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• W3044812873 abstract "Alwyn Wootten, Bryan Butler, Antonio Hales, Stuartt Corder, 1 Robert Brown2 & David Wilner3 Abstract. Stars and planets are the fundamental objects of the Universe. Their formation processes, though related, may differ in important ways. Stars almost certainly form from gravitational collapse and probably have formed this way since the first stars lit the skies. Although it is possible that planets form in this way also, processes involving accretion in a circumstellar disk have been favored. High fidelity high resolution images may resolve the question; both processes may occur in some mass ranges. The questions to be answered in the next decade include: By what process do planets form, and how does the mode of formation determine the character of planetary systems? What is the distribution of masses of planets? In what manner does the metallicity of the parent star influence the character of its planetary system? In this paper we discuss the observations of planetary systems from birth to maturity, with an emphasis on observations longward of 100 μm which may illuminate the character of their formation and evolution. Advantages of this spectral region include lower opacity, availability of extremely high resolution to reach planet formation scales and to perform precision astrometry and high sensitivity to thermal emission. Introduction. Planets are cool bodies and emit through reflected light from their host star and through their own blackbody radiation. Since their mass is a fraction of that of their parent stars, direct radiation from planets has been difficult to detect; most of our information on extrasolar planets is derived from indirect observation, usually at optical and infrared wavelengths. Planets form either as stars do, through gravitational collapse, or through accretion of material in a remnant disk. During early phases under the latter scenario, the large luminous regions in which accretion occurs may be directly observable. As the condensations grow and sweep up material from their natal disks, structures in the disks can signal the presence of embedded planets even when the condensations themselves are not visible. A wobble in the position of the central star is induced by the planetary retinue which may be detected through precision astrometry. Finally, as interactions between bodies distribute debris in the disks, gaps due to planetary sweepup of material may provide additional clues as to the presence of planets. Wavelengths longer than 100 μm can offer complementary information on the character of planets and planetary systems. Here we explore some observable effects. Imaging Very Young Systems. Observations indicate that nearly all young low mass stars are born surrounded by disks of molecular gas and dust. Such disks appear to be a natural feature of" @default.
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• W3044812873 date "2009-01-01" @default.
• W3044812873 modified "2023-09-24" @default.
• W3044812873 title "Investigations of the Formation and Evolution of Planetary Systems" @default.
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