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PoS(FRAPWS2018)061 https://pos.sissa.it/ rodynamics and radiation pressure ]. Explosive formation of jets in the tinuously for a long time, and explo- of jet collimation may be connected r beam, and focus [5,6]. nected with supernovae, gamma ray nside a , acceleration by rel- ctive galactic nuclei (AGN). The mech- ny, Moscow reg., Russia e 31, Moscow 115409, Russia ive Commons onal License (CC BY-NC-ND 4.0). ∗ [email protected] anisms of jet formation may be divided in regular, acting con Jets are observed in young stellar objects, X-ray sources, a sive ones [1]. Continuous mechanisms are related with elect acceleration, hydrodynamical acceleration in the nozzle i with magnetic confinement, or a pressure oflaboratory external is gas modeled [2-4 in the experiments with powerful lase ativistic beam of particles.bursts Explosive and jet explosive events formation in is galactic con nuclei. Mechanisms Speaker. ∗ Copyright owned by the author(s) under the terms of the Creat c Frontier Research in Astrophysics - III (FRAPWS2018)28 May - 2 June 2018 Mondello (Palermo), Italy Attribution-NonCommercial-NoDerivatives 4.0 Internati and Moscow Institute of Physics and Technology MIPT, Dolgoprud G. S. Bisnovatyi-Kogan Space Research Institute, Russian Academy ofProfsoyuznaya Sciences, 84/32, Moscow 117997, Russia and National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), Kashirskoe Shoss E-mail: Mechanisms of astrophysical jet formation, and comparison with laboratory experiments

PoS(FRAPWS2018)061 (2.1) 2, The . magnetic 0” ∼ re presented in G. S. Bisnovatyi-Kogan 47 GHz), in the optics (HST, -rotating disk) had been inves- rounded by , was Gs. At presence of large-scale 2, in the optics (HST, F814W), 33) was observed in radio band . They show behaviour, . angular resolution 2 . The observations of IC 4296 croquasar GRS 1915+105, have . ted ejection from accretion disks 10 ” as supported by observations, and es, and two flows meat each other 0” d. At big distances from BH the extent of the jet is about 360 kpc , and were called as by Chandra telescope, with angular supermassive black holes (SMBH). The jet in the A galaxy M87 rection. Collision of flows leads to 10 ted in Fig.1. ∼ 3-0.5) of the rest mass energy flux. all far from BH, in the radial accretion nd begins to change the flow patterns. − ellar-like objects. AGN jets have been , 7 ent electrical conductivity was estimated cretion of non-rotating gas, with initially nductivity, and radial matter flow to BH in ρ / P 2 p c h 1 π 4 ˜ α = t σ - viscosity in the non-magnetized disks, see next section. A α 1. The observations of jet are summarized in [10], and a . 0” ∼ Jets are observed in objects with black holes, where collima First model of AGN & , as a supermassive , sur Much longer and fainter jet in radiogalaxy IC 4296 (PKS 1333- Accretion disk around BH with large scale magnetic field (non The jet in the quasar 3C 273 was observed in radio (MERLIN, 1.6 and in soft X-ray band (0.2-8 keV) by Chandra telescope, with is expected. Non-relativistic jetsstudied are in observed many in wavebands young of st was the observed electromagnetic in spectrum. radio (14GHz, VLA) with angular resolution suggested by D. Lynden-Bell [7] innow the it year is 1969. widely This accepted model that w About and 10 AGN HMXR nuclei (high contain stellarwhich, mass after black appropriate holes) scaling, are is found[8]. similar in the to the AGN SMBH Astrophysical jet formation 1. Introduction magnetic field the efficiency of accretion is always large (0. field strength in the vicinity of a stellar BH may reach 10 Fig.2. (VLA), at bands between 1.3 andjet 20 are cm, with summarized a in bestRadio resolution [11], 3 observations and (MERLIN, are 5GHz) presented ofbeen in a presented Fig.3. in jet [12], ejection see Total in Fig.2 in the this mi paper. 