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Journal articles on the topic 'Jets'

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Author: Grafiati

Published: 4 June 2021

Last updated: 29 July 2024

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1

Zhang, Yan-Jie, Qing-Min Zhang, Jun Dai, Zhe Xu, and Hai-Sheng Ji. "Recurrent coronal jets observed by SDO/AIA." Research in Astronomy and Astrophysics 21, no. 10 (November 1, 2021): 262. http://dx.doi.org/10.1088/1674-4527/21/10/262.

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Abstract In this paper, we carried out multiwavelength observations of three recurring jets on 2014 November 7. The jets originated from the same region at the edge of AR 12205 and propagated along the same coronal loop. The eruptions were generated by magnetic reconnection, which is evidenced by continuous magnetic cancellation at the jet base. The projected initial velocity of jet2 is ∼402 km s−1. The accelerations in the ascending and descending phases of jet2 are not consistent, the former is considerably larger than the value of g ⊙ at the solar surface, while the latter is lower than g ⊙. There are two possible candidates of extra forces acting on jet2 during its propagation. One is the downward gas pressure from jet1 when it falls back and meets with jet2. The other is the viscous drag from the surrounding plasma during the fast propagation of jet2. As a contrast, the accelerations of jet3 in the rising and falling phases are constant, implying that the propagation of jet3 is not significantly influenced by extra forces.

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2

Moore, Ronald L., Jonathan W. Cirtain, Alphonse C. Sterling, and David A. Falconer. "DICHOTOMY OF SOLAR CORONAL JETS: STANDARD JETS AND BLOWOUT JETS." Astrophysical Journal 720, no. 1 (August 13, 2010): 757–70. http://dx.doi.org/10.1088/0004-637x/720/1/757.

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3

Rhines, Peter B. "Jets." Chaos: An Interdisciplinary Journal of Nonlinear Science 4, no. 2 (June 1994): 313–39. http://dx.doi.org/10.1063/1.166011.

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4

Falle, S. A. E. G. "Jets." Astrophysics and Space Science 216, no. 1-2 (June 1994): 119–25. http://dx.doi.org/10.1007/bf00982478.

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5

Sterling, Alphonse C., Ronald L. Moore, and Navdeep K. Panesar. "Another Look at Erupting Minifilaments at the Base of Solar X-Ray Polar Coronal “Standard” and “Blowout” Jets." Astrophysical Journal 927, no. 1 (March 1, 2022): 127. http://dx.doi.org/10.3847/1538-4357/ac473f.

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Abstract We examine 21 solar polar coronal jets that we identify in soft X-ray images obtained from the Hinode/X-ray telescope (XRT). We identify 11 of these jets as blowout jets and four as standard jets, based on their X-ray-spire widths being respectively wide or narrow (compared to the jet’s base) in the XRT images. From corresponding extreme ultraviolet (EUV) images from the Solar Dynamics Observatory’s (SDO) Atmospheric Imaging Assembly (AIA), essentially all (at least 20 of 21) of the jets are made by minifilament eruptions, consistent with other recent studies. Here, we examine the detailed nature of the erupting minifilaments (EMFs) in the jet bases. Wide-spire (“blowout”) jets often have ejective EMFs, but sometimes they instead have an EMF that is mostly confined to the jet’s base rather than ejected. We also demonstrate that narrow-spire (“standard”) jets can have either a confined EMF, or a partially confined EMF where some of the cool minifilament leaks into the jet’s spire. Regarding EMF visibility: we find that in some cases the minifilament is apparent in as few as one of the four EUV channels we examined, being essentially invisible in the other channels; thus, it is necessary to examine images from multiple EUV channels before concluding that a jet does not have an EMF at its base. The sizes of the EMFs, measured projected against the sky and early in their eruption, is 14″ ± 7″, which is within a factor of 2 of other measured sizes of coronal-jet EMFs.

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6

Sterling, Alphonse C., Ronald L. Moore, and Navdeep K. Panesar. "Solar Active Region Coronal Jets. III. Hidden-onset Jets." Astrophysical Journal 960, no. 2 (January 1, 2024): 109. http://dx.doi.org/10.3847/1538-4357/acff6b.

