colliding winds in pulsar binaries
DESCRIPTION
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 PresentationTRANSCRIPT
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)
Candidates Candidates
PSR 1259-63/2883PSR 1259-63/2883 LS 5039LS 5039 LSI +61303LSI +61303 Cygnus X-1Cygnus X-1
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
View on the systemView on the system
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
The scheme of interaction of the The scheme of interaction of the winds winds
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.
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.
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
Equations for the relativistic windEquations for the relativistic wind
Equations for the nonrelativistic Equations for the nonrelativistic windswinds
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
The method of solution In the far The method of solution In the far zone zone
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.
The shock front for plane parallel The shock front for plane parallel stellar windstellar wind
High High ηη
Dependence of the fronts on Dependence of the fronts on ηη
Dependance of the asymptotic Dependance of the asymptotic opening angle of the fronts on opening angle of the fronts on ηη
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
Adiabatic coolingAdiabatic cooling
Formation of relativistic jet-like Formation of relativistic jet-like flows in the post shock windflows in the post shock wind
The role of the magnetic field The role of the magnetic field
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
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.