2. Accretion disk models 2.1 Large scale magnetic accretion analogous to the turbulent tigated in [13, 14]. Self-consistentuniform model of magnetic stationary field, ac intoaccretion a is black almost radial. hole The (BH) magneticflow energy, was which is constructe is increasing sm faster than allClose other to types the BH of the the matter energy,in flows a the almost symmetry along magnetic plane, field perpendiculardevelopment lin of to a the turbulence, finite magnetic turbulent field electricalthe co di accretion disk, through magnetic field lines. The turbul in [14] as F622W, centered at 6170A), and in softresolution X-ray band (0.2-8 keV) observations of M87 jet are summarized in [9], and are presen PoS(FRAPWS2018)061 in com- is equal P Ω ∇ G. S. Bisnovatyi-Kogan e horizontal, and an overlay of isk model were used in [7]. An- ges are displayed using a logarithmic tic field strength, and self-consistent gular velocity of the disk y induced toroidal electrical currents uggested in the paper [15], was more he F814W filter. Third panel: Adaptively le radial equilibrium equation denoting ks. The small thickness of the disk in 87 in 0.”20 pixels. Fourth panel: Smoothed Hz using the VLA. The spatial resolution is mages have been registered to each other to d version of the HST image, designed to match aling is linear, from [9] 2 . indicate to small importance of the pressure gradient r ≪ h , K Ω Images of the jet in M87 in three different bands, rotated to b Algebraic relation for construction of the thin accretion d Figure 1: Astrophysical jet formation optical contours over the X-ray image.about 0.”2. Top: Image Second at panel: 14.435 Thesmoothed G Chandraimage HST Planetary of Camera the X-ray image emissionChandra in from image t the overlaid jet with of contours M of a Gaussian-smoothe about 0.”05 using thestretch position to of bring the out faint core. features, while The the HST X-ray image and sc VLA ima the Chandra point response function. The X-ray and optical i to the Keplerian one Formation of nonrotating disk around BH, supportedpicture by of magne accretion with accountin of the magnetic accretion field disk created are presented b in Fig. 5. 2.2 Standard accretion disk model other presentation, based on soattractive, called and "alpha was disk" used model, in s comparison with different its types radius of accretion dis parison with gravity and inertia forces.the That balance leads between to the a last simp two forces occurring when the an PoS(FRAPWS2018)061 G. S. Bisnovatyi-Kogan 1 bins overlaid with a version . 05 using the position of knot A1. . ge at 1.647 GHz using the MERLIN tch the X-ray imaging resolution. The 3C 273 in 0” ge in the F622W filter (centered at 6170 Å). o about 0” nd curvature, but the X-ray emission fades to The radio emission is much fainter at knot A1 3 Images of the jet in 3C 273 in three differentbands. Left: Ima Right: Raw Chandra image of the X-ray emission from the jet of array. Middle: Planetary Camera ima Figure 2: Astrophysical jet formation of the HST image smoothedX-ray with and a optical Gaussian images profile have been in registered order to to each ma other t The overall shape of thethe jet end is of remarkably the similar jet,and in so is length individual displayed a C with knots a are logarithmic not scaling, from discernible. [10] PoS(FRAPWS2018)061 rom [11] G. S. Bisnovatyi-Kogan 4 Donald Lynden-Bell and Nikolay Shakura Figure 4: Jet in the IC 4296 at 20 cm with 3".2 resolution, f Figure 3: Astrophysical jet formation PoS(FRAPWS2018)061 (2.2) (2.3) (2.6) (2.4) (2.5) is a sound speed, ρ / . G. S. Bisnovatyi-Kogan P h ropic pressure, so that t p ρυ = = s . υ η Ω tationary accretion of non-rotating dr d r is an integration constant equal to , η P ole. in is a component of the viscous stress j α = . ϕ − 2 ϕ r . / r t t 1 2 librium is substituted by an algebraic one, = / the accreting matter outside the disk, is shown,  2 1 s , enerated in the non-rotating accretion disk, from ,  2 in 3 ϕ r r r P ρ component of the Euler equation has an integral GM K αρυ ht 2 ϕ  Ω 2 5 −  2 = r = K = 1 π K s in Ω 2 j υ Ω t − ≈ = h ρυ )= Ω ≈ in is an average turbulent velocity, j t Ω υ dr − d j ), ( s hr t ˙ M αυ ρυ = = t is the specific angular momentum, ϕ υ r t 2 r of the stress tensor is taken [15] proportionally to the isot Ω ϕ r t = r 0 is a mass flux per unit time into a black hole, ϕ > υ Sketch of the magnetic field threading an accretion disk in a s disk model ( ˙ = M α j [14], (right). gas. Increase of the field owingfrom to [13] magnetic (left). field Similar freezing, in picture, with account of the field g Figure 5: Astrophysical jet formation in a stationary case written as tensor, the component For a the differential equationdetermining for the a half-thickness vertical of equi the disk in the form The balance of angular momentum, related to the the specific angular momentum of matter falling into a black h Here In the PoS(FRAPWS2018)061 G. S. Bisnovatyi-Kogan of a keplerian accretion disk critical luminosity. I - radiation K. The model of accretion disk 9 e X ray source X-1, and 10 ter with low angular momentum falls n disk around a black hole has three ], see Fig.7. It was shown in [17], that ]. Mechanism for producing fast par- ong poloidal magnetic field will arise. − e convectively unstable, and, therefore, 8 a are indicated, from [18]. region, scattering. III - gas-dominated 6 Alexandr Ruzmaikin and Sergey Blinnikov Figure 6: Sketch of picture of a disk accretion on to a black hole at sub- Self-consistent structure of the optically thick accretio A presence of a large scale magnetic field in the inner regions with a hot coronatransition was between used different states for in explanation this of source [17]. properties of th Figure 7: regions, depending on the origin ofinner, pressure radiation and dominated opacity regions [16 ofproduce the a accretion hot disk corona ar with electron temperature about 10 2.3 Convection and hot corona Astrophysical jet formation dominated region, electron scattering.region, II Krammers opacity; - convective gas-dominated region, and hot coron create mechanism of particle ejectionticles and is jet analogous formation to [17 theinto the process. black If hole magnetized (in mat addition to the disk accretion), a str PoS(FRAPWS2018)061 1 . 0 (3.1) ≈ c / in which υ pairs to be B e ) c + / e υ ( ≈ G. S. Bisnovatyi-Kogan Mev where E )] he disk owing to the Faraday Gauss 7 10 [19], see Fig.8. ( Gauss, such will generate et. Similar model of a jet formation, energy along the accretion disk was only advective models, qualitatively / ity, approaching Eddington limit, and ld of strength 7 B dels are characterized by decrease of a flow of high-energy particles along the [ ccretion disk is optically thick at larger, 10 4 ition between these regions [21, 22]. Set 10 ≈ 19]. · B 3 , P ≈ α keV. It would be possible here for 7 = Be 5 ) ϕ r c 10 t / υ ≈ ( R ≈ P" viscosity prescription α cm is the characteristic scale. In a field 7 Sketch of the electromagnetic outflows from the two sides of t 10 ≈ Standard (local) accretion theory is not correct at luminos R unipolar dynamo action of a rotating magnetized disk, from [ 3. Solutions with advection and optically thin at smaller radiuses, with a gradual trans in the vicinity of ataken last into stable account orbit in around [20]. BH.different Advection from In of standard very ones, luminous give accretion propervertical disks results. optical These depth mo with decreasing of a radius, so that a of equations for " Figure 8: electrons are accelerated to energies Astrophysical jet formation By analogy to , rotation will generate an electric fie and formed and to participate in themagnetic synchrotron field radiation. should The be visible aswith a account highly of collimated dynamo flow processes - was j considered in the paper with energies up to PoS(FRAPWS2018)061 (3.4) (3.5) (3.2) (3.3) g term ts of general ion, G. S. Bisnovatyi-Kogan . 