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Solar Physics & upper-Atmosphere Research Group Robert Erdélyi 1 st Helas WS, Nice 25 – 27 September 2006 University of.

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Presentation on theme: "Solar Physics & upper-Atmosphere Research Group Robert Erdélyi 1 st Helas WS, Nice 25 – 27 September 2006 University of."— Presentation transcript:

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2 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield

3 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield www.iaus247.org LOC contact: Cesar Mendoza-Briceno (Venezuela) SOC contact: Robertus Erdélyi (UK)

4 Solar Physics & upper-Atmosphere Research Group 1st Helas WS, Nice 25 – 27 September 2006 University of Sheffield Leakage of photospheric motions into the magnetic solar atmosphere… R. Erdélyi B. De Pontieu, C. Malins, B. Pintér, Y. Taroyan… robertus@sheffield.ac.uk SPARG, Department of Applied Mathematics, The University of Sheffield (UK) http://www.shef.ac.uk/~robertus

5 Solar Physics & upper-Atmosphere Research Group 1st Helas WS, Nice 25 – 27 September 2006 University of Sheffield aka New prospects of magneto- seismology R. Erdélyi B. De Pontieu, C. Malins, B. Pintér, Y. Taroyan… Robertus@sheffield.ac.uk SPARG, Department of Applied Mathematics, The University of Sheffield (UK) http://www.shef.ac.uk/~robertus

6 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield Visible 5000 K Magnetic field 5000 K UV 1600 Å 8000 K Hα 15,000 K He EUV 50,000 K Fe VIII/IX EUV 1 MK Magnetic coupling in the atmosphere

7 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield Introduction Reminder of a basic fact: Photosphere – chromosphere – TR (– corona are) magnetically coupled. Manifestation of coupling has (at least) two exciting aspects: Influence of magnetic atmosphere, e.g. magnetic carpet on oscillations. Role of p modes in the dynamics of the solar atmosphere! (Less explored.)

8 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield Solar interior Global oscillations p, f, (g) modes One waveguide, many modes Solar atmosphere More local oscillations Sunspot oscillations, prominence oscillations, coronal loop oscillations, plume oscillations One mode, many waveguides Oscillations ubiquitous in Sun Objects: atmospheric oscillations

9 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield Coupling scales and elements ¤ Magnetic fields ¤ Flow fields Manifestations of presence in solar atmosphere: Organised flows (meridional; differential rotation, etc.) Random flows (granulation, convection, etc.) Coherent global fields (e.g. canopy) Random fields (magnetic carpet)

10 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield An example: line-widths (GONG++) Surface gravity (f) modes Acoustic (p) modes Dziembowski and Goode, ApJ 2005

11 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield Simple-minded solar model corona chromospheric transitional layer (L) photosphere x z y g solar interior B(z) canopy (h)

12 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield Eigenmodes (L  0, B  0)

13 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield ¤ Three-layer model ¤ Polytropic interior ¤ Magnetic transitional layer  resonances  damping ¤ Isothermal magnetic upper atmosphere ¤ Presence of Alfvén/slow continuum ¤Tirry et al. 1998, Pintér et al. 1999 Eigenmodes (L  0, B  0)

14 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield ¤ Three-layer model ¤ Polytropic interior ¤ Magnetic transitional layer  resonances  damping ¤ Isothermal magnetic upper atmosphere ¤ Presence of Alfvén/slow continuum ¤ Erdélyi and Pintér 2005 ¤ Pintér et al. 2006 l = 100 L = 2 Mm Δν (μHz) B c (G) p3p3 p8p8 p4p4 f p1p1 p2p2 l = 100 L = 2 Mm Im ν (nHz) Eigenmodes (L  0, B  0)

15 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield ¤ Erdélyi, Pintér & Goossens 2005 Eigenmodes (L  0, B  0) Local magneto-seismology

16 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield ¤ Pintér, Erdélyi & Goossens 2006 Eigenmodes (L  0, B  0) Local magneto-seismology

17 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield Model improvement Dowdy et al. (1986) Solar Phys., 105, 35

18 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield Possible challenges… ¤ De Pontieu, Tarbell & Erdélyi 2003

19 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield The Klein-Gordon waves Leakage of photospheric motion into LA Sound, slow, Alfvén waves  = 5/3  1 Non-adiabatic plasma Inclination of magnetic wave guides Isothermal atmosphere Photosphere: ν ac = 4.8 mHz  P = 210 s (acoustic cut-off frequency) Corona: ν ac = 0.18 mHz  P = 91.7 min

20 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield The Klein-Gordon waves Stratified atmosphere (VALIIIC, g=const) driver p-modes 40° 50° 0°

21 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield Dynamics: Solar spicules

22 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield Lower atmospheric moss oscillations Bright reticulated layer of EUV emission consisting of 1 - 3 Mm bright elements with dark “holes” (jets): 1 MK upper transition region at footpoint of hot 3-5 MK loops above unipolar plage (Berger et al., Fletcher & De Pontieu, De Pontieu et al., 1999, Martens et al, 2000)

23 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield Not steady waves but wave trains of finite duration. Oscillations usually last for 32±7 mins or 3 to 7 cycles (just like p modes): rarely continue for more than 40 min. Wavelet analysis using Morlet wavelet (k=6) Lower atmospheric moss oscillation Oscillations usually suddenly start and stop.

24 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield p-mode driven spicules (and coronal oscillations) Vertical flux tube Inclined flux tube (50°) Chromospheric dynamics in inclined flux tubes are dominated by five minute periods because of significantly increased leakage of photospheric p modes into the atmosphere

25 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield P-mode driven spicules (and coronal oscillations)  = 50° The match between predicted spicule occurrence and observed spicule occurrence is good, especially considering the limitations of the numerical model

26 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield P-mode driven spicules: 2-D

27 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield Numerous examples of waves and oscillations by SOHO and TRACE in the solar atmosphere structures MHD theory seems to be a satisfactory description Atmospheric seismology provides us information about: magnetic field, transport coefficients, fine structures, etc. Coupling of photospheric motions (p modes, granules, etc.) to lower atmosphere (and above) Stratification has significant effect Lower atmosphere has back-reaction on global oscillations Summary

28 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield The end

29 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield Editors: Robertus Erdélyi ( robertus@sheffield.ac.uk ) and John Leibacher ( john.leibacher@gmail.com ) MHD Waves and Oscillations in Solar Magnetic Structures Solar Physics “Topical Issue” Deadline:12 January 2007 -Theory of MHD modes of magnetic structures - Magnetic helioseismology and waves in sunspots - MHD waves in the lower atmosphere - Prominence oscillations - Waves in the corona, MHD coronal seismology

30 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield LOC contact: Cesar Mendoza-Briceno (Venezuela) SOC contact: Robertus Erdélyi (UK) www.iaus247.org

31 Solar Physics & upper-Atmosphere Research Group Robert Erdélyi http://www.shef.ac.uk/~robertus 1 st Helas WS, Nice 25 – 27 September 2006 University of Sheffield

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