SFN

Size: px
Start display at page:

Download "SFN"

Transcription

1 THE STAR FORMATION NEWSLETTER No March /04/ X-Shooter spectroscopy of young stellar objects in Lupus. Atmospheric parameters, membership and activity diagnostics 17. The evolution of protoplanetary disks from their taxonomy in scattered light: Group I vs Group II 18. Very High Excitation Lines of H2 in the Orion Molecular Cloud Outflow 19. Dissecting the molecular structure of the Orion B: Insight from Principal Component Analysis 20. Thermochemical modelling of brown dwarf discs

2 X-Shooter spectroscopy of young stellar objects in Lupus A. Frasca et al. Accepted by A&A Determination of atmospheric parameters from X-shooter spectra of 102 YSO candidates Targets: 102 YSO candidates in Lupus I, II, III, and IV clouds pc Class II, ClassIII ( ) Atmospheric parameter Class III 102 YSO candidates (95: Class II, 7: Class III) VLT/X-shooter parameter Data sample - Telescope: VLT - Instrument: X-shooter (wide band & intermediate resolution spectrograph) - Paramaters ( nm) ( nm) ( nm)

3 Results - ROTFIT code Effective temperature (Teff), surface gravity (log g), radial velocity (RV), projected rotational velocity (v sin i) : σteff = 70 K, σlog g = 0.21 dex, σrv = 2.3 km/s, σv sin i = 4 km/s - 13/102 Lupus (by their RV, very low log g) 11 Giants (RGB AGB phase) 2 lithium-rich giants Giants? litium rich

4 Results - Teff - Hα flux Class III emission chromospheric Class II chromospheric, accretion accretion Border (by Frasca et al. 2015) Bolometric flux (FHα/σTeff 4 ) Class II White&Basri(2003) accretion Class III Transition disk chromospheric emission - Flux per unit surface accretion luminosity line-luminosity accretion luminosity calibration effect " " (emission line accretion )

5 Results - FCall1842/FCall8498 Optically thick emission source photosphere accretion shock - FHα/FHβ ~ optically thick emission Call with smaller optical depth

6 The evolution of protoplanetary disks from their taxonomy in scattered light: Group I vs. Group II A. Garufi et al. Accepted by A&A Near-IR observations of 6 Group II disks in scattered light Group I disk vs. Group II disk - MIR-FIR SED power-law fit : Group II (flat disk) - power-law : Group I (flaring disk) - Group I Group II e.g. Group I Group II - Group I Group II NIR-IR scattered light Group I disk evolution

7 Sample - 6 Group II disk - archive data 11 B-F type star (10: Group I, 1: Group II) Observation - Telescope: VLT - Instrument: AO-assisted NAOS/CONICA - Mode: Polarimetric Differential Mode Results - 3/6 - HD CO snowline ring-structure - HD (AK Sco) HD AU disk - Group I, Group II 5 AU disk cavity - Group I II

8 Conclusion - Group II Group I - Group II HD163296: Group I HD (AK Sco) HD142666: Group I

9 Very High Extinction Lines of H2 in the Orion Molecular Cloud Outflow T. R. Geballe et al. Accepted by ApJ K-band spectral observation of OMC-1 outflow Pike et al (ApJ) - Harbin-Hero 7 (HH7) bowshock K-band K ~ K H % : T = ~ 1800 K ( ) 1.5 % : T = ~ 5000 K 5000 K (Hot H2 ) OMC-1 K-band Observation - Telescope: Gemini - Instrument: GNIRS (near-infrared spectrograph)

10 Results - OMC-1 ~5000K %??

11 Dissecting the molecular structure of the Orion B cloud: Insight from Principal Component Analysis P. Gratier et al. Accepted by A&A Principal component analysis for Orion B cloud - Orion B Principal Component Analysis (PCA) Principal Component Analysis (PCA): - (PC) (wikipedia)