1 −  2 ∗ τ 2 , 3 1 + − 0  onal equations was obtained in [21]. τ 4 . thin transition were take from [23] as 2 ∗ 3 τ 2 h 2 3 + 4 / , which takes place in a region with inter- 1 1 2 + α / T 1 τ 0 acT 2 ) τ 4  ρ α 3 0 ≫ τ τ 21 4 0 0 + 8 3 τ τ 1 10 · +  = ( 2 1 . c ∗ 4 5  0 τ τ 4 ≃ 3 aT 3 2 α aT Igor Novikov and Richard Lovelace τ = + − T Q 1, with advection, had been solved in [21]. Radiative coolin R ρ Figure 9: ≤ is the optical depth with respect to bremsstrahlung absorpt of Paczynski-Witta [24] was used, accounting for some effec = α α g P τ ϕ is a total Thomson scattering depth of the disk and h κρ is a parameter, = α 0 τ , and equation of state, describing smooth optically thick- − is the effective optical depth valid for the case Q where Astrophysical jet formation mediate optical depths, relativity: A numerical solution of theGravitational set potential of the following non-dimensi Here PoS(FRAPWS2018)061 . ith- in (3.7) (3.9) (3.6) (3.8) ℓ (3.10) (3.11) , where Edd ˙ , and M s c / ˙ , M υ 2 s , = c R , r β m D N = G. S. Bisnovatyi-Kogan 0, ˙ .  T 1 50 . 1 − = , ion of equations (3.6)-(3.8), − 2 2 s P ρ m  c the effective optical depth (right) υ 2 ∗ =  τ 2 3 2 s optically thin region exceeds 500 − c + . Dashed lines correspond to the solu- ) 0 ⊙ 2 2 τ 4 , 3 M − − T 2 s . x x 10 + c ( R 3 he mass accretion rate higher than the critical , 1 r 2 s 2 = g , c are given in Figs.10,11, from [25]. υ r = + ) 2 BH α  g D N ∗ P  r P 0 GM M − + ( τ 2 4 9 = r ) 3 T = 2 in ′ 2 r , ℓ υ = υ ) + β 1 − ∗ , from [25]. r g 5 and 1 = r . x x 0, and the thin solid line to ˙ ϕ ( 0 . (  , ∗ 50 (from the center to the edge of the picture respectively). x Ω ≡ g τ 4 36 = r ∗ , c = 3 r − 36. Dotted lines correspond to the non-physical solutions w ) α Ω = ; aT ∗ 2 m T r = ˜ m ( Ω = σ = 0 cr /  τ p e ˙ P Ω m 2 ) x 2 s pair creation takes place [26]. β denote algebraical expressions, depending only on < c 2 36 and ˙ , c − − m D e 2 = cGMm 1 + c + ( π GM cr e 1 4 and ˙ m = = = N g = s ′ s r c c Edd m r L , , g 2 r r c / The dependence of the Thompson scattering depth (left), and = is a specific angular momentum on the last stable orbit. Solut Edd x L in ℓ = Edd ˙ on the radius , and for the models with M Figure 10: Astrophysical jet formation In a rotating BH, with the Kerr metric, the temperature in the keV, when an intensive where the notations out advection for ˙ with account of (3.9)-(3.11), for Here tions without advection and ˙ one. Thick solid line corresponds to ˙ Solid lines correspond to the solutions with advection and t PoS(FRAPWS2018)061 , from x ≡ ∗ r G. S. Bisnovatyi-Kogan odels as in Fig.10; 10 Julia Artemova and Alexandr Klepnev Figure 12: The dependence of the temperature on the radius for the same m Figure 11: Astrophysical jet formation [25]. PoS(FRAPWS2018)061 G. S. Bisnovatyi-Kogan 0”4); an optical V band (middle, mation [29], where initial charge tions of the jet in M87 [28], that ic field, preventing jet expansion and ectrical current, as in a capacitance- stinctly show existence of bright knots Figs.1,2. related, see Fig.14. 0”7; 0.1 - 10 keV band) image. The labels in . N is the nucleus, from [27] (left). Scheme of 4] (right). 11 Gray-scale representations of a 6 cm radio (top; resolution It was shown by optical photoelectric polarization observa Observations of extragalactic jets in different objects di This behavior was interpreted in the model of magnetic colli Figure 13: resolution 0”7); and the Chandrathe X-ray lower panel (bottom, refer resolution to the knots vertically above the label magnetic collimation due to torsional oscillations, from [ along a whole jet in different wavelengths, Fig.13, see also polarization angles in neighboring blobs are orthogonally separation in the neighboringinductance blobs system. leads This current to produces oscillating azimuthal magnet el Astrophysical jet formation 4. Magnetic jet collimation PoS(FRAPWS2018)061 1, = (4.3) (4.2) (4.1) γ , with γ ρ K = remains zero during G. S. Bisnovatyi-Kogan , P . Ω 0 K ω is a size of the blob in the = √ τ D = , 0 0 0 at R = , differential equations have a form = z The polarization angles in neighboring ω , where z υ one non-dimensional parameter c , , ential equation is derived, and solved = ons of a cylinder with elongated mag- gular velocity / en circle in the lower left, from [28] (left). 