1 / 37

Polarization in Astronomy

Polarization in Astronomy. 天文学中的偏振. Cheng Zhao 2014/05/09. Contents. Introduction Measurement Mechanisms Applications References. Introduction. Theory. Transverse electromagnetic waves. Electric field is the main component interacting with matter, hence it is

lee
Download Presentation

Polarization in Astronomy

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. Polarization in Astronomy 天文学中的偏振 Cheng Zhao 2014/05/09

  2. Contents • Introduction • Measurement • Mechanisms • Applications • References

  3. Introduction • Theory Transverse electromagnetic waves. Electric field is the main component interacting with matter, hence it is used to describe polarization. Polarization: Asymmetry of the oscillation direction

  4. Introduction • Classification Basis: oscillation feature of Facing the propagation direction of light, there are only two polarization states (basis): linear polarization in x, y direction.

  5. Introduction • QM Description Transformation with linear polarization basis (+) ()

  6. Introduction • Formalism Stokesvector: I：intensity Q, U：linear component V：circular component （For linear polarizationV=0） Degree of polarization Natural light: P=0 Linear polarization: P=1

  7. Measurement • Polarizer – Sheet or Plate Polarizers • Sheet polarizer • Aligned anisotropic crystals or polymers. Extinction ratio(transmitted intensity for the polarizing direction over that for the perpendicular direction) is typically about 100. • Wire-grid polarizer • Conducting wires with spacing smaller than the wavelength (From sub-millimeter to optical regime). Fairly large extinction ratios, and applicable over large wavelength ranges. • Brewster window • A simple piece of glass. The only polarizer in far UV regime. Extinction ratio mostly depends on the incidence angle.

  8. Measurement • Polarizer– Polarizing Beam-Splitters • Keep all the incident light as output. The polarizer acts as a beam-splitter. • Cube beam-splitter with multilayer coating • Fairly large extinction ratios are obtained when there are internal reflections at the Brewster angle. • Birefringentcrystals • The refractive index in the crystal is an anisotropic tensor. Incident light that is not in the direction of the crystal axes will be split into two beams with different linear polarization states and speeds.

  9. Measurement • 起偏器

  10. Measurement • Retarder Retard the phase of electric field. Manipulate polarization by rotating the angle of linear polarization and thus converting circular into linear polarization. Quarter-wave and half-wave retarders

  11. Measurement • Retarder

  12. Measurement • Novel Components • Mostly owing to developments in the field of nanophotonics and by the liquid crystal display and telecommunications industries. • Circular polarizer • Based on chiral nanostructures. [Gansel et al. 2009] • Passive devices (theta cell) • Based on twisted nematic liquid crystals that locally rotate the direction of linear polarization. • Many astronomical objects exhibit a centrosymmetric linear polarization pattern around a central source. Such a passive liquid crstal device aligns this pattern in one direction so that only one Stokes parameter has to be measured. [Snik, Frans, 2009]

  13. Measurement • Novel Components • Polarization grating • Such a grating not only acts as a dispersion element, but as a polarizing beam-splitter as well. This polarization grating may replace the combination of a spectrograph and a polarizer. [Packham et al. 2010] • Polarization-maintaining (birefringment) fiber • Polarimetric versions of fiber-based integral field units. [Lin and Versteegh 2006]

  14. Measurement • Detector • Similar as other astronomical instruments: low dark current, high linearity, high dynamic range, small gain variations, etc. • Read-out noise • Polarimetric noise levels should be smaller than photon noise. Nonideal detector properties can create unwanted polarization signals [Keller 1996]. Electron-multiplying CCD (EMCCD) can reduce the influence of read-out noise. • Read-out speed • Polarimetry often requires fast read-out rates, sometimes >1 kHz. Single-pixel detectors like photomultiplying tubes (PMT) and avalanche photodiodes (APD) can cope with this speed. CCD and other 2D detectors are usually too slow.

  15. Measurement • Detector • ZIMPOL(Zurich Imaging Polarimeter) • Shifting charges back and forth in synchrony with the polarization modulation, without reading out. Developed for VLT for the direct detection of extra solar-planets. • Advantage: images in two polarization sates are registered practically simultaneously, no flat field problems. Atmosphric and instrumental aberrations affecting both images are identical. • Disadvantage: The many charge transfers and asymmetries of charge transfer limit the polarimetric performance.

