LEADER 03814nam 22005415 450 001 996418450403316 005 20200901141047.0 010 $a981-15-7439-1 024 7 $a10.1007/978-981-15-7439-9 035 $a(CKB)4100000011413964 035 $a(DE-He213)978-981-15-7439-9 035 $a(MiAaPQ)EBC6331577 035 $a(PPN)250221543 035 $a(EXLCZ)994100000011413964 100 $a20200901d2020 u| 0 101 0 $aeng 135 $aurnn|008mamaa 181 $ctxt$2rdacontent 182 $cc$2rdamedia 183 $acr$2rdacarrier 200 10$aWater Snowline in Protoplanetary Disks$b[electronic resource] /$fby Shota Notsu 205 $a1st ed. 2020. 210 1$aSingapore :$cSpringer Singapore :$cImprint: Springer,$d2020. 215 $a1 online resource (XIII, 134 p. 53 illus., 51 illus. in color.) 225 1 $aSpringer Theses, Recognizing Outstanding Ph.D. Research,$x2190-5053 311 $a981-15-7438-3 327 $aIntroduction -- Modeling Studies I. The Case of the T Tauri Star -- Modeling studies II. The Case of the Herbig Ae Star -- Modeling Studies III. Sub-millimeter H216O and H218O Lines -- ALMA Observation of the Protoplanetary Disk around HD 163296 -- Summary and Future Works. 330 $aThis book presents pioneering work on a critical observational test of the planet formation theory based on the theoretical study of the water snowline, beyond which water takes the form of ice, in the protoplanetary disks ? the place where planets are formed. Since the water snowline is thought to divide the regions of rocky and gas-giant planet formation, the location of the snowline is essential for the planet formation process. The book proposes a novel method to locate the snowlines using high-dispersion spectroscopic observations of water vapor lines, which is based on in sophisticated chemical modeling and line radiative transfer calculations. The author obtained the water vapor distribution in the disks using the chemical reaction network, which includes photoreactions and gas?grain interactions. The simulated transition lines of water vapor in the disks demonstrate that relatively weak transition lines with moderate excitation energies are the best tracers of water snowline. Furthermore, the author observed submillimeter lines of water vapor in a disk using ALMA (Atacama Large Millimeter/submillimeter Array) to obtain the upper limit of the line fluxes with the highest sensitivity to date. These unprecedented findings are important in locating the snowlines in the disks, and the method goes a long way toward achieving a comprehensive understanding of the planet formation processes as well as of the origin of water on rocky planets, including our Earth, based on future observations using ALMA and SPICA (Space Infrared Telescope for Cosmology and Astrophysics). 410 0$aSpringer Theses, Recognizing Outstanding Ph.D. Research,$x2190-5053 606 $aObservations, Astronomical 606 $aAstronomy?Observations 606 $aPlanetary science 606 $aAstronomy, Observations and Techniques$3https://scigraph.springernature.com/ontologies/product-market-codes/P22014 606 $aPlanetary Sciences$3https://scigraph.springernature.com/ontologies/product-market-codes/P22060 615 0$aObservations, Astronomical. 615 0$aAstronomy?Observations. 615 0$aPlanetary science. 615 14$aAstronomy, Observations and Techniques. 615 24$aPlanetary Sciences. 676 $a520 700 $aNotsu$b Shota$4aut$4http://id.loc.gov/vocabulary/relators/aut$0932867 801 0$bMiAaPQ 801 1$bMiAaPQ 801 2$bMiAaPQ 906 $aBOOK 912 $a996418450403316 996 $aWater Snowline in Protoplanetary Disks$92099672 997 $aUNISA