PPT-Radiative processes during GRB prompt emission

Based on works by Asaf Peer ITC Harvard University in collaboration with Peter Meszaros PSU Martin Rees IoA Christoffer Lundman Felix Ryde Stockholm. nitrogen. 刘玲莉. . 中国科学院植物研究所. 植被与环境变化国家重点实验室. The 7. th. ISOME & the 4. th. IYEF, . GuangZhou. , 06/12/2013. Outline. Non-reactive nitrogen (N. Astrophysical and Laboratory Plasmas. Lecture 1: Temperature-Density regime. . Many physical processes. . Focus on . Atomic+Plasma. interactions. . Atomic properties are . intrinsic. , . independent of external factors (temp, den, etc.). tropical cyclones. Robert Fovell and . Yizhe. Peggy Bu. University of California, Los Angeles. rfovell@ucla.edu. 1. Thanks to. : . Greg . Thompson, NCAR/. DTC; Ligia . Bernardet. and Mrinal . Biswas. . Sanshiro. Shibata (Konan Univ.). Collaborator: . Nozomu. . Tominaga. (Konan Univ., IPMU). Introduction. Models for the prompt emission. Internal shock model. A standard scenario for a long time.. In astronomy, the main source of information about celestial bodies and other objects is the visible light or more generally electromagnetic radiation.. From Wikipedia.. It also is important for the atmosphere of Earth, so you’ll meet it if you are going into Earth atmosphere science…. and Photocurrent. . in a Blue LED. Ben Stroup & Timothy Gfroerer, Davidson College, Davidson, NC. Yong Zhang, University of North Carolina at Charlotte, Charlotte, NC. Contrast Imaging. Motivation: Solar Cells. Helsinki Winter School in . Theoretical Chemistry. F-. element optical and NMR spectroscopy-insights from experiment and . theory. 17/12/2014. Optical . Spectroscopy. 1:. Lanthanides. Louise Natrajan. Will Potter. Junior Research Fellow, . University of Oxford. Outline. An extended relativistic fluid jet emission model based on observations of M87.. Fitting radio observations to constrain the structure and dynamics of jets.. Judy Racusin. Penn State University. 2008 Nanjing GRB Workshop, Nanjing, China, June 23-27. Broadband Observations of the Extraordinary . Naked-Eye GRB 080319B. . J. L. . Racusin. , S.V. . Karpov. , M. . 2losses are eliminated by employing large combustion vessels at microgravity, heat loss via gaseousradiation is probably the dominant extinction mechanism [8-11].Nevertheless, it is unclear whether ra Radiance Observations. Will McCarty. Global Modeling and Assimilation Office. NASA Goddard Space Flight Center . 2015 JCSDA Summer Colloquium . 28 July . 2015. What is Infrared Radiation?. What is Infrared . Radiance Observations. Will McCarty. Global Modeling and Assimilation Office. NASA Goddard Space Flight Center . 2015 JCSDA Summer Colloquium . 28 July . 2015. What is Infrared Radiation?. What is Infrared . Gabrielle (“Gabby”) Dreyfus, PhD*, Stephen A. Montzka, PhD**, Stephen O. Andersen, PhD*, Richard (“Tad”) Ferris, JD, LLM*, and Durwood Zaelke, JD*. * Institute for Governance & Sustainable Development (IGSD). ?. R. . Mochkovitch. , F. Daigne, R. . Hascoët. (IAP). Basic properties of flares:. from a few 10 s to a few 10. 5. s, superimposed . . to underlying AG light curve. shape and spectral evolution comparable to that of prompt pulses .