Formation and Evolution. of the SS 433 Jets. Herman L. Marshall (MIT Kavli Institute) Sebastian Heinz (University Wisconsin)
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1 Formation and Evolution Herman L. Marshall (MIT Kavli Institute) Sebastian Heinz (University Wisconsin) Norbert S. Schulz (MIT Kavli Institute) of the SS 433 Jets
2 SS 433 Background Periodically Doppler shifting Hα HeI and Hβ Model: oppositely directed jets at 0.26 c Precession period: 162 days Orbital period: days Radio: verifies model and sets orientation Only jet known to contain baryons Red jet cm Blue jet Blundell & Bowler 2005 Margon et al Texas Symposium Dec 12, /16 Herman L. Marshall SS 433
3 Jet Model Jet is clumped > cm, radio-dominated > cm Clumps move ~ ballistically over x1000 in r Atomic H, He recombination emission at cm Texas Symposium Dec 12, /16 Herman L. Marshall SS 433
4 Two HETGS Spectra Hydrogenic lines Helium-like lines Lines from many ions at 10 7 K < T < 10 8 K Red jet is weak in 1999 but strong in 2001 Lines are broad due to jet expansion Texas Symposium Dec 12, /16 Herman L. Marshall SS 433
5 Jet Model Jet is clumped > cm, radio-dominated > cm Clumps move ~ ballistically over x1000 in r Atomic H, He recombination emission at cm Jet cools from kt > 15 kev Jet contains common metals (from accretion) Jet has constant speed, spreading as it cools Texas Symposium Dec 12, /16 Herman L. Marshall SS 433
6 Trailed Spectra Aug. 8 Made by Doppler Shifting to rest frame Used many lines: Mg XII, Si XIV, Fe XV, etc. Aug. 12 Aug. 16 Aug ,000 Velocity (km/s) 0 Time (ks) -30, ks Texas Symposium Dec 12, /16 Herman L. Marshall SS 433
7 Blue Jet X-ray Spectrum Corrected spectra for time-varying Doppler shifts Combine spectra Ignore red-shifted lines Fit in isis to 4T model Ni: x10 overabundant Texas Symposium Dec 12, /16 Herman L. Marshall SS 433
8 Jet Cooling Model Texas Symposium Dec 12, /16 Herman L. Marshall SS 433
9 Eclipse Spectrum Soft flux doesn t eclipse Texas Symposium Dec 12, /16 Herman L. Marshall SS 433
10 Results from X-ray Data X-ray region cooling time < 5000 s Radiative cooling of thermal plasma < 200 s X-ray emission < 4 x cm (0.05 mas) from shocks that redirect jet and heat gas spectral fit: rmin = 5 x cm, Ljet = 3 x erg/s (Lx ~ ) Jet redirected on 0.2d time scale by 2 Blue, red jets different Perturbed by local effects where jet is directed --> supports a redirection model Eclipsed region spectrum: hard, weak Fe XXV line Most of jet is not eclipsed; > 2 x cm from disk Supports redirection model (or internal shocks) Ni overabundance, enhanced metals --> gas from companion coated with SN products or by jet? Texas Symposium Dec 12, /16 Herman L. Marshall SS 433
11 Jet Model Jet is clumped > cm, radio-dominated > cm Clumps move ~ ballistically over x1000 in r Atomic H, He recombination emission at cm Jet cools from kt > 15 kev Jet contains common metals (from accretion) Jet has constant speed, spreading as it cools Jet is continuous at cm Adiabatic and radiative cooling are comparable Direction is separately set for opposite jets Texas Symposium Dec 12, /16 Herman L. Marshall SS 433
12 Two Shock Geometries Jet starts out baryonic, v~c Model 1: perpendicular shock starts at 20 to disk axis plows through thick accr. disk X-rays visible only on exit Shock zone Accretion Disk Model 2: oblique shock starts out on-axis encounter wind from outer disk can bend jet 20 jet precession due to outer disk Wind Wind Shock zone Texas Symposium Dec 12, /16 Herman L. Marshall SS 433
13 Perpendicular Shock Solutions using Synge EOS Vshock < 0.08c in observed frame kte > 185 kev after shock Texas Symposium Dec 12, /16 Herman L. Marshall SS 433
14 Oblique Shock Model Solve eqns for v2 = 0.26c, θ=20 Eg. Γ1 > 2-3, shock angle = 6-7 Shock is stationary in observed frame Wind Wind Shock zone Texas Symposium Dec 12, /16 Herman L. Marshall SS 433
15 10 12 cm Texas Symposium Dec 12, /16 Herman L. Marshall SS 433
16 Jet Model Jet is clumped > cm, radio-dominated > cm Clumps move ~ ballistically over x1000 in r Atomic H, He recombination emission at cm Jet cools from kt > 15 kev Jet contains common metals (from accretion) Jet has constant speed, spreading as it cools Jet is continuous at cm Adiabatic and radiative cooling are comparable Direction is separately set for opposite jets Shocks likely heat accreted gas to kt > 30 kev Shock model 1: jet intercepts disk funnel Shock model 2: jet bent by wind from outer disk Texas Symposium Dec 12, /16 Herman L. Marshall SS 433
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