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Abstract Solar quiet- and coronal-hole region coronal jets frequently clearly originate from erupting minifilaments, but active-region jets often lack an obvious erupting-minifilament source. We observe a coronal-jet-productive active region (AR), AR 12824, over 2021 May 22 0–8 UT, primarily using Solar Dynamics Observatory (SDO) Atmospheric Imaging Array (AIA) EUV images and SDO/Helioseismic and Magnetic Imager magnetograms. Jets were concentrated in two locations in the AR: on the south side and on the northwest side of the AR’s lone large sunspot. The south-location jets are oriented so that we have a clear view of the jets’ origin low in the atmosphere: their source is clearly minifilaments erupting from locations showing magnetic flux changes/cancelations. After erupting a projected distance ≲5″ away from their origin site, the minifilaments erupt outward onto far-reaching field as part of the jet’s spire, quickly losing their minifilament character. In contrast, the northwest-location jets show no clear erupting minifilament, but the source site of those jets are obscured along our line of sight by absorbing chromospheric material. EUV and magnetic data indicate that the likely source sites were ≳15″ from where the we first see the jet spire; thus, an erupting minifilament would likely lose its minifilament character before we first see the spire. We conclude that such AR jets could work like non-AR jets, but the erupting-minifilament jet source is often hidden by obscuring material. Another factor is that magnetic eruptions making some AR jets carry only a harder-to-detect comparatively thin (∼1″–2″) minifilament “strand.”

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7

Plaschke, Ferdinand, and Heli Hietala. "Plasma flow patterns in and around magnetosheath jets." Annales Geophysicae 36, no. 3 (May 3, 2018): 695–703. http://dx.doi.org/10.5194/angeo-36-695-2018.

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Abstract. The magnetosheath is commonly permeated by localized high-speed jets downstream of the quasi-parallel bow shock. These jets are much faster than the ambient magnetosheath plasma, thus raising the question of how that latter plasma reacts to incoming jets. We have performed a statistical analysis based on 662 cases of one THEMIS spacecraft observing a jet and another (second) THEMIS spacecraft providing context observations of nearby plasma to uncover the flow patterns in and around jets. The following results are found: along the jet's path, slower plasma is accelerated and pushed aside ahead of the fastest core jet plasma. Behind the jet core, plasma flows into the path to fill the wake. This evasive plasma motion affects the ambient magnetosheath, close to the jet's path. Diverging and converging plasma flows ahead and behind the jet are complemented by plasma flows opposite to the jet's propagation direction, in the vicinity of the jet. This vortical plasma motion results in a deceleration of ambient plasma when a jet passes nearby. Keywords. Magnetospheric physics (magnetosheath; MHD waves and instabilities; solar wind–magnetosphere interactions)

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8

Kimura, Motoaki, and Norimasa Miyagi. "STUDY ON DIFFUSION OF BUOYANT ROUND JETS(Jet and Plume)." Proceedings of the International Conference on Jets, Wakes and Separated Flows (ICJWSF) 2005 (2005): 413–18. http://dx.doi.org/10.1299/jsmeicjwsf.2005.413.

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9

Spencer, Ralph, Chris De La Force, and Alastair Stirling. "Microquasar Jets: A Comparison with Extragalactic Jets." Symposium - International Astronomical Union 205 (2001): 264–65. http://dx.doi.org/10.1017/s0074180900221141.

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10

Denis, S., J. Delville, J.-H. Garem, and J.-P. Bonnet. "Control of jets expansion by impeding jets." ZAMM - Journal of Applied Mathematics and Mechanics / Zeitschrift für Angewandte Mathematik und Mechanik 80, S1 (2000): 81–84. http://dx.doi.org/10.1002/zamm.20000801321.

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11

Gottlieb, Ore, Omer Bromberg, Chandra B. Singh, and Ehud Nakar. "The structure of weakly magnetized γ-ray burst jets." Monthly Notices of the Royal Astronomical Society 498, no. 3 (August 22, 2020): 3320–33. http://dx.doi.org/10.1093/mnras/staa2567.

