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HIGH-QUALITY FAST QPOs FROM MAGNETARS: AN ELECTRIC CIRCUIT MODEL A.Stepanov (Pulkovo Observatory, St.Petersburg) V.Zaitsev (Institute of Applied Physics,

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Presentation on theme: "HIGH-QUALITY FAST QPOs FROM MAGNETARS: AN ELECTRIC CIRCUIT MODEL A.Stepanov (Pulkovo Observatory, St.Petersburg) V.Zaitsev (Institute of Applied Physics,"— Presentation transcript:

1 HIGH-QUALITY FAST QPOs FROM MAGNETARS: AN ELECTRIC CIRCUIT MODEL A.Stepanov (Pulkovo Observatory, St.Petersburg) V.Zaitsev (Institute of Applied Physics, N.Novgorod) E.Valtaoja (Tuorla Observatory, Turku) Expanding the Universe Tartu April 2011

2 Soft Gamma-ray Repeater - neutron star (D ~ 10 km, M ≤ 1.5M Sun ) with magnetic field B ~ G

3 Energy release in impulse phase (duration ≤ 1 s): up to 2×10 46 ergs High-quality, Q ≥ 10 5, high-frequency ( Hz) pulsations in ‘ringing tails’ of flares (~ ergs). Background: ~ 0.1 Hz QPOs due to star rotation (dipole emission).

4 Ringing tail (Strohmayer & Watts ApJ 2006)

5 Starquakes: electric current generation driven by crust cracking ( Ruderman 1991) Neutron star (D ~ 10 km) with magnetic field B ~ G

6 Flare scenario Fireball (≥1 MeV electron-positron plasma + gamma-rays) – the source of main pulse of flare. Trapped fireball (≤ 1 MeV e/p plasma + γ) – a source of ‘ringing tail’ δB → SGR flux modulation

7 Existing models of magnetar fast QPOs Strohmayer & Watts (2006), Sotani et al (2008): Torsion Alfven oscillations of relativistic star with global dipole magnetic field. Levin (2006, 2007): Torsion oscillations of crust. Interaction between normal modes of magnetar’s crust and MHD-modes in its fluid core. Israel et al (2005): Coupling of toroidal seismic modes with Alfven waves propagating along magnetospheric field lines. Vietri et al (2007): Estimation of magnetic field from Cavallo-Fabian-Rees luminosity variability limit of ‘ringing tail’, B ~ 8×10 14 G. Timokhin et al (2008) Variations of magnetospheric currents due to crust torsion oscillations. Glampedakis et al (2006): Interaction of global magneto-elastic vibrations of the star and fluid core. Bo Ma et al (2008): Standing slow magneto-sonic waves of flux tubes in magnetar coronae. These models do not explain: - Excitation of oscillations in the ‘ringing tail’ and before impulse phase - Very high Q-factor of fast QPOs, Q ≥ 10 4 (Levin 2006: Q ~30 ) - Broad discrete spectrum of fast QPO frequencies ( Hz).

8 The main task: To estimate the physical parameters of trapped fireball plasma using oscillations of ‘ringing tail’ 1-D physics because B is very high (no loss-cone, for example)

9 Helioseismology Inside the Sun – check of “standard” model of the Sun Asteroseismology Coronal seismology stellar evolution model waves & oscillations in corona (flaring loops, coronal heating)

10 Solar-stellar analogy & Coronal seismology Wave and oscillatory phenomena in solar and stellar coronae A new and rapidly developing branch of astrophysics. Two main approaches: Coronal magnetic loops and flux tubes are resonators and wave guides for MHD oscillations and waves, Coronal loops as an equivalent electric (RLC) circuit.

11 Flare loop as an equivalent electric circuit Severny (1965): vertical currents I ~ 3  A near sunspot Electric circuit approach : Alfven & Carlquist (1967): electric circuit analog of a flare Stenflo (1969), Spicer (1977), Ionson (1982), Zaitsev & Stepanov (1992), Melrose (1995), The last review: Zaitsev & Stepanov ‘Coronal magnetic loops’ (Phys. Uspekhi 2008) Alfven & Carlquist (Sol.Phys.1967)

12 The Sun: Loop formed by photosphere convection Zaitsev, Stepanov, Urpo (A&A 2001) Loop footpoints – in nodes of supergranula cells, Δ ≈ km Convection velocity V r ≈ km/s Magnetar corona Beloborodov & Thompson (ApJ 2007)

13 Our approach: Coronal seismology (RLC-model) Based on Beloborodov & Thompson model (2007) for magnetar corona and on the model of coronal loop as an equivalent electric circuit (Zaitsev & Stepanov 2008). Current in a loop is closed in metallic crust Electric current appears due to crust cracking (Ruderman 1991) Trapped fireball consists of ~ current- currying loops (RLC-circuits). Eigen-frequencies and Q-factors are

14 RLC-circuit model SGR flare on Dec. 27, Total energy 5×10 39 J Circuit energy E = LI 2 /2, from loop geometry: For loop length l = 3×10 4 m, loop radius r = 3×10 3 m we obtain circuit inductance L ≈ 5×10 4 m ≈ 5×10 -3 H. From the energy of ‘ringing tail’ E = 0.5LI 2 = J we derive loop electric current I ≈ 3×10 19 A. Using current magnitude we estimate the magnetic field minimum value: B φ ≈ I/cr ≈ G < B q = m 2 c 3 /ħe = 4,4×10 13 G. Power released in ‘ringing tail’ W = R I 2 = W → R = 2.3×10 -6 Ohm For anomalous (turbulent) conductivity σ eff = e 2 n/mν eff we get ν eff = (W p /nT)ω p ≈ 0.1 ω p