12 Data α ashin (x/α) (α=0.64 K)

13 Results - -

14 Results (PC1-PC3) H2, UV radiation field emission PCA

15 Thermochemical modelling of brown dwarf disks A.J. Greenwood et al. Accepted by A&A Thermochemical modelling of brown dwarf protoplanetary dies Brown dwarf protoplanetary disk - T tauri disk T tauri disk - ALMA r ~ 10 AU CO, continuum Thermodynamical model ALMA disk HCN, HCO+, CO Model - Code: ProDiMo code - ρoph CO(3-2), continuum small grid of brown dwarf model - T tauri disk Brown dwarf disk 2-D radiation thermochemical model

16 Model - SED - 12CO(3-2) - Parameter

17 Results - brown dwarf disk HCO+, HCN, CO flux ratio T tauri disk

2 X-ray 6 gamma-ray 7 1 17.1 0:38m 0:77m nm 17.2 Hz Hz 1 E p E E = h = ch= (17.2) p = E=c = h=c = h= (17.3) continuum continuous spectrum line spectru

2 X-ray 6 gamma-ray 7 1 17.1 0:38m 0:77m nm 17.2 Hz Hz 1 E p E E = h = ch= (17.2) p = E=c = h=c = h= (17.3) continuum continuous spectrum line spectru 1 17 object 1 observation 17.1 X electromagnetic wave photon 1 = c (17.1) c =3 10 8 ms ;1 m mm = 10 ;3 m m =10 ;6 m nm = 10 ;9 m 1 Hz 17.1 spectrum radio 2 infrared 3 visual light optical light 4 ultraviolet

More information

Ando_JournalClub_160708

Ando_JournalClub_160708 Independent discoveries of a tidally disrupting dwarf galaxy around NGC 253! A Tidally Disrupting Dwarf Galaxy in the Halo of NGC 253 Toloba, E. et al. 2016, ApJL, 816, L5 (hereafter T16, accepted 2015.12.07)

More information

kawaguchi2.pdf

kawaguchi2.pdf Dusty Clumpy Torus (AGN) (BH) BH 3 BH 1 AGN () 1/3 (i) (ii) Kawaguchi(2003) 1/5 (iii) AGN : T. Kawaguchi & M. Mori, ApJL, 2010, 724, 183 187 T. Kawaguchi & M. Mori, ApJ, 2011, 737, 105 120 Toshihiro KAWAGUCHI

More information

爆発的星形成? AGN関係を 生み出す物理機構の観測的示唆

爆発的星形成? AGN関係を 生み出す物理機構の観測的示唆 Umemura, Fukue & Mineshige 1997, 1998 Ohsuga et al. 1998 R ring ~100pc dv r = v 2 ϕ dt r 1 dp ρ dr dφ 1 r d(rv ϕ ) dt = 3χE 2c typical timescale dr + χ c F r 3 2 Myr r R ring V ring 3χE 2c v ϕ Umemura,

More information

NRO談話会 key

NRO談話会 key Probing the growth of IC5146 by filamentary accretion Yoshito SHIMAJIRI (CEA/Saclay) 1. 誘発的星団形成の観測的研究 2. フィラメント形成に関する観測的研究 フィラメント形成シナリオ フィラメント形成シナリオにおける問題点 Probing the mass accretion by the surrounding

More information

系外惑星大気

系外惑星大気 transiting planet http://hubblesite.org/newscenter/archive/2001/38/ 2004 6 17 HDS 2 3 (Mayor & Queloz 1995) 4.2 4 (Charbonneau et al. 2000, Henry et al. 2000) HST HST Brown et al. (2001) 5 6 Radial velocity

More information

太陽系外惑星探査

太陽系外惑星探査 http://hubblesite.org/newscenter/archive/2001/38/ Terra MODIS http://modarch.gsfc.nasa.gov/ http://www.nasa.gov/home/index.html / 2 Are we alone? Origins Where are they? (Fermi 1950) 3 4 0.5 arcsec 10pc

More information

系外惑星大気

系外惑星大気 http://hubblesite.org/newscenter/archive/2001/38/ 2004 9 30 1781 1846 1930 50 2 3 radial velocity HDS 5m/s HD209458 HD209458+I 2 cell Subaru/HDS 4 (Mayor & Queloz 1995) 4.2 5 2 1.5% HST 4 orbits Brown