1 2 ere charge separation is not necessary. , ith charge separation, there is a cylinder 2 0 D  ) c equation of state = tively the range of parameters where jets R z lde". 0 K ∼ e cylinder axis. The stabilizing azimuthal , y ω t ω Ω ( 0 b ; aphragms used are shown in the upper left of the osc z ) cillations in the blob, from [29] (right). = Ω C P τ r 0 2  a = , m 12 sin 0 ϕ ˜ R R 1 D υ KC 0 a π a − 2 , 1 ) = ( z = y z 1 , t , ( D = 0 ˜ R R ra τ dz d = = r y υ , , z t ω = = τ dy d τ Photoelectric polarization observations of the jet in M87. is the frequency of radial oscillations. In these variables ω Magnetic collimation, connected with torsional oscillati Approximate simplified model is developed.numerically, Ordinary what differ gives a possibility tomay estimate be quantita stabilized by torsional oscillations. The polytropi with a periodically distributed initialmagnetic rotation field around is th created here by torsional oscillations, wh netic field, was considered in [4]. Instead of initial blobs w jet, see Fig.14. blobs are orthogonally related. Thefigure. relative The sizes position of of the the di nucleusMagnetically of collimated M87 jet is by shown inductance-capacitance by os a small op disappearance. The period of oscillations should be Figure 14: Therefore, the problem is reduced to a system (4.3) with only Astrophysical jet formation Here introduce non-dimensional variables in the plane, where an was considered. Using approximate relations oscillations. the variables in this plane are denoted by "ti PoS(FRAPWS2018)061 z z y 1 ≈ . 2 2 n α 2 = D c gential 2 π D 2 < 2 s 2 υ in rather peculiar to 3 groups. s nonlinear system D 1.5 G. S. Bisnovatyi-Kogan rom 1, there is a larger r several low-amplitude on (4.3) returned to the ming separate blobs, but time increases, and at 1 0 Ω 3 and larger the radius goes to ceed the light velocity, so the = 0.5 ro depends on D ude and large-amplitude oscillations, haos of these oscillations is analysed in 0 ome average value, forming rather com- 1 0

-1 -2 -3 -4 -5 -6 2, the jet should contain baryons, which sented in Figs. 1-18 of [4]. Frequency of

uld be enough also for the whole period ,z y, / . The solution of this system was obtained c (upper curve), and non-dimensional velocity D 1, has a physical sense only at y = =2.5. From 0 D y 13 between 2.28 and 2.9 the dependence of the radius at is the space period of the torsional oscillations along 7 D 0 1 for a strongly non-linear oscillations we obtain a very =2.4, 2.6; or goes trough very large radius, and returned . 10 z 0 , D 1 (right). . At . ∼ 0 π z 3 2 = D τ 2 n = = α D k , 1 . While in the intermediate collimation regime the outer tan 100 100, like at < 2 4 c , the amplitude of torsional oscillations n ≤ D α < τ , time 0 1 (left), and A 2 s . 2 υ kV 50 n = are integrals of motion, see [4] for details. Solution of thi between 1.5, and 3.1. Roughly the solutions may be divided in α D m D = C is taken from linear approximation. When y(0) is different f 5 (Fig.15, right). before the right side of the second equati . < 2.1 there is no confinement, and radius grows to infinity afte ω = 2.28 and larger the radius finally goes to zero with time, for 2 ω Time dependence of non-dimensional radius D D and < 0 0 2 1 b

is Alfven velocity. Taking

