The Polstar high resolution spectropolarimetry MIDEX mission
The Polstar high resolution spectropolarimetry MIDEX mission
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Polstar 高分辨率光谱偏振 MIDEX 任务
DOI：
10.1007/s10509-022-04107-9
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发表时间：
2022
影响因子：
1.9
通讯作者：
Wisniewski, John
中科院分区：
文献类型：
--
作者：
Scowen, Paul A.;Gayley, Ken;Ignace, Richard;Neiner, Coralie;Vasudevan, Gopal;Woodruff, Robert;Casini, Roberto;Shultz, Matt;Andersson, B.-G.;Wisniewski, John
Polstar任务将提供一个星载60厘米分光偏振计，在紫外（UV）波长下工作，捕获所有四个斯托克斯参数（强度，两个线性偏振分量，和圆偏振）Pol星星的能力旨在满足其目标，确定如何拱星气流改变和通知大质量星星的演变，影响恒星残余人口，搅拌和丰富星际介质（ISM）。这些将通过研究热恒星的风和盘的动力学几何结构、星际尘埃的组成和磁性排列以及在重要过渡边界处的紫外线亮恒星的恒星形成吸积盘来实现。这些区域共同描绘了大质量恒星之间的一种双向界面及其对我们银河系的影响，其中恒星风使ISM富含金属和动能，在经历超新星之前预处理它们的环境和恒星端点。ISM尘埃反过来揭示了导致新星星形成的成分和磁环境，Herbig Ae/Be恒星的吸积盘揭示了ISM气体如何返回以形成新的大质量恒星。Polstar将联合收割机结合时域高分辨率光谱学和高精度紫外偏振测量。多普勒频移紫外线共振线不透明度将提供有关拱星运动学的信息，而偏振提供有关看不见的结构的补充几何信息。最小星际尘埃颗粒的组成和磁性排列提供了利用辐射排列理论（RAT）的ISM探测器。Polstar将在122-200 nm的远紫外（FUV）波长下以约的高光谱分辨率工作，在122-320 nm的FUV和近紫外（NUV）波长下以较低的光谱分辨率工作。预计检测到的偏振水平弱至0.1%，时间节奏范围从5-10分钟的大多数风变率研究，到数小时或数天的采样旋转，到数天或数周的采样双轨道，到数月到一年的采样子结构的内部区域的原行星盘。亚米级孔径非常适合访问这种广泛的时域科学，通过限制到几百颗明亮的大质量恒星，必然被一个小到中等的星际尘埃柱包围，告知恒星的属性和它们被看到的ISM。因此，重点是我们自己的星系及其演化驱动因素，但麦哲伦云中的一些目标提供了将这种理解扩展到低金属含量环境的潜力。
ThePolstarmission will provide a space-borne 60 cm spectropolarimeter operating at ultraviolet (UV) wavelengths, capturing all four Stokes parameters (intensity, two linear polarization components, and circular polarization).Polstar’s capabilities are designed to meet its goal of determining how circumstellar gas flows alter and inform massive star evolution, affect the stellar remnant population, and stir and enrich the interstellar medium (ISM). These will be achieved by investigating the dynamical geometries in the winds and disks of hot stars, the composition and magnetic alignment of interstellar dust, and the star-forming accretion disks of UV-bright stars at an important transition boundary. Together these areas map out a kind of two-way interface between massive stars and their effect on our galaxy, wherein the stellar winds enrich the ISM with metals and kinetic energy, preconditioning their environment and the stellar endpoints prior to undergoing supernova. The ISM dust in turn reveals the composition and magnetic environment leading to new star formation, and the accretion disks of Herbig Ae/Be stars reveal how the ISM gas returns to make new massive stars.Polstarwill combine high-resolution spectroscopy in the time domain with high-precision UV polarimetry. Doppler-shifted UV resonance line opacity will provide information about circumstellar kinematics, while polarization gives complementary geometric information about unseen structures. The composition and magnetic alignment of the smallest interstellar dust grains provides a probe of the ISM utilizing radiative alignment theory (RAT).Polstarwill operate in the far-UV (FUV) at 122–200 nm at high spectral resolution of around, and at FUV and near-UV (NUV) wavelengths of 122–320 nm at lower spectral resolutions of. Detection of polarization levels as weak as 0.1% are expected, with a temporal cadence ranging from 5–10 minutes for most wind variability studies, to hours or days for sampling rotation, to days or weeks for sampling binary orbits, to months to a year for sampling substructure in the inner regions of protoplanetary disks. Sub-meter-class aperture is well suited to access this wide array of time domain science, made possible by restricting to a few hundred bright, massive stars, necessarily extincted by a small to moderate column of interstellar dust, informing both the attributes of the stars and the ISM through which they are seen. As such, the focus is on our own galaxy and its evolutionary drivers, but a few targets in the Magellanic clouds offer the potential to extend this understanding to low-metallicity environments.
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