1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

www.iaus247.org

LOC contact: Cesar Mendoza-Briceno (Venezuela)

SOC contact: Robertus Erdélyi (UK)

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Leakage of photospheric motions Leakage of photospheric motions into the magnetic solar into the magnetic solar

atmosphere…atmosphere…R. Erdélyi

B. De Pontieu, C. Malins, B. Pintér, Y. Taroyan…

robertus@sheffield.ac.ukSPARG, Department of Applied Mathematics,

The University of Sheffield (UK)

http://www.shef.ac.uk/~robertus

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

IntroductionIntroduction

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.)

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

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 Objects: atmospheric oscillationsoscillations

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

Coupling scales and elementsCoupling 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)

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

Simple-minded solar modelSimple-minded solar model corona

chro

mos

ph

eric

tr

ansi

tion

al

laye

r (L

)

photospherexzy g solar interior

B(z)

canopy (h)

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

Eigenmodes (L Eigenmodes (L 0, B 0, B 0) 0)

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

       

¤ 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 Eigenmodes (L 0, B 0, B 0) 0)

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

¤ 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 = 100L = 2 Mm

Δν

(μ

Hz)

Bc (G)

p3

p8

p4

f

Bc (G)

p1 p2

l = 100L = 2 Mm

Im ν

(nH

z)Eigenmodes (L Eigenmodes (L 0, B 0, B 0) 0)

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

¤ Pintér, Erdélyi & Goossens 2006

Eigenmodes (L Eigenmodes (L 0, B 0, B 0) 0)

Local magneto-seismology

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

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.

Wav

elet

ana

lysi

s us

ing

Mor

let w

avel

et (

k=6)

Lower atmospheric Lower atmospheric moss oscillationmoss oscillation

Oscillations usually suddenly start and stop.

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

pp-mode driven -mode driven spiculesspicules (and coronal (and coronal oscillations)oscillations)

Ver

tical

flu

x tu

be

Incl

ined

flu

x tu

be (

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

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

P-mode driven spicules: 2-DP-mode driven spicules: 2-D

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

       

• 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

SummarySummary

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

       

The end

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

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

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus

LOC contact: Cesar Mendoza-Briceno (Venezuela)

SOC contact: Robertus Erdélyi (UK)

www.iaus247.org

1st Helas WS, Nice 25 – 27 September 2006

University of Sheffield

Solar Physics & upper-Atmosphere Research Group

Robert Erdélyihttp://www.shef.ac.uk/~robertus