  16. Measurement • Detector • CMOS • Each pixel has a individual read-out capacitor [Keller, 2004]. However it may have high dark current.

  17. Mechanisms • Scattering and Reflection – Theory Fresnel equations describe the phase shift (electric field) of the reflected light when light moves from a medium into a second medium. If the light is incident at the Brewster angle, the reflection light is perfectly linearly polarized. For complex particles having a preferred handedness(like biology molecules), the reflection light can be circularly polarized.

  18. Mechanisms • Scattering and Reflection – Sources • Solar system bodies • Microphysical properties of small particles like dust grains and atmospheric aerosols can only be unambiguously determined using spectropolarimetry [Hansen and Travis, 1974],such as the small sulphuric acid cloud droplets in Venus’atmosphere. • Stellar ejecta and • circumstellar material • Disks, jets, (AGN) halo, • exoplanets, etc.

  19. Mechanisms • Multiple Scatering – Theory When aligned dust grains (by magnetic field) are illuminated anisotropically and scatter this light, they can also produce circular polarization.

  20. Mechanisms • Multiple Scattering – Sources • Interstellar dust aligned with the galactic magnetic field • Smallest dimension of nonspherical dust grains are always aligned with the direction of the local magnetic field[Hough, 2007]. Perfect for mapping and understanding the galactic magnetic field structure. • Dense molecule clouds • Star formation area,disks around young stars(protostar disk and protoplanetary disk).

  21. Mechanisms • Cyclotron and Synchrotron Radiation – Theory Non-relativistic electron gyrates around a strong magnetic field: cyclotron radiation.Linear polarization in the direction perpendicular to the magnetic field; circular polarization along the direction of the magnetic field. For relativistic electron,the radiation is synchrotron radiation. Strongly linearly polarized. Circular polarization is also generated when the magnetic field has a net component along the line of sight. In extreme environments, synchrotron radiation dominates.

  22. Mechanisms • Cyclotron and Synchrotron Radiation – Sources • AGNjets • Neutron star • Study the structure of magnetic fields. Crab nebula Jet of M87

  23. Mechanisms • Zeeman Effect – Theory Magnetic field modifies the energy of the magnetic sublevels of an atom (-μ·B), and splits the spectral lines. According to the selection law of transition, Δm=0,±1. For Δm=±1, angular momentum of the emergent photon is ±ℏ (projection along the direction of the magnetic field), corresponding to left-hand and right-hand polarization respectively(σpolarization). For Δm=0, the photon has no angular momentum component along the magnetic field direction, and is linearly polarized(πpolarization).

  24. Mechanisms • Zeeman Effect – Theory Polarization state depends on the orientation of the magnetic field with respect to the line of sight. The emergent light can be red/blue-shifted by the strong magnetic field. Polarization due to Zeeman effect

  25. Mechanisms • Zeeman Effect – Sources • Sunspot • The magnetic field is fairly weak in this case. • Large-scale and strong magnetic fields • Particularly applies to unresolved stars. Surface magnetic field of SU Aurobtained through Zeeman effect

  26. Mechanisms • Hanle Effect – Theory When there is magnetic field along the line of sight, the scattering linear polarization will precess around it, and is mostly depolarized. It is highly complementary to Zeeman effect: the sensitive magnetic field strength is much smaller, typically mG – 100G.Furthermore, Hanle effect can be applied for mixed-polarity magnetic field [Trujillo Bueno, 2006 & 2009].

  27. Mechanisms • 汉勒效应(Hanle Effect)-原理 Hanle Effect Polarization by different directions of magnetic field

  28. Mechanisms • Hanle Effect – Sources • Sun(corona) • A standard tool in solar physics. • Stellar atmosphere and stellar wind Brightness and magnetic field of a sunspot group

  29. Applications • Application of Polarization in Astronomy Bastien, Manset, et al., 2011, Astronomical Polarimetry 2008: Science from Small to Large Telescopes

  30. Applications • Solar Physics & Space Physics 目前，太阳表面和内部的许多物理过程和活动现象都还未被完全了解清楚，主要原因在于获取一些物理参量（如磁场、密度等）较为困难。 偏振被广泛地应用到了太阳物理中，例如探测日冕的电子密度、磁场、冕流等。 太阳的许多剧烈活动现象，例如耀斑等，都与太阳上的磁暴有关，因此偏振的观测还有助于了解太阳活动的过程、预测空间“天气”。

