1 / 27

Spectropolarimetry with the green line: Observations and Simulations A . Bemporad

Spectropolarimetry with the green line: Observations and Simulations A . Bemporad INAF- Osservatorio Astrofisico di Torino, Italy. Introduction : LCTP for the green line Spectropolarimetric o bservations during the 2010 TSE Simulation of green line polarized emission. OUTLINE.

xuxa
Download Presentation

Spectropolarimetry with the green line: Observations and Simulations A . Bemporad

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Spectropolarimetry with the green line: Observations and Simulations A. Bemporad INAF-OsservatorioAstrofisicodi Torino, Italy ISSI Team on “Coronal Magnetometry”, First Meeting, 24/02-01/03/2013, Bern

  2. Introduction: LCTP for the green line Spectropolarimetricobservationsduring the 2010 TSE Simulation of green line polarizedemission OUTLINE

  3. (in collaboration with L. Abbo, G. Capobianco, S. Fineschi, G. Massone) LCTP calibration

  4. Liquid-crystal Tunable Lyot Filter for Solar Coronagraphy

  5. LCTP Perfomances

  6. (in collaboration with L. Abbo, C. Benna, P. Calcidese, G. Capobianco, S. Fineschi, G. Massone, M. Romoli) Fe xiv 530.3 spectropolarimetry: observations

  7. The CorMag was operated during the total solar eclipse of July, 11th 2010 on Tatakoto Atoll (French Polynesia)

  8. 2010 TSE coronalconfiguration K-corona image (filtered) by M. Druckmuller

  9. 2010 TSE coronalconfiguration SDO/AIA 171 SOHO/LASCO C2 run.diff.

  10. 2010 TSE Cormag data • 1024X1024 pix, 16 bit/pix, 2MB per image, pix 24um, 6.2’’/pix • 31 exposures (exptime 8 sec): 21, 5 and 5 with pol. angles 0°, 60° and 120° resp.

  11. 2010 TSE cormag & ekpol data LASCO/C2 + EKPol CorMagFeXIV + EIT 304

  12. LCTP scan

  13. cormagresults FeXIV line intensity FeXIV line doppler shifts

  14. Prasad et al. (2013) cormagresults Habbal et al. (2010) FeXIV line widths (s) (afterdeconvolution with Lyotfilterinstrumentalprofile) Fe 13+ionskinetictemperatures

  15. Pasachoff et al. (2011) Fe13+Kinetic Temperature contourlevels:Blue: 1.5106 Kgreen: 3.0106 Kred : 4.5106K K-corona image by M. Drukmuller

  16. CoMP-S instrument @ Lomnicky STIT Observatory (SLOVAK R.)

  17. LCTP FILTER @ CLIMSO CORONAGRAPH PIc du midi (france)?

  18. (in collaboration with L. Abbo, L. Belluzzi, R. Casini, S. Fineschi, P. Judge) Fe xiv 530.3 spectropolarimetry: simulations

  19. Simulations of FeXIV green line polarizedemission: performed with the numerical code originallydeveloped by P. G. Judge and R. Casini for forbiddenlines (see Casini & Judge 1999; Judge & Casini 2001). Lines assumed to be opticallythin, excited by (anisotropic) photosphericradiation + thermalparticlecollisions. Assumingthatcollisionalexcitationisisotropic → collisional component isunpolarized → collisionaldepolarization. ScatteringredistributionfunctionPa’is proportional to ~ sin2q’ (a2 + b2 cos2q) withqandq’ angles between the field and the direction of the incident and scattered radiation, -a2 / b2 = 1/3 → q VV~ 54.6° (House 1977). Direction of linear polarization→ projecteddirection of POS magneticfield, butpolarizationchangessignatq VV→ambiguity by 90°. The simulation

  20. Q/I (%) Q/I (%) qB = ± qVV qB = ± π/4 + First test: centereddipole, no losintegration (dipolarfield, isothermal corona at 2ˣ106 K, densityprofile from Antonucci et al. (2006) for streamer – c.holeinterface)

  21. |U|/I (%) |U|/I (%) qB = ±qVV, π ± qVV qB = kπ/2 + First test: centereddipole, no losintegration (dipolarfield, isothermal corona at 2ˣ106 K, densityprofile from Antonucci et al. (2006) for streamer – c.holeinterface)

  22. Second test: centereddipole, losintegration Q/I (%) Q/I (%) qB = ± qVV qB = ± π/4 + (dipolarfield, isothermal corona at 2ˣ106 K, densityprofile from Antonucci et al. (2006) for streamer – c.holeinterface)

  23. Second test: centereddipole, losintegration |U|/I (%) |U|/I (%) qB = ±qVV, π ± qVV qB = kπ/2 + (dipolarfield, isothermal corona at 2ˣ106 K, densityprofile from Antonucci et al. (2006) for streamer – c.holeinterface)

  24. third test: shifteddipole, losintegration Q/I (%) Q/I (%) + (dipolarfield, isothermal corona at 2ˣ106 K, densityprofile from Antonucci et al. (2006) for streamer – c.holeinterface)

  25. third test: shifteddipole, losintegration |U|/I (%) |U|/I (%) + (dipolarfield, isothermal corona at 2ˣ106 K, densityprofile from Antonucci et al. (2006) for streamer – c.holeinterface)

  26. fourth test: centereddipole, losintegration, loopdensity [dipolarfield, isothermal corona at 2ˣ106 K, densityprofile from Antonucci et al. (2006) for streamer – c.holeinterface + loopat 109 cm-3 from Ugarte-Urra et al. (2005)]

More Related