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Astrophysical plasmas Sun: coronal seismology Exoplanet atmospheres . Sergio Elaskar - Matías Schneiter – Walkiria Schulz Mariana Cécere - Andrés Cimino Carlos Francile - Carlos Fernández Sebastián Maglione Nuevos integrantes : Carolina Villarreal – Ernesto Zurbriggen.

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Presentation Transcript
slide1

Astrophysical plasmas

Sun: coronal seismology

Exoplanet atmospheres

Sergio Elaskar- MatíasSchneiter – Walkiria Schulz

Mariana Cécere - Andrés Cimino

Carlos Francile - Carlos Fernández

SebastiánMaglione

Nuevosintegrantes:

Carolina Villarreal – Ernesto Zurbriggen

Andrea Costa

plasma parameters slow large scale variations
Plasma parametersSlowlarge-scalevariations

Electrostatic vs Kinetic

Collectivebehaviour

CompressibleElastic

Magnetized plasma

slide3

Coronal phenomenology

  • Low corona magneticallyhighlystructuredsystem – X-Ray and EUV emissionishighlystructured
  • Tracerof magneticfield
  • Theunderlyingchromosphereverydynamic: smallscalestructures and turbulentmotionprevails
slide5

Coronal phenomenology- magnetized plasma

  • Large Reynolds number – field lines and plasma frozen
  • Corona: gas pressure << magnetic pressure
  • The magnetic field governs the dynamic
  • Chromosphere: magnetic pressure << gas pressure
  • The fluid governs the dynamic
slide6

Importance of shock wave contributionfortheseismology

  • Large Reynolds  frozen plasma – magnetic field
  • Gas pressure << magnetic pressure
  • Dynamic governed by the magnetic field
  • Sound speed << Alfvén speed
  • Energy: compressibility medium– elasticity medium
  • Inhomogeneity of the medium couples elastic perturbations with compressible ones. In the average transfer of energy to compressible modes
  • Favors the appearence of shock waves: compressive modes with Mach>1
slide7

Simulations fundamental and global modes

Cécere, Costa, Reula A&A, 2011Slendertube - Logaritmic – coronal conditionsDuetochromospheric line-tied and inhomogeneities and nonlinearities

puremodesdifficulttosustain

Jumpconditionsacrosstheradiusamplifiesthespectrum of modes

Trapped –LeakyEvolutionto a quasi-static 2nd slowharmonicstateoccursviatheonsetof anexternalcompressionalAlfvénwave or a weakshock wave M<1.3thattriggersthesausagemode and couplestheslowmode

slide8

Costa, Elaskar, Fernández, Martínez, MNRAS 2009Fernández, Costa, Elaskar, Schulz, 2009

Schulz, Costa, Elaskar, Cid, MNRAS 2010

Maglione, Schneiter, Costa, Elaskar, A&A 2011

Costa, Pl.Phis.Contr.Fusion, 2011

Interpretations:

Rain of blobs of dense and cool plasma after a CME falling gravitationally back

Flux tubes linking an above current sheet retract downwards under the force of the

magnetic tension

Top of colapsing loops with void tails in the wakes where reconnection occurs

Verwichte, Nakariakov, Cooper A&A, 2005 Observational analysis

Kink wave trains guided by ray tadpole structures. However speeds ~ vs not ~vA

slide13

Moretonwaves

Francile,Costa, Schneiter, Elaskar, 2011

Chromospheric shock wavesorfastmagnetoacoustic wave

Triggeredby a notstablished coronal phenomenon

slide14

Exoplanetatmospheres: we derive theL_Alphaabsortionfordifferentwindconditions

Schneiter,Velázquez,Raga, 2007-Villareal,Schneiter,Costa, 2011-Schneiter, Costa, Velázquez, 2011

HD209458b

HD17156b