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Colliding winds Colliding winds in pulsar in pulsar binaries binaries S.V.Bogovalov S.V.Bogovalov 1 1 , , A.V.Koldoba A.V.Koldoba 2 2 ,G.V.Ustugova ,G.V.Ustugova 2 2 , D. , D. Khangulyan Khangulyan 3 , F.Aharonian , F.Aharonian 3 3 1-National Nuclear Research University (Moscow) 1-National Nuclear Research University (Moscow) 2-Institute of applied mathematics RAN (Moscow) 2-Institute of applied mathematics RAN (Moscow) 3-Max-Planck-Institute for Nuclear Physics (Heidelberg) 3-Max-Planck-Institute for Nuclear Physics (Heidelberg)

Colliding winds in pulsar binaries

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Colliding winds in pulsar binaries. S.V.Bogovalov 1 , A.V.Koldoba 2 ,G.V.Ustugova 2 , D. Khangulyan 3 , F.Aharonian 3 1-National Nuclear Research University (Moscow) 2-Institute of applied mathematics RAN (Moscow) 3-Max-Planck-Institute for Nuclear Physics (Heidelberg). Candidates. - PowerPoint PPT Presentation

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Page 1: Colliding winds in pulsar binaries

Colliding winds in Colliding winds in pulsar binariespulsar binaries

S.V.BogovalovS.V.Bogovalov11,,

A.V.KoldobaA.V.Koldoba22,G.V.Ustugova,G.V.Ustugova22, D. , D. KhangulyanKhangulyan33, F.Aharonian, F.Aharonian33

1-National Nuclear Research University (Moscow)1-National Nuclear Research University (Moscow)

2-Institute of applied mathematics RAN (Moscow)2-Institute of applied mathematics RAN (Moscow)

3-Max-Planck-Institute for Nuclear Physics (Heidelberg) 3-Max-Planck-Institute for Nuclear Physics (Heidelberg)

Page 2: Colliding winds in pulsar binaries

Candidates Candidates

PSR 1259-63/2883PSR 1259-63/2883 LS 5039LS 5039 LSI +61303LSI +61303 Cygnus X-1Cygnus X-1

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System PSR1259-63/SS2883System PSR1259-63/SS2883 Companion star PulsarCompanion star PulsarM ~ 10 Solar mass P=47.7 msM ~ 10 Solar mass P=47.7 msL ~ 3.3 10L ~ 3.3 103737 erg/s Lsd=8.3 10 erg/s Lsd=8.3 1035 35 erg/serg/sT ~ 2.3 10T ~ 2.3 1044 K KStellar outflow Binary system Stellar outflow Binary system Polar wind Distance d =1.5 kpcPolar wind Distance d =1.5 kpcVp ~ 2000 km/s e=0.87 Vp ~ 2000 km/s e=0.87 Mp ~2 10Mp ~2 10-8-8 Solar mass/yr Periastron separation Solar mass/yr Periastron separation Equatorial outflow Dmin=9.6 10Equatorial outflow Dmin=9.6 101212 cm cm Vd ~ 150-300 km/sVd ~ 150-300 km/sMd ~ 5 10Md ~ 5 10-8-8 Solar mass/yr Solar mass/yr

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View on the systemView on the system

Page 5: Colliding winds in pulsar binaries

Parameterization Parameterization

Separation distance D=1.Separation distance D=1.

At Lorentz factor At Lorentz factor γγ >> 1 >> 1

All the flow depends on the only All the flow depends on the only parameterparameter

For PSR 1259-63 10For PSR 1259-63 10-2-2 < <ηη<1<1

0vMc

Erot

Page 6: Colliding winds in pulsar binaries

The scheme of interaction of the The scheme of interaction of the winds winds

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Basic problems at the numerical Basic problems at the numerical modelingmodeling

The position of the shocks and The position of the shocks and discontinues is unknown discontinues is unknown a priorya priory

Large difference in equations and Large difference in equations and properties of the relativistic and properties of the relativistic and nonrelativistic flowsnonrelativistic flows

Different Courant numbers in Different Courant numbers in relativistic and nonrelativistic flows. relativistic and nonrelativistic flows.

Instability of the contact discontinuity. Instability of the contact discontinuity.

Page 8: Colliding winds in pulsar binaries

Two zone solutionTwo zone solution

Nearest zone includes all the regions Nearest zone includes all the regions of subsonic flows- Method of of subsonic flows- Method of relaxationrelaxation

Far zone – supersonic flow. Cauchy Far zone – supersonic flow. Cauchy problem.problem.

Page 9: Colliding winds in pulsar binaries

Method of solution in the Method of solution in the nearest zonenearest zone

The equations are solved The equations are solved

only in the post shock regionsonly in the post shock regions Adaptive mesh is used. Adaptive mesh is used.

Beams are fixed, position ofBeams are fixed, position of

fronts varyfronts vary

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Equations for the relativistic windEquations for the relativistic wind

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Equations for the nonrelativistic Equations for the nonrelativistic windswinds

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Dynamics of the discontinuitiesDynamics of the discontinuities

To define evolutionTo define evolution

of the shocks andof the shocks and

Contact discontinuity Contact discontinuity

The Reimann problemThe Reimann problem

About discontinuity decayAbout discontinuity decay

Has been solvedHas been solved

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The method of solution In the far The method of solution In the far zone zone

Page 14: Colliding winds in pulsar binaries

ResultsResults

1.1. The termination shock front of the The termination shock front of the pulsar wind is not always closed. pulsar wind is not always closed.

For For ηη > 1.25 10 > 1.25 10-2-2 the shock front is the shock front is opened. opened.

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The shock front for plane parallel The shock front for plane parallel stellar windstellar wind

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High High ηη

Page 17: Colliding winds in pulsar binaries
Page 18: Colliding winds in pulsar binaries

Dependence of the fronts on Dependence of the fronts on ηη

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Dependance of the asymptotic Dependance of the asymptotic opening angle of the fronts on opening angle of the fronts on ηη

Page 20: Colliding winds in pulsar binaries

Energy flow in the relativistic post Energy flow in the relativistic post shock windshock wind

Total energy along Total energy along flow line is flow line is conservedconserved

windicrelativisthot for - 4T w

windcoldfor - 1w

equation) (Bernoully

constw

Page 21: Colliding winds in pulsar binaries

Adiabatic coolingAdiabatic cooling

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Formation of relativistic jet-like Formation of relativistic jet-like flows in the post shock windflows in the post shock wind

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The role of the magnetic field The role of the magnetic field

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For comparison - interaction of the For comparison - interaction of the magnetized isotropic pulsar wind magnetized isotropic pulsar wind with isotropic interstellar medium with isotropic interstellar medium

Page 25: Colliding winds in pulsar binaries

Basic conclusionsBasic conclusions relativistic wind in the post shock region relativistic wind in the post shock region

becomes relativistic even at the distance becomes relativistic even at the distance comparable with the separation distance.comparable with the separation distance.

At higher distances the Lorentz factor can At higher distances the Lorentz factor can achieve initial valuesachieve initial values

Even moderate relativistic motion of the Even moderate relativistic motion of the post shock plasma can have strong impact post shock plasma can have strong impact on the light curve of radiation (synchrotron on the light curve of radiation (synchrotron and IC)and IC)

Adiabatic cooling can result into Adiabatic cooling can result into suppression of the synchrotron radiation suppression of the synchrotron radiation and excess of IC radiation. and excess of IC radiation.