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ABSTRACT The interaction of gamma-ray burst (GRB) jets with the dense media into which they are launched promote the growth of local hydrodynamic instabilities along the jet boundary. In a companion paper, we study the evolution of hydrodynamic (unmagnetized) jets, finding that mixing of jet–cocoon material gives rise to an interface layer, termed jet–cocoon interface (JCI), which contains a significant fraction of the system energy. We find that the angular structure of the jet + JCI, when they reach the homologous phase, can be approximated by a flat core (the jet) + a power-law function (the JCI) with indices that depend on the degree of mixing. In this paper, we examine the effect of subdominant toroidal magnetic fields on the jet evolution and morphology. We find that weak fields can stabilize the jet against local instabilities. The suppression of the mixing diminishes the JCI and thus reshapes the jet’s post-breakout structure. Nevertheless, the overall shape of the outflow can still be approximated by a flat core + a power-law function, although the JCI power-law decay is steeper. The effect of weak fields is more prominent in long GRB jets, where the mixing in hydrodynamic jets is stronger. In short GRB jets, there is small mixing in both weakly magnetized and unmagnetized jets. This result influences the expected jet emission which is governed by the jet’s morphology. Therefore, prompt and afterglow observations in long GRBs may be used as probes for the magnetic nature at the base of the jets.

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12

Kudoh, T., K. Shibata, and R. Matsumoto. "8.9. MHD simulations of jets from accretion disks: nonsteady jets vs. steady jets." Symposium - International Astronomical Union 184 (1998): 361–62. http://dx.doi.org/10.1017/s0074180900085223.

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We present the results of 2.5-dimensional MHD simulations for jet formation from accretion disks in a situation such that not only ejection but also accretion of disk plasma are also included self-consistently. Although the jets in nonsteady MHD simulations (e.g., Uchida & Shibata 1985, Shibata & Uchida 1986, Matsumoto et al. 1996) have often been referred to as transient phenomena resulting from a special choice of initial conditions, we found that the characteristics of the nonsteady jets are very similar to those of steady jets: (1) The ejection point of the jet, which corresponds to slow magnetosonic point in steady MHD jet theory, is determined by the effective potential which results from the gravitational force and the centrifugal force along a field line (Blandford & Payne 1982). (2) The dependence of the velocity (vz) and mass outflow rate (Ṁω) on the initial magnetic field strength is about Ṁω ∝ B0 and vz ∝ (Ω2FB20/Ṁω)1/3, where B0 is an initial poloidal magnetic field strength, and ΩF is an ‘angular velocity of the field line’ which is nearly the same as the Keplerian angular velocity where the jet is ejected. These are consistent with those of 1D steady solution (Kudoh & Shibata 1997), although the explanation is a little complicated in the 2.5D case because of an avalanche-like accretion. We also confirm that the velocity of the jet is of order of the Keplerian velocity of the disk for a wide range of parameters. We conclude that the ejection mechanism of nonsteady jets found in the 2.5-dimensional simulations are understood with a previous theory which is studied on the assumption of steady state even when nonsteady avalanche-like accretions occur along the surface of disks.

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13

Pasko, Victor P. "Electric jets." Nature 423, no. 6943 (June 2003): 927–28. http://dx.doi.org/10.1038/423927a.

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14

Wilson, M. J., and S. A. E. G. Falle. "Steady jets." Monthly Notices of the Royal Astronomical Society 216, no. 4 (October 1985): 971–85. http://dx.doi.org/10.1093/mnras/216.4.971.

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15

Bell, A. R. "Magnetohydrodynamic jets*." Physics of Plasmas 1, no. 5 (May 1994): 1643–52. http://dx.doi.org/10.1063/1.870666.

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16

Antkowiak, Arnaud, Nicolas Bremond, Jérôme Duplat, Stéphane Le Dizès, and Emmanuel Villermaux. "Cavity jets." Physics of Fluids 19, no. 9 (September 2007): 091112. http://dx.doi.org/10.1063/1.2775413.

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17

Chicone, C., B. Mashhoon, and K. Rosquist. "Cosmic jets." Physics Letters A 375, no. 12 (March 2011): 1427–30. http://dx.doi.org/10.1016/j.physleta.2011.02.036.

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18

Bicknell, Geoffrey V., Dayton L. Jones, and Matthew Lister. "Relativistic jets." New Astronomy Reviews 48, no. 11-12 (December 2004): 1151–55. http://dx.doi.org/10.1016/j.newar.2004.09.005.

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19

Leoncini, Xavier, and George M. Zaslavsky. "Chaotic jets." Communications in Nonlinear Science and Numerical Simulation 8, no. 3-4 (September 2003): 265–71. http://dx.doi.org/10.1016/s1007-5704(03)00038-8.

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20

HEWITT, RICHARD E., and PETER W. DUCK. "Pulsatile jets." Journal of Fluid Mechanics 670 (January 12, 2011): 240–59. http://dx.doi.org/10.1017/s0022112010005227.