More information

「産業上利用することができる発明」の審査の運用指針(案)

「産業上利用することができる発明」の審査の運用指針(案) 1 1.... 2 1.1... 2 2.... 4 2.1... 4 3.... 6 4.... 6 1 1 29 1 29 1 1 1. 2 1 1.1 (1) (2) (3) 1 (4) 2 4 1 2 2 3 4 31 12 5 7 2.2 (5) ( a ) ( b ) 1 3 2 ( c ) (6) 2. 2.1 2.1 (1) 4 ( i ) ( ii ) ( iii ) ( iv)

More information

理論懇2014

理論懇2014 Proposal for a project of high-precision stellar radial velocity work, Struve (1952)! But there seems to be no compelling reason why the hypothetical stellar planets should not, in some instances, be much

More information

( )

( ) 1. 2. 3. 4. 5. ( ) () http://www-astro.physics.ox.ac.uk/~wjs/apm_grey.gif http://antwrp.gsfc.nasa.gov/apod/ap950917.html ( ) SDSS : d 2 r i dt 2 = Gm jr ij j i rij 3 = Newton 3 0.1% 19 20 20 2 ( ) 3 3

More information

atomic line spectrum emission line absorption line atom proton neutron nuclei electron Z atomic number A mass number neutral atom ion energy

atomic line spectrum emission line absorption line atom proton neutron nuclei electron Z atomic number A mass number neutral atom ion energy 1 22 22.1 atomic line spectrum emission line absorption line atom proton neutronnuclei electron Z atomic number A mass number neutral atom ion energy level ground stateexcited state ionized state 22.2

More information

Telescope aperture 1.5mφ Telescope length Fit within the H-IIA nose fairing Spatial resolution 0.1" in UV 0.16" in Vis/NIR (Diffraction limit of 1.5mφ

Telescope aperture 1.5mφ Telescope length Fit within the H-IIA nose fairing Spatial resolution 0.1 in UV 0.16 in Vis/NIR (Diffraction limit of 1.5mφ , (NAOJ) (Kyoto U.) Telescope aperture 1.5mφ Telescope length Fit within the H-IIA nose fairing Spatial resolution 0.1" in UV 0.16" in Vis/NIR (Diffraction limit of 1.5mφ at 1µm ) FOV ~200" x 200" to cover

More information

44 4 I (1) ( ) (10 15 ) ( 17 ) ( 3 1 ) (2)

44 4 I (1) ( ) (10 15 ) ( 17 ) ( 3 1 ) (2) (1) I 44 II 45 III 47 IV 52 44 4 I (1) ( ) 1945 8 9 (10 15 ) ( 17 ) ( 3 1 ) (2) 45 II 1 (3) 511 ( 451 1 ) ( ) 365 1 2 512 1 2 365 1 2 363 2 ( ) 3 ( ) ( 451 2 ( 314 1 ) ( 339 1 4 ) 337 2 3 ) 363 (4) 46

More information

i ii i iii iv 1 3 3 10 14 17 17 18 22 23 28 29 31 36 37 39 40 43 48 59 70 75 75 77 90 95 102 107 109 110 118 125 128 130 132 134 48 43 43 51 52 61 61 64 62 124 70 58 3 10 17 29 78 82 85 102 95 109 iii

More information

PowerPoint Presentation

PowerPoint Presentation Sgr A* の赤外線観測 西山正吾 ( 京都大学 ) NIR obserbvations of the Galactic center 2/46 NIR obserbvations of the Galactic center 3/46 NIR obserbvations of the Galactic center 4/46 Dereddened flux density [mjy] 40 20

More information

untitled

untitled & SDPS team 2004219 T/Herbig AeBe HL Tau, HH30, GM Aur, HD141569, AB Aur disk-planet connection NIR/Mid-IR thermal dust (OIR interferometer, AsAst.) Domain sampled in current images at 150 pc Scattered

More information

(Blackbody Radiation) (Stefan-Boltzmann s Law) (Wien s Displacement Law)

(Blackbody Radiation) (Stefan-Boltzmann s Law) (Wien s Displacement Law) ( ) ( ) 2002.11 1 1 1.1 (Blackbody Radiation).............................. 1 1.2 (Stefan-Boltzmann s Law)................ 1 1.3 (Wien s Displacement Law)....................... 2 1.4 (Kirchhoff s Law)...........................