0.6 0.4 0.2 2.4 2.2 1.8 1.6 1.4 1.2 0.8 τ ,z y, -0.2 -0.4 C A V 1. At 2. With growing of On the edge of the cylinder the rotational velocity cannot ex 3. At , where 2 n 2 α c 40 with different behavior, depending on way, and may happen at with time may be very complicated,which consisting finally of lead low-amplit to zero. The time at which radius becomes ze (lower curve), for axis, changes qualitatively with changing of the parameter moderate restriction back to zero value at very large time Figure 15: positive value. The results of numericaloscillations solution are repre Astrophysical jet formation where numerically for oscillations. variety of solutions: regular and chaotic.[30] Development of c solution with initial conditions, corresponding to of the time. To have the sound velocity not exceeding velocity is not changing significantly, this restriction wo radius is not growing to infinity,plicated but is curve (Fig.15, oscillating around left). s zero at PoS(FRAPWS2018)061 m, and T is the target µ G. S. Bisnovatyi-Kogan jet should be larger than t, heated by the laser beam, o heating of the foil, with the cosecond laser facility [31], see beams of accelerated protons using . olved in 2-D problem with a finite ymmetric approximation, assuming ibution of beams of accelerated protons. o compare parameters of laboratory s means that the mathematical model , 3 , icknesses of 11 - 80 3 e experiment and the region of modeling cm/s, − cm, g/cm 10 18 cm Gs, K. s, 10 26 2 3 10 8 − − − 11 × × 14 Jets from AGN nuclei (VLBI) 3 10 3 10 10 10 10 cm s 18 9 3 10 10 3 × × − ) ) g/cm 3 3 Gs m); from [32]. cm K 1 µ cm/s ÷ 26 ÷ 2 − 11 9 − 3 − 3 . . 0 10 0 10 10 10 10 ======( = ( n H T Laboratory jet after scaling, from [32] x υ ρ t m) or Ta (50 µ cannot be very small, and its input in the total density in the Scheme for the experiments investigating the spatial distr 0 ρ Experiments aimed at studying the spatial distributions of Analysis of the experiment showed the formation of a jet due t Numerical simulations of the flow of the matter from the targe about 30% [4]. 5. Laboratory experiments and numerical simulations CR-39 track detectors were carriedFig.16 out at the Neodim 10- TW pi Figure 16: Astrophysical jet formation density geometry of the incident laser beamfor not the being formation important. of Thi thethat jet the can laser-heated be spot constructedelectrical is in conductivity, circular. an without gravity. axially MHD The s scheme equations of were th s have been presented inexperiments [32]. with jets Similarity on the conditions from permit AGN’s and t quasars, see Tabl of Cu (30 and 50 A, B, C are the CR-39 track detectors, F are filters of Al with th PoS(FRAPWS2018)061 (5.1) ameter max max Z R [32]. const G. S. Bisnovatyi-Kogan EdV = Σ B d R v 760, 18-02-00619, and Funda- 0 clear processes) d by O.D. Toropina, is presented in ic) ? ssure or explosions) BLOBS -!? putations are performed for the target nitial magnetic pressere . thod and numerical results are presented e given. The ring structure, observed on 0 0 2 2 s A c V γ 2 = max R jet 15 - 2 0 0 P H π 8 = β is a background density. The important non-dimensional par 0 ρ Experiment scheme (left). Region of modeling (right), from , where 0 ρ Jets in Lab should help to answer! Figure 17: 300 ≈ ρ 1. Jet origin (blobs or continuous injection; radiation2. pre Jet collimation (magnetic, or outer pressure, or kinemat 3. Jet constitution (baryonic or pure leptonic) Baryonic4. -! Particle acceleration (shocks, reconnection, kinetic) 5. Radiation mechanisms (synchrotron, inverse Compton, nu This work of was partially supported by RFBR grants 17-02-00 The example of results of numerical calculations, performe is a ratio of the initial gas pressure at the jet origin to the i β Astrophysical jet formation 6. Conclusion - Problems Acknowledgments mental Research Program of Presidium of the RAS #28. the photo of the experiment, is visible on this figure. The com are presented in Figs.17. The detailed descriptionin of [32]. the me Fig.18 from [32], where detailed results of calculations ar density PoS(FRAPWS2018)061 e left column, G. S. Bisnovatyi-Kogan ence of the poloidal magnetic 16 1 at time moments t = 5, t = 10, t = 25, t = 45. Density is given in th . 