  31. Applications • Star Formation and Circumstellar Disks 过去的20年中，星周环境（circumstellar environment）的模型取得了重大的进展。现在已经有了年轻星体（YSO）周围尘埃密度分布的详尽模型，包括图像、色图与偏振图。 偏振观测能够给出尘埃的性质与排列，从而检验理论模型。 在更高的分辨率上，偏振可以用于原行星盘的研究。在光学和近红外波段，偏振可以给出尘埃微粒非常详尽的性质，包括它们的大小、形状与孔隙等。利用这些性质可以推断尘埃（与行星）的演化过程和原行星盘动力学模型。

  32. Applications • Stellar Evolution and Magnetic Stars 2005年后，通过光谱偏振测量，在一些低温度、低质量、充分对流的主序星上发现偶极主导的磁场，与现有的动力学理论相矛盾。 偏振观测有助于了解恒星内的对流、对流层与辐射层的相互作用，从而改进恒星演化和恒星结构的理论模型。 由于对磁场和尘埃散射敏感，偏振还可用来研究演化晚期的星体，例如中子星、超新星遗迹等。对超新星偏振辐射的研究，可以推测超新星爆发的一些细节。 此外，由于偏振能够确定一些几何性质，它也被广泛地用来研究双星，限制其理论模型。

  33. Applications • Extrasolar Planet Detection 目前已知的地外行星中，大部分都依赖于间接观测，因为它们相对于宿主恒星而言太昏暗了。考虑到行星反射的光是高度偏振的，而恒星发出的光在很大程度上不具有偏振特性，现在偏振正被用来探测地外行星。 理论上讲，对地外行星的偏振观测可以获取大量信息，例如轨道倾角、质量、大气微粒性质、反射率、行星半径、温度等。偏振测量因而被当作将来地外行星探测的重要手段，并能对行星大气模型给出更多的约束。 偏振可以用于对行星云层或海洋组成的研究，而一些复杂的生物分子能散射出圆偏振光，因此偏振又是极少的能够探测地外生命的方法之一。

  34. Applications • Interstellar Medium 从上世纪50年代起，就提出了尘埃排列理论，用以解释银河系中的线偏振。近几年该理论取得了显著进展。 偏振光谱能够确定尘埃的组成、大小、增长和消失，从而确定分子云与星际介质的相互作用。 在远红外和亚毫米波段观测到的去偏振效应需要用磁场来解释，而偏振观测可以很好地确定磁场的性质，但仍需要更多高空间分辨率的观测。 对恒星形成星云的圆偏振观测，还可能使我们了解地球生物分子同手型的来源。

  35. Applications • Galaxies and AGN 偏振在AGN统一模型的建立和发展上起了重要作用。 最近的高空间分辨率偏振观测显示出核附近的信息，有助于发展AGN的统一理论，和研究AGN与宿主星系的相互作用。对更高红移处AGN的偏振研究可能使我们了解AGN的演化和与环境的相互作用。 在光学和近红外波段的光谱偏振测定，可以确定无法直接分辨出的几何结构和散射颗粒的运动速度。

  36. Applications • Cosmology 宇宙微波背景（CMB）的偏振在微开尔文的水平，有两种偏振模式，称为E模式和B模式。 CMB的偏振证实了早期宇宙密度的不均匀性（各向同性的入射光通过汤姆孙散射无法产生偏振），更进一步，CMB偏振的研究，可以确定早期宇宙密度（温度）起伏的性质和成分。 通过CMB偏振的研究，可以获知宇宙早期的信息，以及宇宙大尺度结构的形成。

  37. References • Snik, Keller, 2013, Astronomical Polarimetry: Polarized Views of Stars and Planets, Springer Science+Business Media Dordrecht, p.175 • Bastien, Manset, et al., 2011, Astronomical Polarimetry 2008: Science from Small to Large Telescopes • 赵凯华, 2004, 新概念物理教程·光学, 高等教育出版社 • Schmid, Gisler et al., 2005, ZIMPOL/CHEOPS: a Polarimetric Imager for the Direct Detection of Extra-solar Planets • Trujillo Bueno, 2009, Diagnostic methods based on scattering polarization and the joint action of the Hanle and Zeeman effects • Raouafi, 2011, Coronal Polarization • Hough, 2007, New opportunities for astronomical polarimetry, J. Quantit. Spectr. Rad. Transfer, 106, 122–132

More Related