More information

ライトカーブ観測から何がわかるか

ライトカーブ観測から何がわかるか 2004.7.2 M 2.5log F F 10 0.4*M M F S= (abc)[sin 2 A(sin 2 ( )/a 2 +cos 2 ( )/b 2 )+cos 2 (A)/c 2 ] 1/2 a,b,c A aspect angle S M = (abc)[sin 2 (A)/b 2 +cos 2 (A)/c 2 ] 1/2 S m = (abc)[sin 2 (A)/a 2 +cos

More information

I II III IV V

I II III IV V I II III IV V N/m 2 640 980 50 200 290 440 2m 50 4m 100 100 150 200 290 390 590 150 340 4m 6m 8m 100 170 250 µ = E FRVβ β N/mm 2 N/mm 2 1.1 F c t.1 3 1 1.1 1.1 2 2 2 2 F F b F s F c F t F b F s 3 3 3

More information

1. 2. 3. 2010-02- 22-24 1.1 1.1.1 1.1.2 1.1.3 F10.7 1.2 1.2.1 1.2.2 1.2.3 14 C 1.2.4 10 Be 1.2.5 14 C 10 Be 1.1 太陽放射とその変動 20100223-24森羅万象学校 1.1.1 (from Encyclopedia of Earth) op1cal depth (Lean et al.,

More information

0.2 Button TextBox: menu tab 2

0.2 Button TextBox: menu tab 2 Specview VO 2012 2012/9/27 Specview Specview STSCI(Space Telescope SCience Institute) VO Specview Web page http://www.stsci.edu/resources/software hardware/specview http://specview.stsci.edu/javahelp/main.html

More information

ISLE 2010/08/17

ISLE 2010/08/17 ISLE 2010/08/17 Talk plan 1. ISLE 2. 3. 4. 2011A 2010/8/17 OAOUM 2010 ISLE 2010/8/17 OAOUM 2010 ISLE OASIS HAWAII (HgCdTe 1024 1024) 4.2 4.2 arcmin 2, 0.25 arcsec/pix (13 Filters) 2006B FWHM = 0.75 arcsec

More information

B

B B07557 0 0 (AGN) AGN AGN X X AGN AGN Geant4 AGN X X X (AGN) AGN AGN X AGN. AGN AGN Seyfert Seyfert Seyfert AGN 94 Carl Seyfert Seyfert Seyfert z < 0. Seyfert I II I 000 km/s 00 km/s II AGN (BLR) (NLR)

More information

総研大恒星進化概要.dvi

総研大恒星進化概要.dvi The Structure and Evolution of Stars I. Basic Equations. M r r =4πr2 ρ () P r = GM rρ. r 2 (2) r: M r : P and ρ: G: M r Lagrange r = M r 4πr 2 rho ( ) P = GM r M r 4πr. 4 (2 ) s(ρ, P ) s(ρ, P ) r L r T

More information

Specview Specview Specview STSCI(Space Telescope SCience Institute) VO Specview Web page htt

Specview Specview Specview STSCI(Space Telescope SCience Institute) VO Specview Web page   htt Specview Specview Specview STSCI(Space Telescope SCience Institute) VO Specview Web page http://www.stsci.edu/resources/software_hardware/specview http://specview.stsci.edu/javahelp/main.html Specview

More information

SFN saigo

SFN saigo 2017年10月20日 西合 SFN 296 #36 Chandra X-ray observation of the young stellar cluster NGC 3293 in the Carina Nebula Complex T. Preibisch, S. Flaischlen, B. Gaczkowski, L. Townsley and P. Broos Accepted by

More information

New version (2.15.1) of Specview is now available Dismiss Windows Specview.bat set spv= Specview set jhome= JAVA (C:\Program Files\Java\jre<version>\

