权益分类	功能权益	普通用户	{{item.name}}会员
{{category.name}}	{{benefitItem.name}}

Hertfordshire Astronomy

赫特福德郡天文学

基本信息

批准号：
ST/J001333/1
负责人：
Janet Drew
金额：
$ 168.93万
依托单位：
University of Hertfordshire
依托单位国家：
英国
项目类别：
Research Grant
财政年份：
2012
资助国家：
英国
起止时间：
2012 至无数据
项目状态：
已结题

来源：
https://gtr.ukri.org/projects?ref=ST%2FJ001333%2F1
关键词：
Hertfordshire Astronomy

项目摘要

The Centre for Astrophysics Research carries out observational programmes spanning the wavelength range from X-ray up to the radio - supporting this by extensive computer modelling, theoretical studies and instrument development. Our research ranges from theoretical modelling of the highest energy process in the Universe through to inventing our own instruments to detect planets outside our Solar System. In between these extremes, we carry out the largest multi-wavelength surveys conducted to date to understand the properties of stars, galaxies and their evolution. Our research makes use of observations from all of the main European and international astronomical observatories, including ground-based observatories at optical, radio and submillimetre wavelengths, and space observatories at wavelengths ranging from the far infrared to gamma rays. We also use computer simulations to obtain a better understanding of the physical processes detected in our observations. Below is a brief description of our research in each of these areas.We perform searches of nearby stars to discover planets. We especially target low mass M stars since they are the dominant type of star in the Universe and have not yet been searched. We focus on detection through Doppler wobble and by looking for planets periodically eclipsing their parent star. During the period of the grant we expect to make the first detections of Earth-mass planets in the habitable zones of the closest stars. We also discover, follow-up and model the properties of the coolest brown dwarfs whose temperatures overlap with those of planets. These studies aim to clarify the population of brown dwarfs and to establish how their modes of formation fit in with those of their brethren of different masses, ie. heavier (stars) or lighter (planets).The Milky Way is our home galaxy. The material in the form of gas is the raw material for the formation of stars and planetary systems. At the end of stellar lives some of this material remains locked up in stellar remnants but much of it is returned in late superwind phases and supernova explosions. This cycle is responsible for the chemical enrichment of the gaseous medium and is important for its dynamics, because of the thermal and mechanical energy injected into the gas. By using large area mainly imaging surveys, our research looks at this gas in the Milky Way and its satellites. Our surveys of the Milky Way will span the optical to sub-mm domains tracing extinction, molecular clouds, their dust properties and associated star formation. We thus study the relationship between star formation, dust and molecular cloud properties.In the nearby Universe it is possible to appraise how stars form and evolve in different environments, from small dwarf galaxies to the very outer regions of galaxies like our own. Our research focuses on the gas content of galaxies, which provides the material for star formation, and links this to stellar populations and the locations of star formation in the full range of local galaxies. By understanding the processes that trigger star formation and its evolution in the nearby Universe, we can begin to apply this understanding to the very earliest galaxies and the formation of stars in the distant Universe.A new generation of surveys is mapping out the most distant galaxies, and allows us to investigate what links the processes of star formation and the growth of supermassive black holes. We also use detailed X-ray and radio observations to measure the energy injected by jets ejected from supermassive black holes into distant galaxies and clusters of galaxies, affecting star formation and gas properties, and having a long-term role in their evolutionary history. Understanding the particle composition, magnetic field properties, dynamics and energetics of these relativistic jets is essential in order to get a complete picture of star formation and of galaxy evolution.

天体物理研究中心开展的观测项目涵盖从 X 射线到无线电波的波长范围 - 通过广泛的计算机建模、理论研究和仪器开发来支持这一项目。我们的研究范围从宇宙最高能量过程的理论建模到发明我们自己的仪器来探测太阳系外的行星。在这两个极端之间，我们进行了迄今为止最大规模的多波长调查，以了解恒星、星系的特性及其演化。我们的研究利用了所有主要欧洲和国际天文台的观测结果，包括光学、无线电和亚毫米波长的地面天文台，以及从远红外到伽马射线波长范围的太空天文台。我们还使用计算机模拟来更好地理解我们观察中检测到的物理过程。以下是我们在每个领域的研究的简要描述。我们对附近的恒星进行搜索以发现行星。我们特别关注低质量 M 星，因为它们是宇宙中的主要恒星类型，但尚未被搜索到。我们专注于通过多普勒摆动进行探测，并寻找周期性地遮蔽其母星的行星。在资助期间，我们预计将在距离最近的恒星的宜居带中首次探测到地球质量的行星。我们还发现、跟踪和模拟最冷的褐矮星的特性，这些矮星的温度与行星的温度重叠。这些研究旨在澄清褐矮星的种群，并确定它们的形成模式如何与其不同质量的兄弟相适应，即。更重（恒星）或更轻（行星）。银河系是我们的家乡星系。气体形式的物质是形成恒星和行星系统的原材料。在恒星生命结束时，其中一些物质仍然被锁在恒星残骸中，但其中大部分在超级风阶段和超新星爆炸后期返回。该循环负责气体介质的化学富集，并且由于注入气体中的热能和机械能而对其动力学非常重要。通过使用大面积主要成像调查，我们的研究着眼于银河系及其卫星中的这种气体。我们对银河系的调查将跨越光学到亚毫米域，追踪灭绝、分子云、它们的尘埃特性和相关的恒星形成。因此，我们研究恒星形成、尘埃和分子云特性之间的关系。在附近的宇宙中，可以评估恒星在不同环境中的形成和演化，从小型矮星系到像我们这样的星系的最外层区域。我们的研究重点是星系的气体含量，它为恒星形成提供了物质，并将其与恒星种群以及整个当地星系中恒星形成的位置联系起来。通过了解附近宇宙中触发恒星形成及其演化的过程，我们可以开始将这种理解应用于遥远宇宙中最早的星系和恒星的形成。新一代的调查正在绘制最遥远的星系，并使我们能够研究恒星形成过程和超大质量黑洞生长之间的联系。我们还使用详细的 X 射线和射电观测来测量从超大质量黑洞喷射到遥远星系和星系团的喷流注入的能量，影响恒星的形成和气体特性，并在其演化历史中发挥长期作用。为了全面了解恒星形成和星系演化，了解这些相对论性喷流的粒子组成、磁场特性、动力学和能量学至关重要。