for the interstellar extinction to NGC 7009, the internal A V /N H has been mapped for the first time in a PN. Results. The extinction map of NGC 7009 has considerable structure, broadly corresponding to the morphological features of the nebula. The dust-to-gas ratio, A V /N H , increases from 0.7 times the interstellar value to >5 times from the centre towards the periphery of the ionized nebula. The integrated A V /N H is about 2× the mean ISM value. A large-scale feature in the extinction map is a wave, consisting of a crest and trough, at the rim of the inner shell. The nature of this feature is investigated and instrumental and physical causes considered; no convincing mechanisms were identified to produce this feature, other than AGB mass loss variations. Conclusions. Extinction mapping from H emission line imaging of PNe with MUSE provides a powerful tool for revealing the properties of internal dust and the dust-to-gas ratio.

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“…In the aspect of astrophysics, a high magnetic field is related to many high-energy astrophenomena, such as the jet formation [5] , magnetic reconnection (MR) [6,7] and collisionless shock formations. Laboratory generation of strong magnetic fields makes it possible to study them in a new regime and controllable way.…”

Section: Magnetic-field Generation In the Laboratorymentioning

confidence: 99%

Laboratory astrophysics with laser-driven strong magnetic fields in China

Wang

Pei

Han

et al. 2016

High Pow Laser Sci Eng

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In this paper, the recent studies of laboratory astrophysics with strong magnetic fields in China have been reviewed. On the Shenguang-II laser facility of the National Laboratory on High-Power Lasers and Physics, a laser-driven strong magnetic field up to 200 T has been achieved. The experiment was performed to model the interaction of solar wind with dayside magnetosphere. Also the low beta plasma magnetic reconnection (MR) has been studied. Theoretically, the model has been developed to deal with the atomic structures and processes in strong magnetic field. Also the study of shock wave generation in the magnetized counter-streaming plasmas is introduced.

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Laboratory formation of a scaled protostellar jet by coaligned poloidal magnetic field

Cited by 200 publications

References 31 publications

Detailed characterization of laser-produced astrophysically-relevant jets formed via a poloidal magnetic nozzle

Detailed characterization of laser-produced astrophysically-relevant jets formed via a poloidal magnetic nozzle

The extinction and dust-to-gas structure of the planetary nebula NGC 7009 observed with MUSE

Laboratory astrophysics with laser-driven strong magnetic fields in China

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