New version (2.15.1) of Specview is now available Dismiss Windows Specview.bat set spv= Specview set jhome= JAVA (C:\Program Files\Java\jre<version>\ Specview VO 2012 2012/3/26 Specview Specview STSCI(Space Telescope SCience Institute) VO Specview Web page http://www.stsci.edu/resources/software hardware/specview http://specview.stsci.edu/javahelp/main.html

More information

vol5-honma (LSR: Local Standard of Rest) 2.1 LSR R 0 LSR Θ 0 (Galactic Constant) 1985 (IAU: International Astronomical Union) R 0 =8.5

vol5-honma (LSR: Local Standard of Rest) 2.1 LSR R 0 LSR Θ 0 (Galactic Constant) 1985 (IAU: International Astronomical Union) R 0 =8.5 2.2 1 2.2 2.2.1 (LSR: Local Standard of Rest) 2.1 LSR R 0 LSR Θ 0 (Galactic Constant) 1985 (IAU: International Astronomical Union) R 0 =8.5 kpc, Θ 0 = 220 km s 1. (2.1) R 0 7kpc 8kpc Θ 0 180 km s 1 270

More information

Akira MIZUTA(KEK) AM, Nagataki, Aoi (ApJ, , 2011) AM + (in prep)

Akira MIZUTA(KEK) AM, Nagataki, Aoi (ApJ, , 2011) AM + (in prep) Akira MIZUTA(KEK) AM, Nagataki, Aoi (ApJ, 732 26, 2011) AM + (in prep) 2011.12.28 GRB GRB. ex. GRB980425/SN1998bw, GRB030329/SN2003dh XRF060218/SN2006aj. GRB091127/SN2009nz XRF100316D/SN2010bh Spectrum

More information

i

i 14 i ii iii iv v vi 14 13 86 13 12 28 14 16 14 15 31 (1) 13 12 28 20 (2) (3) 2 (4) (5) 14 14 50 48 3 11 11 22 14 15 10 14 20 21 20 (1) 14 (2) 14 4 (3) (4) (5) 12 12 (6) 14 15 5 6 7 8 9 10 7

More information

42 3 u = (37) MeV/c 2 (3.4) [1] u amu m p m n [1] m H [2] m p = (4) MeV/c 2 = (13) u m n = (4) MeV/c 2 =

42 3 u = (37) MeV/c 2 (3.4) [1] u amu m p m n [1] m H [2] m p = (4) MeV/c 2 = (13) u m n = (4) MeV/c 2 = 3 3.1 3.1.1 kg m s J = kg m 2 s 2 MeV MeV [1] 1MeV=1 6 ev = 1.62 176 462 (63) 1 13 J (3.1) [1] 1MeV/c 2 =1.782 661 731 (7) 1 3 kg (3.2) c =1 MeV (atomic mass unit) 12 C u = 1 12 M(12 C) (3.3) 41 42 3 u

More information

1 2

1 2 ( ) ( ) ( ) 1 2 59 2 21 24 275 43 3 26 486 103 27 28 98 105 104 99 1 48 25 29 72 14 33 11-10 3 11 8 14,663 4 8 1 6.0 8 1 0.7 11-6 27 19 22 71 5 12 22 12 1,356 6 4,397 3 4 11 8 9 5 10 27 17 6 12 22 9

More information

Contents 1. Ia? 2. Ia 3. WISH Ia cosmology 4. WISH Ia + rate 5.

Contents 1. Ia? 2. Ia 3. WISH Ia cosmology 4. WISH Ia + rate 5. Type Ia Supernova Survey w/ WISH Contents 1. Ia? 2. Ia 3. WISH Ia cosmology 4. WISH Ia + rate 5. Contents 1. Ia? 2. Ia 3. WISH Ia cosmology 4. WISH Ia + rate 5. Type Ia Supernova + +?? (single degenerate)?