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We consider the evolution of high-Reynolds-number, planar, pulsatile jets in an incompressible viscous fluid. The source of the jet flow comprises a mean-flow component with a superposed temporally periodic pulsation, and we address the spatiotemporal evolution of the resulting system. The analysis is presented for both a free symmetric jet and a wall jet. In both cases, pulsation of the source flow leads to a downstream short-wave linear instability, which triggers a breakdown of the boundary-layer structure in the nonlinear regime. We extend the work of Riley, Sánchez-Sans & Watson (J. Fluid Mech., vol. 638, 2009, p. 161) to show that the linear instability takes the form of a wave that propagates with the underlying jet flow, and may be viewed as a (spatially growing) weakly non-parallel analogue of the (temporally growing) short-wave modes identified by Cowley, Hocking & Tutty (Phys. Fluids, vol. 28, 1985, p. 441). The nonlinear evolution of the instability leads to wave steepening, and ultimately a singular breakdown of the jet is obtained at a critical downstream position. We speculate that the form of the breakdown is associated with the formation of a ‘pseudo-shock’ in the jet, indicating a failure of the (long-length scale) boundary-layer scaling. The numerical results that we present disagree with the recent results of Riley et al. (2009) in the case of a free jet, together with other previously published works in this area.

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21

Halzen, Francis, and Duncan A. Morris. "Coplanar jets." Physical Review D 42, no. 5 (September 1, 1990): 1435–39. http://dx.doi.org/10.1103/physrevd.42.1435.

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22

Thoroddsen, S. T., and Amy Q. Shen. "Granular jets." Physics of Fluids 13, no. 1 (January 2001): 4–6. http://dx.doi.org/10.1063/1.1328359.

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23

DE YOUNG, D. S. "Astrophysical Jets." Science 252, no. 5004 (April 19, 1991): 389–96. http://dx.doi.org/10.1126/science.252.5004.389.

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24

Wall, C. T. C. "Equivariant jets." Mathematische Annalen 272, no. 1 (March 1985): 41–65. http://dx.doi.org/10.1007/bf01455927.

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25

MURAMATSU, Akinori, Kuu Kashino, and Seiichi Terahara. "Side jets in strongly-forced round air jets." Journal of the Visualization Society of Japan 28-1, no. 2 (2008): 1009. http://dx.doi.org/10.3154/jvs.28.1009.

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26

Saltó, Oriol. "+ Jets and + Heavy Flavor Jets at the Tevatron." Nuclear Physics B - Proceedings Supplements 186 (January 2009): 15–18. http://dx.doi.org/10.1016/j.nuclphysbps.2008.12.003.

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27

Smith, B. L., and G. W. Swift. "A comparison between synthetic jets and continuous jets." Experiments in Fluids 34, no. 4 (February 5, 2003): 467–72. http://dx.doi.org/10.1007/s00348-002-0577-6.

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28

Pumplin, Jon. "How to tell quark jets from gluon jets." Physical Review D 44, no. 7 (October 1, 1991): 2025–32. http://dx.doi.org/10.1103/physrevd.44.2025.

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29

Tomac, Mehmet N. "Novel impinging jets-based non-periodic sweeping jets." Journal of Visualization 23, no. 3 (March 5, 2020): 369–72. http://dx.doi.org/10.1007/s12650-020-00633-2.

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30

Sapinski, Mariusz. "Expected performance of ATLAS for measurements of jets, b-jets, τ-jets, and ETmiss." EPJ direct 4, S1 (September 2002): 1–12. http://dx.doi.org/10.1007/s1010502cs108.

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31

Toyoda, Kuniaki, Jun Akazawa, Hayato Mori, and Riho Hiramoto. "EFFECT OF STREAMWISE VORTICES ON THE CHARACTERISTICS OF JETS(Plane Jet)." Proceedings of the International Conference on Jets, Wakes and Separated Flows (ICJWSF) 2005 (2005): 171–76. http://dx.doi.org/10.1299/jsmeicjwsf.2005.171.

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32

Shinohara, Eri, Fumitoshi Okamoto, Yuki Kitaoka, Kazuya Tatsumi, and Kazuyoshi Nakabe. "MIXING CHARACTERISTICS OF MULTI-JETS MODIFIED BY CYCLIC PERTURBATION(Multiple Jet)." Proceedings of the International Conference on Jets, Wakes and Separated Flows (ICJWSF) 2005 (2005): 255–60. http://dx.doi.org/10.1299/jsmeicjwsf.2005.255.

