Spectro-interferometric imaging of protoplanetary disks

星星和行星的形成是现代天体物理学中最活跃、最令人兴奋的研究领域之一。这个领域的许多基本问题都与原行星盘最内部区域的结构和物理学有关，在那里，物质被输送到形成中的星星上，以强大的喷流和外流喷出，或吸积到新形成的行星上。然而，大多数上述过程发生在星星周围的几个天文单位内，无法用传统的成像技术进行直接调查。在这个研究项目中，我们将利用红外干涉测量提供的新机会，获得原行星盘的类地行星形成区的独立模型图像。提供衍射限制的200米光学望远镜的角分辨率，这些图像将产生独特的磁盘+吸积物理约束，并允许我们搜索行星相关的磁盘表面结构，如潮汐清除间隙或嵌入的原行星周围的热吸积点。利用VLTI、CHARA和阿尔马干涉仪现有的和即将到来的红外和亚毫米仪器，我们将在宽波长范围内空间分辨内部盘区域。为了得到三维密度和温度分布和尘埃成分，我们将采用TORUS气体+尘埃辐射传输程序。采用高光谱色散（高达R=12000），我们的干涉观测将空间和光谱解决光谱线发射的起源，提供有关亚AU尺度上的气体速度场的直接信息。光谱干涉仪和光谱数据将使用大型TORUS线辐射传输网格进行建模，为YSO中的质量吸积和外流发射机制提供新的基本约束。

Star and planet formation is one of the most active and exciting research areas of modern astrophysics. Many of the fundamental open questions in this field are related to the structure and physics of the innermost regions of protoplanetary disks, where material is transported onto the forming star, ejected in powerful jets & outflows, or accreted onto newly-formed planets. However, most of the aforementioned processes take place in the inner few astronomical units around the star, eluding a direct investigation with conventional imaging techniques. In this research project, we will employ the new opportunities provided by infrared interferometry to obtain model-independent images of the terrestrial planet-forming zone of protoplanetary disks. Providing the angular resolution of a diffraction-limited 200 m optical telescope, these images will yield unique constraints on disk+accretion physics and allow us to search for planet-related disk surface structures, such as tidally cleared gaps or hot accretion spots around embedded protoplanets. Using existing and upcoming infrared & sub-mm instrumentation at the VLTI, CHARA and ALMA interferometers, we will spatially resolve the inner disk regions over a wide wavelength range. In order to derive the 3-D density & temperature distribution and dust composition, we will employ the TORUS gas+dust radiative transfer code. Employing high spectral dispersion (up to R=12000), our interferometric observations will spatially and spectrally resolve the origin of spectral line emission, providing direct information about the gas velocity field on sub-AU scales. The spectro-interferometric and spectroscopic data will be modelled using a large TORUS line radiative transfer grid, providing fundamental new constraints on the mass accretion and outflow launching mechanism in YSOs.