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Large amplitude transverse oscillations in a multi-stranded EUV prominence centre for fusion, space and astrophysics J. M. Harris C. Foullon, V. M. Nakariakov,

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Presentation on theme: "Large amplitude transverse oscillations in a multi-stranded EUV prominence centre for fusion, space and astrophysics J. M. Harris C. Foullon, V. M. Nakariakov,"— Presentation transcript:

1 Large amplitude transverse oscillations in a multi-stranded EUV prominence centre for fusion, space and astrophysics J. M. Harris C. Foullon, V. M. Nakariakov, E. Verwichte

2 Prominence Oscillations ☼Solar prominences float in the corona, held in place by the magnetic field ☼They are cooler and denser than the coronal plasma, therefore appearing: bright against a dark background in 304 Å (70,000 K), but dark against the bright corona in 195 Å (1.5 million K). ☼Oscillations traditionally observed in Hα lines as ‘winking filaments’ e.g. Dyson et al (1930), Brusek (1951), Ramsey & Smith (1966). The line of sight velocity can be measured using the Doppler shift. 195 Å EUV images of a prominence on the NE limb (SOHO/EIT)‏ 304 Å

3 Prominence Oscillations ☼Now also observed by EUV imagers e.g. Foullon et al (2004, 2010), Isobe & Tripathi (2006), Pinter et al (2008). This enables long periods and the field of view velocity to be measured. ☼Small amplitude oscillations: velocity ≈ 2-3 km/s. ☼Large amplitude oscillations: velocity > 20km/s. can be triggered by nearby flares or EIT waves, observational analyses are scarce, see Tripathi et al (2009) for a review. ☼Analysis of these oscillations enables us to: measure plasma parameters (e.g. magnetic field) via coronal seismology, understand more about solar prominences (e.g. link to prominence eruptions), verify oscillation and damping theories.

4 Prominence Oscillation on 30 th July 2005 ☼Observed using SOHO/EIT: 195 Å, 12 min cadence, 304 Å, 6 hour cadence. ☼Two successive trains of transverse oscillations, ☼triggered by EIT waves from two flares in the same remote active region: X1.3 class flare at 06:17 C8.9 class flare at 16:39

5 EIT Waves 16: :3516: :4517: :5517: :07 EIT Wave 2 ☼1 st EIT wave seen over only 1 frame using running difference images (Type II radio burst, 1801 km/s) ☼2 nd EIT wave seen over 4 fast frames (no Type II reported) ☼Intensity depletion is larger following the 1 st EIT wave 16: :35 06: :02 17: :35 EIT Wave 1 EIT Wave 2

6 Evolution of the Apparent Height Foullon & Verwichte (2006)‏ Image using ratio of 304/195 Å with region of interest indicated = Carrington longitude = Carrington longitude when over the limb = apparent height = actual height = solar radius rotation position over the limb when position at

7 Evolution of Apparent Height 5 days flare 1flare 2 Region of interest moves with the rotation of the prominence

8 Time - Distance Plots: slit 1

9 Time - Distance Plots: slit 4

10 Analysis of Time Series: slit 1 P = 122 ± 23 min Τ = 131 ± 94 min v = 12 ± 5 km/s P = 101 ± 1 min Τ = 218 ± 47 min v = 32 ± 10 km/s

11 Analysis of Time Series: slit 4 P = 97 ± 21 min Τ = 274 ± 497 min v = 5 ± 4 km/s P = 94 ± 2 min Τ = 119 ± 19 min v = 30 ± 4 km/s P = 108 ± 2 min Τ = 277 ± 80 min v = 17 ± 3 km/s P = 111 ± 4 min Τ = 362 ± 212 min v = 11 ± 3 km/s

12 Results: Amplitude & Period

13 Results: Damping Times consistent with damping via resonant absorption Coronal loop oscillation data: Nakariakov et al (1999)‏Aschwanden et al (2002)‏ Wang & Solanki (2004)‏Verwichte et al. (2004)‏ Van Doorsselaere et al. (2007)‏Hori et al. (2007)‏ Van Doorsselaere et al (2009)‏Verwichte et al. (2009)‏ Verwichte et al. (2010)‏ Prominence oscillation data: Harris et al (2010)‏

14 Conclusions ☼Large amplitude transverse (horizontal) prominence oscillation. ☼Velocity amplitudes: Generally increasing with height, up to 32km/s following the X1.3 class flare and up to 12km/s after the C8.9 class flare, as expected due to the difference in flare energy. ☼Periods of around 100 minutes (±10 minutes): Generally increasing with height and varying for different strands, indicating that the prominence doesn’t oscillate as a solid body but according to its filamentary structure. Around 10% shorter during the 1 st oscillatory train than the 2 nd (c.f. 15x flare energy, 5x amplitude), suggesting the period is largely dependent on the properties of the prominence rather than the triggering mechanism, as expected for an MHD mode. ☼Damping times: 2 to 3 periods for most strands. when combined with data from loop oscillations, this is consistent with damping via resonant absorption. Other strands exhibit much longer decay times, but the errors in these cases are very large. Harris et al. 2010, in preparation


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