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33

Isoguchi, Osamu, and Hiroshi Kawamura. "Coastal Wind Jets Flowing into the Tsushima Strait and Their Effect on Wind-Wave Development." Journal of the Atmospheric Sciences 64, no. 2 (February 1, 2007): 564–78. http://dx.doi.org/10.1175/jas3858.1.

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Abstract Coastal wind jets that flow into the Tsushima Strait, Japan, and their effects on wind waves are investigated using synthetic aperture radar (SAR) images and altimeter-derived wind and waves. The coastal wind jets appear in 7 of 28 SAR-derived wind fields under the conditions of ambient southeasterly winds. Atmospheric conditions corresponding to the appearance of the coastal wind jets are examined by a high-resolution atmospheric community model, which indicates that stratified flows are influenced by the land topography and then pass through the strait forming low-level jet flows. Sensitivity experiments reveal that easterly to southerly stratified flows are a necessary condition for a jet’s formation and the degree of its enhancement is mostly controlled by the Froude number of the upstream flows. Atmospheric conditions in which the SAR observed the coastal jets meet the model-derived necessary conditions, which corroborate the validity of the model simulation and the jet’s formation mechanism. Next, the authors present a case study concerning effects of the coastal jets on wind-wave development by using altimeter-derived wind speed and significant wave height (SWH). Both profiles show similar convex spatial distribution within the wind jet range. The nondimensional SWH and fetch indicate agreements with the empirical fetch graph formula, suggesting that the wind waves are locally developed by the coastal jet. Through investigation of ship-based climatological data, it is found that the coastal jets occur frequently in midsummer due to prevailing southeasterly flows, which is accounted for by the seasonal evolution of the Asian summer monsoon.

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34

Dekrét, Anton. "On quasi-jets." Časopis pro pěstování matematiky 111, no. 4 (1986): 345–52. http://dx.doi.org/10.21136/cpm.1986.118284.

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35

Fendt, Christian, and Somayeh Sheikhnezami. "BIPOLAR JETS LAUNCHED FROM ACCRETION DISKS. II. THE FORMATION OF ASYMMETRIC JETS AND COUNTER JETS." Astrophysical Journal 774, no. 1 (August 8, 2013): 12. http://dx.doi.org/10.1088/0004-637x/774/1/12.

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36

Lim, A. J. "Variable stellar jets -- II. Precessing jets and stagnation knots." Monthly Notices of the Royal Astronomical Society 327, no. 2 (October 21, 2001): 507–16. http://dx.doi.org/10.1046/j.1365-8711.2001.04772.x.

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37

Tyliszczak, Artur. "Multi-armed jets: A subset of the blooming jets." Physics of Fluids 27, no. 4 (April 2015): 041703. http://dx.doi.org/10.1063/1.4917179.

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38

Jacquemin-Ide, J., J. Ferreira, and G. Lesur. "Magnetically driven jets and winds from weakly magnetized accretion discs." Monthly Notices of the Royal Astronomical Society 490, no. 3 (October 3, 2019): 3112–33. http://dx.doi.org/10.1093/mnras/stz2749.

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Abstract Semi-analytical models of disc outflows have successfully described magnetically driven, self-confined super-Alfvénic jets from near-Keplerian accretion discs. These jet-emitting discs (JEDs) are possible for high levels of disc magnetization μ defined as μ = 2/β, where beta is the usual plasma parameter. In near-equipartition JEDs, accretion is supersonic and jets carry away most of the disc angular momentum. However, these solutions prove difficult to compare with cutting-edge numerical simulations, for the reason that numerical simulations show wind-like outflows but in the domain of small magnetization. In this work, we present for the first time self-similar isothermal solutions for accretion–ejection structures at small magnetization levels. We elucidate the role of magnetorotational instability-like (MRI) structures in the acceleration processes that drive this new class of solutions. The disc magnetization μ is the main control parameter: Massive outflows driven by the pressure of the toroidal magnetic field are obtained up to μ ∼ 10−2, while more tenuous centrifugally driven outflows are obtained at larger μ values. The generalized parameter space and the astrophysical consequences are discussed. We believe that these new solutions could be a stepping stone in understanding the way astrophysical discs drive either winds or jets. Defining jets as self-confined outflows and winds as uncollimated outflows, we propose a simple analytical criterion based on the initial energy content of the outflow, to discriminate jets from winds. We show that jet solution is achieved at all magnetization levels, while winds could be obtained only in weakly magnetized discs that feature heating.

