The Starburst Program

星爆计划

• 批准号: 1311098
• 负责人: Gregg Hallinan
• 金额: $ 55.34万
• 依托单位: California Institute of Technology
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2013
• 资助国家: 美国
• 起止时间: 2013-09-01 至 2016-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1311098&HistoricalAwards=false
• 关键词: Starburst; Program

This project will use in tandem two large radio antennas located at the Owens Valley Radio Observatory to monitor a sample of nearby active stars for radio bursts associated with large stellar flares or coronal mass ejections (CMEs). The necessary custom electronic hardware to process the signals will be constructed, and advantage will be taken of new receivers on the telescopes; all of these are designed to permit broad spectral bandwidth observations, which give high sensitivity, as well as high time resolution. The search for radio bursts will be carried out in a real-time, automated fashion.Scientific targets include young stellar objects (YSOs), close binary stars, and active M dwarf stars. The target sample consists of 15 stars, and these will be monitored for 2.5 years, accumulating 500 hours of observation time per star. This will give a unique data set for assessing coronal and interplanetary conditions around active stars and their orbiting planetary systems. There will be simultaneous low frequency coverage for every target observed, by using a new low frequency array at Owens Valley. The result will be observations spanning 2 decades of frequency (28 MHz to 6 GHz), thus tracking coronal mass ejection events from the stellar corona into the interplanetary medium. Simultaneous optical spectroscopic observations will also be made, as well as triggered VLBI follow-up observations.These observations should register substantial broader impacts in the form of public interest, which is particularly keen around the current time of Solar maximum. The project team is active in public outreach lectures and other activities. Funding for this project is being provided by NSF's Division of Astronomical Sciences through its Advanced Technologies and Instrumentation program.

该项目将使用位于欧文斯谷射电天文台的两个大型射电天线串联监测附近活跃恒星的样本，以监测与大型恒星耀斑或日冕物质抛射有关的无线电爆发。 将建造必要的定制电子硬件来处理信号，并将利用望远镜上的新接收器;所有这些都是为了进行宽光谱带宽观测，从而提供高灵敏度和高时间分辨率。 对射电暴的搜索将以实时、自动化的方式进行，科学目标包括年轻恒星天体（YSO）、近距离双星和活跃的M矮星。 目标样本由15颗恒星组成，这些恒星将被监测2.5年，每颗星星累积500小时的观测时间。 这将为评估活跃恒星及其轨道行星系统周围的日冕和行星际条件提供独特的数据集。 通过在欧文斯谷使用一个新的低频阵列，将对观察到的每个目标进行同时的低频覆盖。 其结果将是在20年的频率（28兆赫至6千兆赫）范围内进行观测，从而跟踪从恒星日冕到行星际介质的日冕物质抛射事件。 同时还将进行光学光谱观测以及触发VLBI后续观测。这些观测将以公众利益的形式产生更广泛的影响，特别是在目前太阳活动最大的时候。 项目小组积极参加公共外联讲座和其他活动。 该项目的资金由NSF的天文科学部通过其先进技术和仪器计划提供。