1 / 33

Comprehensive Analysis of Scattering Polarization in Young Stellar Objects and Supernovae

This study investigates the polarization characteristics of young stellar objects (YSOs), particularly focusing on single and multiple scattering mechanisms in protoplanetary disks and envelopes. Key observations include parameters from V1352 Aql and DG Tau, detailing their polarization angle and binary system dynamics. Additionally, we analyze the polarization in various supernovae, discussing the electron-scattering atmosphere and its implications for asymmetries in supernova collapses. This research emphasizes the importance of polarimetric techniques in understanding astrophysical phenomena.

zia
Télécharger la présentation

Comprehensive Analysis of Scattering Polarization in Young Stellar Objects and Supernovae

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. Tercera parte

  2. Young Objects

  3. Greene 01

  4. Scattering: Disks/Envelopes SINGLE SCATTERING, Wood et al. (1996)

  5. no-null polarization perpendicular to disk (edge-on) null polarization (pole-on) SINGLE SCATTERING, Wood et al. (1996)

  6. no-null polarization parallel to disk (edge-on) MULTIPLE SCATTERING, Bastien & Menard (1988)

  7. no-null polarization parallel to disk MULTIPLE SCATTERING, Bastien & Menard (1988)

  8. V1352 Aql (T Tau) • Observed: 2005/jun/24, aperture: 1.25” • P(H): [0.76  0.04] %, PA: 124.9° • Binary system • PA axis outflow: 106° (Hartigan et al. 1983) • HH: 32A, 32B, 32C and 32D • PA P(H) ~ parallel to axis jet. • As the jet is perpendicular to disk: • PA P(H) ~ perpendicular to disk. • Consistent with NIR pol. beeing produzed by SINGLE scattering in a optically THIN disk. H Jet 10” Hartigan et al. 1983

  9. DG Tau (T Tau) • Observed: 2005/oct/12, aperture: 1.25” • P(H): [1.29  0.09] %, PA: 129.0° • PA jet: 222° (Lavalley et al. 1997) • PA P(H) is perpendicular to jet. • As the jet is perpendicular to disk: • PA P(H) is // disk. • Consistent with NIR pol. beeing produzed by MULTIPLE scattering in a optically THICK disk. H Jet [OI]6300 - continuum Lavalley et al. (1997)

  10. Envelopes ofEvolvedObjects

  11. PPN Hen 3-1475 Ueta et al. 00 HST, .55m

  12. PPN Hen 3-1475 LNA jun/05 PH (observed): (3.0 0.1)% @ 49.2° (H)obs. // (optical)obs. Model Disk/Torus: Opt. : optic. thick NIR : optic. thin (λ > K) Rodrigues et al. 03

  13. Opportunity Targets(SNs, GRB)

  14. Asymmetries in SNs SN = unresolved source with electron-scattering atmosphere Leonard 06

  15. SN2004bv (Ia) Pereyra & Magalhães 05

  16. SN2004bv (Ia) R ~ 14.5 SN: (0.11  0.02)% @ 119° Foreground: (0.12  0.02)% @ 163° Pereyra & Magalhães 05

  17. SN2005af (II) Pereyra & Magalhães 06

  18. Carnegie Supernova Project site

  19. Pereyra & Magalhães 06

  20. Pereyra & Magalhães 06

  21. Pereyra & Magalhães 06

  22. GRB030329 LNA 03/mar/31 (R) 16’x16’ Afterglow optical polarization: R ~ 16 (1.97 ± 0.48) % @ 83° Magalhães et al. 2003 Asymmetric collapse A Field stars: A:(0.58 ± 0.11)% @ 25° B:(0.06 ± 0.12)% @ 21° OT B

  23. SpectropolarimetryIAGPOL + EIFU

  24. EIFU Lepine 00

  25. EIFU + IAGPOL: Data Extraordinary beam (E) Ordinary beam (O) EIFU 2D reconstructed image Sky E O Extracted fibers (aperture: 2pix = 2”)

  26. RY Tau (T Tau) Gemini image

  27. RY Tau (T Tau) Axis Jet: <PA> ~ 115º Bastien 2007: (Halpha – I) image

  28. RY Tau (T Tau) (1.8  0.2)% @ (11  3)° (binned)

  29. RY Tau (T Tau) U Observed pol. (continuum): (1.8  0.2)% @ (11  3)° ISP: 2.8% @ 26° (Petrov et al. 99) Intrinsic pol.: (1.6  0.2)% @ 134° Axis Jet: <PA> ~ 115º ISP Intrinsic pol. Q Observed pol. Probably, optically thin disk

  30. (Q,U) Diagram: line polarization diagnostic • A. Depolarization line: • extended H source;  ~ pol • linear excursion in (Q,U) • B. Position Angle flip • compact H source;  > pol • loop in (Q,U) • C. Null effect: • circular geometry • dot in (Q,U) A B C

  31. RY Tau (T Tau) U • Loop detected Q • int= 0.5 tan-1(U/Q) = (168 ± 11)°

  32. Summary • A competitive polarimetric facility is available at brazilian LNA site • Projects of medium/long term as monitoring or surveys are (and will be) the main focus of attention • Collaborations with projects in optical and NIR polarimetry (and also spectropolarimetry) are welcomed.

  33. THE END

More Related