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39

Okita, Yuji, Katsutaka Nakamura, Yuuta Shiizaki, and Daisuke Nobuta. "LASER OBSERVATION ON THE INNER FLOW STRUCTURE OF WATER JETS(Water Jet)." Proceedings of the International Conference on Jets, Wakes and Separated Flows (ICJWSF) 2005 (2005): 337–42. http://dx.doi.org/10.1299/jsmeicjwsf.2005.337.

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40

Takaichi, Naoaki, Naoya Shigemori, and Katsuhiro Yamamoto. "BEHAVIOR OF HIGH-SPEED PULSE WATER JETS IN THE ATMOSPHERE(Water Jet)." Proceedings of the International Conference on Jets, Wakes and Separated Flows (ICJWSF) 2005 (2005): 343–48. http://dx.doi.org/10.1299/jsmeicjwsf.2005.343.

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41

Tsujimoto, Koichi, Toshihiko Shakouchi, Shuji Sasazaki, and Toshitake Ando. "Direct Numerical Simulation of Jet Mixing Control Using Combined Jets(Numerical Simulation)." Proceedings of the International Conference on Jets, Wakes and Separated Flows (ICJWSF) 2005 (2005): 725–30. http://dx.doi.org/10.1299/jsmeicjwsf.2005.725.

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42

Ferreira, Jonathan, and Pierre Olivier Petrucci. "Jet launching and field advection in quasi-Keplerian discs." Proceedings of the International Astronomical Union 6, S275 (September 2010): 260–64. http://dx.doi.org/10.1017/s1743921310016121.

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AbstractThe fact that self-confined jets are observed around black holes, neutron stars and young forming stars points to a jet launching mechanism independent of the nature of the central object, namely the surrounding accretion disc. The properties of Jet Emitting Discs (JEDs) are briefly reviewed. It is argued that, within an alpha prescription for the turbulence (anomalous viscosity and diffusivity), the steady-state problem has been solved. Conditions for launching jets are very stringent and require a large scale magnetic field Bz close to equipartition with the total (gas and radiation) pressure. The total power feeding the jets decreases with the disc thickness: fat ADAF-like structures with h ~ r cannot drive super-Alfvénic jets. However, there exist also hot, optically thin JED solutions that would be observationally very similar to ADAFs.Finally, it is argued that variations in the large scale magnetic Bz field is the second parameter required to explain hysteresis cycles seen in LMXBs (the first one would be Ṁa).

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43

Waliszewski, Włodzimierz. "Jets in differential spaces." Časopis pro pěstování matematiky 110, no. 3 (1985): 241–49. http://dx.doi.org/10.21136/cpm.1985.118231.

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44

Pfister, Michael. "Deflector-generated jets." Journal of Hydraulic Research 47, no. 4 (2009): 000. http://dx.doi.org/10.3826/jhr.2009.3525.

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45

Hautmann, F. "QCD and Jets." Acta Physica Polonica B 44, no. 4 (2013): 761. http://dx.doi.org/10.5506/aphyspolb.44.761.

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46

Falle, S. A. E. G., D. E. Innes, and M. J. Wilson. "Steady stellar jets." Monthly Notices of the Royal Astronomical Society 225, no. 4 (April 1, 1987): 741–59. http://dx.doi.org/10.1093/mnras/225.4.741.

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47

Falle, S. A. E. G. "Self-similar jets." Monthly Notices of the Royal Astronomical Society 250, no. 3 (June 1, 1991): 581–96. http://dx.doi.org/10.1093/mnras/250.3.581.

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48

Langenberg, Heike. "Jets of mystery." Nature Geoscience 1, no. 12 (December 2008): 816. http://dx.doi.org/10.1038/ngeo373.

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49

Stuetz, Engelbert. "Colliding water jets." Physics Teacher 57, no. 3 (March 2019): 208. http://dx.doi.org/10.1119/1.5092500.

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50

Smith, Michael D. "Slender elliptical jets." Astrophysical Journal 421 (February 1994): 400. http://dx.doi.org/10.1086/173659.

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