15 The origin of turbulent resistance ~ η I = 2.3×10 -6 Ohm, R eff ~ ν eff ~ W ~ I 2 Number density of e/p pair in trapped fireball: I = 2necS = 3 ×10 19 A → n = 2×10 16 см -3 → ω p = 8×10 12 s -1 (f p ≈ 1 THz ) ν eff = (W p /nk B T)ω p ≈ ω p Possible origin of small-scale turbulence: Beam instability in electron-positron plasma (Eichler et al 2002; Lyutikov 2002)

16 Self-excitation of current oscillations Equation for oscillations of electric current in a loop: Because R eff ~ ν eff ~ W~ I 2, R ~ αI 2 Current oscillations are excited if I < I max e.g. on the rising stage of a flare and on flare ‘tail’. δI → δB → SGR flux modulation

17 ν From minimal ( ν 1 = 18 Hz) and maximal ( ν 2 = 2384 Hz) frequencies of ‘ringing tail’ we can estimate capacities of loops in trapped fireball: C 1 ≈1,5×10 -2 F, C 2 ≈ 8×10 -7 F. From the other side, the loop capacity is (Zaitsev & Stepanov 2008): C ≈ ε A S/l, for S = πr 2 ≈ 3×10 11 cm 2, ε A = c 2 /V A 2 ≈ 1 и l = 3×10 6 cm, C ≈ F. We can get various loop capacities C = F for the loops with different lengths l and cross-sectional areas S.

18 Magnetar coronal loop – a system with compact parameters? Oscillations of electric current should be in-phase in all points of a loop. On the other hand, variations of the current propagate along the loop with the Alfven velocity. Therefore, for the condition of phase coincidence, the Alfven time should be substantially smaller than the period of oscillations. QPO-frequency ν = ν RLC ≈ Hz < ν Alfven = c/ l ≥ 10 4 Hz Because V A = c (!) in magnetar coronae = c for ρ → 0 or B → ∞

19 Why we choose the SGR flare on Dec. 27, 2004 ? Flare start: 21:30:26,35 UT

20 Polar Geophysical Institute Tumanny Ionospheric Station

21 Flare start: 21:30:26,35 UT

22 Corona of SGR : Diagnostics From loop geometry → L = 5×10 -3 Henry From ‘ringing tail’ energy LI 2 /2 → I = 3 ×10 19 A. From current value I ≈ B φ cr → B min ≈ G < B q = 4.4×10 13 G From energy release rate W=RI 2 → R = 2.3×10 -6 Ohm From current and loop cross-section area → n = 2.5×10 16 cm -3 For R = 2.3×10 -6 Ohm collisional frequency ν eff = ( W p /nT)ω p = 6×10 -2 ω p For = 625 Hz → capacitance С = 1.3×10 -5 F Circuit quality Q = (R√C/L) -1 ≈ 8×10 5 From observations: Q = πν Δt ≥ 4×10 5 for train duration Δt ≥ 200 с. Various high-quality QPO’s detected in giant flare of SGR ( ν = 18, 30, 92, 150, 625, 1480 Hz) are due to persistence of loops with various geometry, plasma density, and magnetic field in a fireball.

23 Summary Phenomenological approach: “ringing tile” - a trapped fireball - as a set of current-carrying coronal loops is quite effective diagnostic tool for magnetar corona. I = 3 ×10 19 A, B min ≈ G < B q = 4.4×10 13 G, n = 2.5×10 16 cm -3 Because B < B q = 4.4×10 13 G, the physical processes in ‘trapped fireball’ can be studied in non-quantum plasma approach. Estimations from energetic reasons give us real physical parameters of magnetars. For impulse phase (fireball) I = A, B ≈ 4 ×10 14 G.

24 European Week of Astronomy and Space Science (JENAM-2011) July Saint-Petersburg Important Dates: - May : Deadline of Abstracts submission/EAS Grant Applications - May : Results of Grant applications/Final programme release - June : End of early registration - June : End of late registration - July : EWASS-2011

25 Symposia S1: Magnetic Universe S2: Planets of the Solar System and Beyond S3: The Sun: New Challenges S4: Solar System Measurements of the Next Decade S5: Physics of Stars S6: Combined Radio/X-rays Approaches to Relativistic Astrophysics S7: Far-Infrared Spectroscopy comes of age: the Herschel view S8: Status and prospects in high-energy & particle astrophysics across the electromagnetic spectrum S9: Galaxy Evolution: the key for Galaxy Formation theories Special Sessions SPS1: Close Binaries with Compact Components SPS2: Massive Stars Formation SPS3: Science with the Virtual Observatory SPS4: What powers AXPs and SGRs? SPS5: Minor merging as a driver of galaxy evolution, SPS6: Space Projects SPS7: The Missing Baryons and the Warm-Hot Intergalactic Medium: Current State and Future Prospects, SPS8: Astronomy Education and Public Outreach in Europe SPS9: Amateur and professional astronomers in Europe SPS10: European Astronomy: Moving Forward


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