TPF-I SWG Report - Exoplanet Exploration Program - NASA

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C HAPTER 3 clouds or an OB association – anywhere in the Universe, enabling the detailed investigation of the cosmic evolution of galactic structure. 3.2 Transformational Astrophysics We highlight four research areas where <strong>TPF</strong>-I/Darwin will make revolutionary advances, namely: • Star and planet formation and early evolution. • Stellar and planetary death and cosmic recycling. • The formation, evolution, and growth of black holes. • Galaxy formation and evolution over cosmic time. 3.2.1 Star and Planet Formation and Early Evolution Darwin/<strong>TPF</strong>-I will have a resolution of 1 AU at a distance of 500 pc, the distance to the Orion massive star-forming region. In the nearest regions of low-mass star formation (~125 to 150 pc), 0.25 AU structures will be resolved. Stars are the fundamental building blocks of the baryonic Universe. Short-lived massive stars and clusters are responsible for the nucleosynthesis of elements heavier than helium, for the ultraviolet (UV) radiation that re-ionized the Universe at the end of the cosmic Dark Ages, and for regulating the physical and chemical state of the interstellar media (ISM) of galaxies. Their powerful stellar winds and terminal supernova explosions dominate the generation of random motions in the ISM. Long-lived low-mass stars provide the stable environment needed for the formation of planetary systems and the evolution of life. Figure 3-1. Schematic of the circumstellar environment of an isolated young star. 42
G ENERAL A STROPHYSICS Figure 3-2. HST image of the giant galactic nebula NGC 3603 shows the various stages of the life cycles of stars in one single view, from a starburst cluster of young hot Wolf-Rayet stars and early O-type stars (center) to the evolved blue supergiant Sher 25 (upper right), which marks the end of the life cycle. Star formation is the process that determines the mass-spectrum (initial mass function —IMF; Kroupa 2000) of stars. Star formation determines how galaxies consume their interstellar media and how they convert this material into long-lived low-mass stars, and star formation controls the rate and nature of galactic evolution. In the standard model of star formation (Figure 3-1), the inside-out gravitational collapse of a rotating cloud core leads to the formation of a protostellar core on a time-scale of about 10 4 years. The infall of high-angular-momentum gas forms a spinning, circumstellar disk through which most of the star’s final mass spirals onto the protostar on a time-scale of ~10 5 years. Entrained and dynamo-generated magnetic fields launch powerful jets and bipolar outflows along the rotation axis of the system for a period of order 10 5 to 10 6 years (Reipurth and Bally 2001). Planetary systems form and mature from remnants of the disk in about 10 6 to 10 8 years; low-mass stars reach the main-sequence (MS) in 10 7 to > 10 8 years (see the Grenoble stellar evolutionary tracks, Siess, Dofour, and Forestini 2000). During the last decade, observations have shown that most stars form in highly over-dense, but shortlived clusters that form from the collapsing and fragmenting cores of turbulent molecular clouds (MacLow and Klessen 2004). Furthermore, the birth and early evolution of most stars occurs in the close proximity of luminous, massive stars that irradiate the birth environments with intense UV radiation and which explode as supernovae on time-scales ranging from 3 to 40 Myr, the same time-scale on which 43
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JPL Publication 07-1 Terrestrial Pl
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Abstract Over the past two years, t
Page 7 and 8: Acknowledgements Twenty-two represe
Page 9 and 10: Table of Contents 1 Introduction...
Page 11 and 12: 4.8.3 Post-Nulling Calibration.....
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Page 19 and 20: I NTRODUCTION Standard Interferomet
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Page 28 and 29: C HAPTER 2 Classical interferometry
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Page 54 and 55: C HAPTER 3 3.1.1 Darwin/TPF-I Prope
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Page 60 and 61: C HAPTER 3 the circumstellar disk,
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Page 64 and 65: C HAPTER 3 Continuum interferometry
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Page 68 and 69: C HAPTER 3 3.3 Conclusions Darwin/T
Page 70 and 71: C HAPTER 3 Nguyen, H. T., Kallivaya
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D ESIGN AND A R C H I T E C T U R E
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C HAPTER 5 Heavy launch vehicle. Th
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C HAPTER 5 5.3.2 Combiner Spacecraf
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C HAPTER 5 5.3.5 Beam Transfer betw
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C HAPTER 5 Figure 5-8. Control sche
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C HAPTER 5 Figure 5-9. First sectio
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C HAPTER 5 Figure 5-9 shows the fir
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C HAPTER 5 5.4.4 Shear Metrology Sh
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C HAPTER 5 Figure 5-15. TPF-I Fligh
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C HAPTER 5 secondary mirror along t
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C HAPTER 5 a) c) b) d) IWA = 43 mas
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C HAPTER 5 planets found. Figure 5-
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C HAPTER 5 30 25 5 M earth 3 M eart
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C HAPTER 5 5.8.4 Angular Resolution
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C HAPTER 5 Table 5-3. Angular Resol
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C HAPTER 5 The optimization works b
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T E C H N O L O G Y R OADMAP FOR TP
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F UTURE D EVELOPMENTS 7 Preparatory
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F UTURE D EVELOPMENTS • To comple
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F UTURE D EVELOPMENTS Table 7-1. Pr
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D ISCUSSION AND C ONCLUSION 8 Discu
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Appendices 167
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T E C H N O L O G Y A DVISORY C O M
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F L I G H T S YSTEM C ONFIGURATION
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F L I G H T S YSTEM C ONFIGURATION
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A PPENDIX C 2. Identical FACS fligh
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A PPENDIX C 2. Recall that the coef
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A PPENDIX C Once the formation has
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A PPENDIX C Figure C-3. Example of
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A PPENDIX C Figure C-4. FAST Flight
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A PPENDIX C The “true” time of
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A PPENDIX C References Cohen, S., a
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A PPENDIX D DC DCB DM DM DOCS DOD D
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A PPENDIX D NaCl NAR NASA NASTRAN N
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A PPENDIX E Appendix E TPF-I Review
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A PPENDIX F Alice Quillen, Universi
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A PPENDIX F Figure 3-1 - Original f
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TPF-I SWG Report - Exoplanet Exploration Program - NASA

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