0 = Time dependence of the flow, induced by the laser beam, in pres β field with Figure 18: Astrophysical jet formation temperature is to the right, from [32]. PoS(FRAPWS2018)061 , 968 (2006) 637 , 119 (1996) G. S. Bisnovatyi-Kogan , 369 (1969), , 369 (1969) 13 , 401 (1976) 456 , 45 (1974) 13 42 28 , 215 (1992) 358 ch, E. Terlevich, R. Terlevich and A. , 865 (1999) , p.311 (2007) , 191 (1976) 2 , 409 (2010) v. , , L17 (1995) 304 viet Astronomy, , 283, (1981) nd Space Sci. nd Space Sci., , 23 (1980) 53 I.V., Novikov I.D., ApJ I.V., Novikov I.D., in "Astrophysics and , L167 (2001) , 306 (1986) 31 s Novikov I.D., ApJ . Observ., no. 58, pp. 175-210 (1985). In n F. Nature 296 88 , 683 (2002) n.Lett. ution and Stability. Springer-Verlag Berlin 549 302 564 17 , 395 (1974) , 337 ( 1973) , 41 ( 2004) , 997 ( 2010) 169 24 , 457 (2007) 34 36 376 , 133 (2002) , 756 (1973) , 649 (1976) , 690 (1969) 16 568 262 223 , 340 (1959) 130 ´ ´ nski B., Bisnovatyi-Kogan G., Acta Astronomica nski B., Wiita P.J., Astronomy and Astrophysics Russian. Cosmology After Gamow". Eds. G. S.Zhuk. Bisnovaty-Kogan, Cambridge S. Scientific Sili Publishers, Cambridge, UK, 2007 Heidelberg, p.291 (2011) [7] Lynden-Bell D. Nature, [6] Belyaev V.S., Quantum Electronics, [8] Mirabel I.F., Rodriguez L.F., Cordier B., Paul J., Lebru [4] Bisnovatyi-Kogan G.S., MNRAS [5] Krauz V.I. et al., Physics of Plasma [9] Marshall H.L., Miller B.P., Davis D.S., et al. ApJ, [1] G.S. Bisnovatyi-Kogan, R.V.L. Lovelace, Astron. Ap., [2] G.S. Bisnovatyi-Kogan, B.V. Komberg, A.M. Friedman, So [3] Blandford R.D., Rees M.J., MNRAS, [19] Lovelace, R.V.E. Nature [20] Paczy [21] Artemova Yu.V., Bisnovatyi-Kogan G.S., Igumenshchev [23] Artemova I.V., Bisnovatyi-Kogan G.S., Bjoernsson G., [22] Klepnev A.S., and Bisnovatyi-Kogan G.S., Astrophysic [24] Paczy [25] Artemova Yu.V., Bisnovatyi-Kogan G.S., Igumenshchev [26] Bisnovatyi-Kogan G.S. Stellar Physics 2: Stellar Evol [27] Wilson A.S., Yang Y., ApJ [28] Hiltner W.A., ApJL [29] Bisnovatyi-Kogan G.S., Komberg B.V., Fridman A.M., So [18] Bisnovatyi-Kogan G.S. Biulleten’ Abastuman. Astrofiz [10] Marshall H.L., Harris D.E., Grimes J.P., et al. ApJL, Astrophysical jet formation References [11] Killeen, N. E. B.; Bicknell, G. V.; Ekers, R. D. ApJ, [12] Fender R.P., Garrington S.T., McKay D.J., et al., MNRAS [13] Bisnovatyi-Kogan G.S., & Ruzmaikin A.A., Astrophys. a [17] Bisnovatyi-Kogan G.S., and Blinnikov S.I., Sov.Astro [16] Shakura N.I. & Sunyaev R.A., A&A, [15] Shakura N.I., Sov. Astron., [14] Bisnovatyi-Kogan G.S., & Ruzmaikin A.A., Astrophys. a PoS(FRAPWS2018)061 . e , , 2 62 416 powerful watt/cm 20 and 10 18 G. S. Bisnovatyi-Kogan he laboratory, and how , 477 (2006) 16 enters, the jet is collimated by toroidal aser Phys. oiseenko S.G., et al. Astronomy Reports, watts? supko O.Yu., Krivosheev Yu.M., MNRAS 18 18 Gs, created by the flux of rapid electrons, knocked out from th 8 10 In my opinion it is a magnetic collimation. A measurements of the magnetic field in the jet, created by the The peak intensity of the laser beam is between 10 − 7 10 = ϕ What is the most realistic model of the jet collimation? B Did I read the laser power by right: 10 How are the magnetic fields that collimate the jet created in t 747 (2011) 162 (2018) Astrophysical jet formation [30] Bisnovatyi-Kogan G.S., Neishtadt A.I., Seidov Z.F., T target. [31] Belyaev V.S. , Vinogradov V.I. , Matafonov A.P. et al., L large is the field strength? BISNOVATYI-KOGAN: BISNOVATYI-KOGAN: DISCUSSION JIM BEALL: [32] Belyaev V.S., Toropina O.D., Bisnovatyi-Kogan G.S., M D. BISIKALO: S. FUNK: BISNOVATYI-KOGAN: laser beam, is a very complicated task.magnetic According fields to experim