1 Krzysztof Murawski

2 Obserwacje sejsmiczne - Ziemia

3 Schemat budowy Słońca

4 Solar corona: Main physical facts about the corona: almost fully ionised plasma, temperature is over 1 MK, magnetically-dominated, plasma-  (ratio of gas and magnetic pressures) is low (0.001-0.01), The plasma is “cold”! the origin of the solar wind  space weather, a natural plasma laboratory  controlled fusion. The uppermost part of the solar atmosphere

5 Structures in the solar corona:

6 SOHO – SOlar and Heliospheric Observatory Launched in 1995 by ESA and NASA

7 TRACE – Transition Region And Coronal Explorer NASA, 1998

8 Dynamics: Solar surface:

9 Granulacja słoneczna

10 Komórka konwekcyjna Bieszczady, Rusinowa Polana

11 Sejsmologia wnętrza Słońca Oscylacje globalne

12

13

14 Mędrek i Murawski (2002) Fale stochastyczne

15 Do we see MHD waves? Moreton waves

16 Do we see MHD waves? - Moreton waves

17 Do we see MHD waves? Moreton waves Seen in H  in the chromosphere at 10000 K (Moreton ’60) Propagation speeds 450-2000 km/s, away from a flare site Propagate almost isotropically; confined to an arc rarely exceeding 120º Have been identified as the intersection of coronal shock waves (due to a flare) with the chromosphere (Uchida ‘68; ‘74) Are not seen to decelerate The generation mechanism has not been made clear yet

18 Do we see MHD waves? - Moreton waves

19 Do we see MHD waves? – Coronal Moreton waves

20 E.g., important for interpretation of the “EIT wave”: Perspectives of Global Coronal Seismology?

21

22 Fale jak na powierzchni wody?

23

24 Do we see MHD waves? New: Coronal Moreton waves Thompson et al. (1999) with SOHO/EIT have investigated a global coronal wave generated by the coronal mass ejection or a flare and occupying a significant part of the solar disk. This wave has been called a coronal Moreton wave. Properties accumulated from observations of more than 50 events: (see http://umbra.nascom.nasa.gov/bjt/lscd/ or Ballai et al. 2005 for details) The waves prefer to propagate radially from the epicentre, stopping at neutral lines and coronal hole boundaries, and distorted by active regions. Speeds range is from 200-600 km/sec. Active regions distort the waves locally, bending them possibly toward the lower Alfvén speed regions. The waves can cause "visible deflection" of coronal magnetic field lines and probably are associated with filament oscillations.

25 Observational evidence for coronal waves is abundant: Periods from 1 s to several min. (Quasi) Periodicity: Resonance (characteristic spatial scales) Dispersion Nonlinearity / self-organisation Characteristic scales: 1 Mm-100 Mm, Alfvén speed 1 Mm/s, sound speed 0.3 Mm/s → periods 1 s – several min - magnetohydrodynamic (MHD) waves

26 Simulations require computers...

27 Symulacje numeryczne – model Mędrek, Murawski, Nakariakov (1998)

28 Impuls w koronie Słońca Mędrek, Murawski, Nakariakov (1998)

29 Impuls w fotosferze Mędrek, Murawski, Nakariakov (1998)

30 Sejsmologia korony słonecznej Dywan magnetyczny

31 The Bastille Slinky:

32 Ponad-arkadą

33 Super-arkada

34 TRACE versus CDS : What is perceived as a coronal loop in SoHO/CDS (with an effective resolution of ~10”) consists of about ~10 loop strands that can be resolved with TRACE (~1”).

35 : : What is the spatial size of the finest loop strands ?

36 Pętle koronalne

37 Parówki w pętli?

38 Żmijki w pętli?

39 Mimo trzęsień nadal istnieje… Solanki (2003)

40 Słońca a Ziemia

41 Conclusions There are MHD waves in the Sun, in STP MHD waves are natural for plasma heating/acceleration MHD waves are sensitive to flows Must take into account effects of inhomogeneity/structuring. The structuring plays a crucial role in the wave dissipation and transformation. The waves are an efficient tool for MHD seismology of the solar atmosphere, which allows us to determine values of the mean parameters of the corona, such as the magnetic field strength, density, pressure, and transport coefficients. Some of these values: the magnetic field strength, viscosity, resistivity and thermal conductivity, are not open to measurement by any other means. We can do this by measuring the properties of MHD waves and oscillations (periods, wavelengths, amplitudes, temporal and spatial signatures), combined with theoretical modelling of the wave phenomena.