Observational signatures for shocks in the solar photosphere

1
Observational signatures for shocks in the
solar photosphere possible HINODE/SOT
observations

• Jan Rybak and A. Kucera, A. Hanslmeier, H. Woehl
• Astronomical Institute, Slovak Academy of
  Sciences
• Tatranská Lomnica, Slovakia
• and
• IGAM/Institute for physics, KF University, Graz
  (Austria)
• KIS, Freiburg (Germany)
• Hinode workshop, Orsay, France, 13-15/11/2007

2
NUMERICAL SIMULATIONS (1)

• Numerical simulations (SIMs) of the solar
  convection supersonic flow near edges of
  granules (10 km/s) and shocks on the G/IG
  interface (Cattaneo et al., 1989, 1990, Steffen
  Freytag, 1991, Solanki et al., 1996, Stein
  Nordlund, 1998, Steiner et al., 1998, Gadun,
  2000) at some locations only

Nesis et al., ApJ, 1993, 399, L99
Stein
Nordlund, 1998, ApJ 499, 914
3
NUMERICAL SIMULATIONS (2)

• numerical simulations of the solar atmosphere
  dynamics (PHCH)
• hot cold components at the same time
• spatial fragmentation, dynamical nature of
  processes
• Wedemeyer et al., 2004, AA 414, 1121

4
OPEN QUESTIONS

• Question stated
• Is amount of the dynamic events well estimated?
• It is much more significant we are used to
  think...
• Is this question worth to study?
• Numerical simulations are affected by
• Limited spatial resolution
• Physical simplifications
• Numerical simplifications
• Possible cumulative effects
• Effects of the magnetic field
• Wedemeyer et al., 2004, AA 414, 1121

5
OBSERVATIONS (1)

• Comparison of the results of numerical
  simulations of the photospheric dynamics (SIMs)
  to observational evidence for dynamical events in
  the upper photosphere (OBSs)
• Signature line broadening near the limb
• Case studies of the individual events
• Statistical analysis
• What has been already done/published?
• SIMs OBSs comparison papers
• 1/ Solanki et al., 1996 1D spectra near limb,
  combination of the spectral line parameters FWHM,
  V_doppler, I_cont, I_res in agreement with the 2D
  HD simulations - Solanki, Ruedi, Bianda, Steffen,
  1996, AA 308, 623
• 2/ Rybak et al., 2004 1D spectra near limb,
  combination of the spectral line parameters FWHM,
  V_doppler, I_cont, I_res in agreement with the
  2D/3D HD simulations, temporal evolution of the
  event, relation to the magnetic flux
  concentration statistical estimates - Rybak,
  Wohl, Kucera, Hanslmeier, Steiner, 2004, AA 420,
  1121

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OBSERVATIONS (2)

• An identified shock signature behaviour of the
  spectral characteristics VTT/Tenerife Fe II
  645.6 nm
• Rybak, Wohl, Kucera, Hanslmeier, Steiner, 2004,
  AA 420, 1121

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OBSERVATIONS (3)

• Shock signature statistics of the FWHM -
  VTT/Tenerife Fe II 645.6 nm line
• 
  Rybak, Wohl, Kucera, Hanslmeier, Steiner, 2004,
  AA 420, 1121

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OBSs SIMs

• SIMSs Wedemeyer-Bohm (ITA, Oslo), O. Steiner
  (KIS, Freiburg)
• CO5BOLD LINFOR3D codes 3D snapshot cubes
  inclination, synthetic spectra integration for
  the Fe II 645.6 nm line, degradation of SIMs
  (30km) to resolution of OBSs (300km)
• Rybák, J., Kucera, A., Wohl, H.,
  Wedemeyer-Bohm, S., Steiner, O., 2006, ASP Conf.
  Proc. Series, 354, 80-85

• Rybak, Wohl, Kucera, Hanslmeier, Steiner,
  2004, AA 420, 1121

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AIM

• OBSs
• 2D time series of the spectral line profiles at
  different CLV positions using the best spatial
  resolution with the adaptive optics
• Search for observational evidences of the dynamic
  events in the photosphere (CVL)
• Possibilities
• VTT/Tenerife VTT TESOS (KIS, Freiburg), VTT
  Goettingen FPI (SWG, Goettingen)
• DST/SacPeak DST IBIS (INAF, Arcetri)
• THEMIS/Tenerife THEMIS IPM (INAF, Roma)
• HINODE SOT

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OBSERVATIONS (4)

• OBSs VTT, Observatorio del Teide, (Tenerife)
  Echelle spectrograph TESOS, 16-28/10/2006
• DATA taken mostly only with Tip/Tilt ON, AO
  mostly for the disk centre
• 1 CLV TESOS SET TESOS 543.4 nm 0,45,60
  degrees positions
• 24 scans per run
• each scan 101steps per 1.2mA,
  25s, /- 0.609A, delta 0.0012A, t_exp 50ms
• 0 degrees with AO (2
  interruptions)
• 45 degrees with TT (4
  interruptions)
• 60 degrees without TT/AO (TT
  problems)
• DAY 26/10/2006

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OBSERVATIONS (5)

• Example of a shock signature 60 degrees scan
  16, position 22,20 arc sec
• WL typical, the best images
• NB I_cont, I_res, V_dopp, FWHM_at_0.5, v_bis_at_0.5,
  EQVW

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OBSERVATIONS (6)

• Example of a shock signature 60 degrees scan
  16, position 22,20 arc sec

13
OBSERVATIONS (7)

• Statistics of the SPCHs 0 (two), 45, and 60
  degrees, better scans only, gt 1 million samples

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FUTURE OUTLOOK

• OBSs SIMs aim to publish not only
  observational evidences...
• SIMs data available S. Wedemeyer-Bohm (ITA,
  Oslo), O. Steiner (KIS, Freiburg)
• 3D snapshot cubes, inclination, synthetic spectra
  integration for the Fe I 543.4 nm line
• CO5BOLD LINFOR3D codes
• Degradation of SIMs (30km) to resolution of OBSs
  (300km) method invented and already presented
  here for comparison of the echelle
  high-resolution spectra with results of such
  simulations -gt new one based on suggestions
  published by Keller (2006)
• Targets
• statistical distributions -gt is the photosphere
  so dynamic ?
• Close-look into 3D cubes of the physical
  parameters where/when degraded synthetic spectra
  are similar to the observed ones -gt is the shock
  really what have in mind?
• Other ones e.g. acoustic flux generation in the
  photosphere (disk centre)
• Future to add chromospheric signatures

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HINODE/SOT ?

• OBSs large volume of spectral profiles with
  different CL positions (20 x 100 arcsecs,
  1hour)
• SOT/NFI filtergrams - 90 mA spectral
  resolution Fe I 557.6 nm
• Scanning the profile available but a 30s cadence
  seems to be too low
• SOT/SP spectral profiles of the Fe I 630.1 and
  Fe I 630.2 nm lines
• Can the magnetic and the Doppler signal be
  devided using inversions of these profiles ?
• SOT/BFI context images Ca II H, G-band
  channels
• Avoiding the seeing problems of the ground-based
  observations would be so helpful...