More information

スライド 1

スライド 1 2004/12/25 HOP JTPF JASMINE ILOM JAXA) SPICA JELT Yerkes 1m (1897) Palomar 5m (1948) Subaru 8m (1999) 6.5m Large Binocular Telescope(LBT) 8.4m Mt.Graham 18 3m-6m 6.5m 3m Hubble Space Telescope 2.4m (0.115

More information

α β *2 α α β β α = α 1 β = 1 β 2.2 α 0 β *3 2.3 * *2 *3 *4 (µ A ) (µ P ) (µ A > µ P ) 10 (µ A = µ P + 10) 15 (µ A = µ P +

α β *2 α α β β α = α 1 β = 1 β 2.2 α 0 β *3 2.3 * *2 *3 *4 (µ A ) (µ P ) (µ A > µ P ) 10 (µ A = µ P + 10) 15 (µ A = µ P + Armitage 1 1.1 2 t *1 α β 1.2 µ x µ 2 2 2 α β 2.1 1 α β α ( ) β *1 t t 1 α β *2 α α β β α = α 1 β = 1 β 2.2 α 0 β 1 0 0 1 1 5 2.5 *3 2.3 *4 3 3.1 1 1 1 *2 *3 *4 (µ A ) (µ P ) (µ A > µ P ) 10 (µ A = µ P

More information

第1部 一般的コメント

第1部 一般的コメント (( 2000 11 24 2003 12 31 3122 94 2332 508 26 a () () i ii iii iv (i) (ii) (i) (ii) (iii) (iv) (a) (b)(c)(d) a) / (i) (ii) (iii) (iv) 1996 7 1996 12

More information

Contents 1. Ia cosmology 2. Ia / rate 3.

Contents 1. Ia cosmology 2. Ia / rate 3. WISH ( ) Contents 1. Ia cosmology 2. Ia / rate 3. supernova (CC SN) Ia (SN Ia) supernova classification supernova Ia (SN Ia) - : redshift z~1.5 - progenitor system: Single Degenerate? Double Degenerate?

More information

1 911 9001030 9:00 A B C D E F G H I J K L M 1A0900 1B0900 1C0900 1D0900 1E0900 1F0900 1G0900 1H0900 1I0900 1J0900 1K0900 1L0900 1M0900 9:15 1A0915 1B0915 1C0915 1D0915 1E0915 1F0915 1G0915 1H0915 1I0915

More information

876 542 550 269KPa 1650 1623K 1473K SiC 170 100000 160 150 140 130 10000 120 (121%) 110 100 90 1000 0% 10% 20% 30% 40% 0% 10% 20% 30% 40% (%) (%) 850 230MPa 500 500hr. 450 1073K 800 400 350 K5C(HIP)

More information

磁性物理学 - 遷移金属化合物磁性のスピンゆらぎ理論

磁性物理学 - 遷移金属化合物磁性のスピンゆらぎ理論 email: takahash@sci.u-hyogo.ac.jp May 14, 2009 Outline 1. 2. 3. 4. 5. 6. 2 / 262 Today s Lecture: Mode-mode Coupling Theory 100 / 262 Part I Effects of Non-linear Mode-Mode Coupling Effects of Non-linear

More information

- 2 -

- 2 - - 2 - - 3 - (1) (2) (3) (1) - 4 - ~ - 5 - (2) - 6 - (1) (1) - 7 - - 8 - (i) (ii) (iii) (ii) (iii) (ii) 10 - 9 - (3) - 10 - (3) - 11 - - 12 - (1) - 13 - - 14 - (2) - 15 - - 16 - (3) - 17 - - 18 - (4) -

More information

2 1980 8 4 4 4 4 4 3 4 2 4 4 2 4 6 0 0 6 4 2 4 1 2 2 1 4 4 4 2 3 3 3 4 3 4 4 4 4 2 5 5 2 4 4 4 0 3 3 0 9 10 10 9 1 1

2 1980 8 4 4 4 4 4 3 4 2 4 4 2 4 6 0 0 6 4 2 4 1 2 2 1 4 4 4 2 3 3 3 4 3 4 4 4 4 2 5 5 2 4 4 4 0 3 3 0 9 10 10 9 1 1 1 1979 6 24 3 4 4 4 4 3 4 4 2 3 4 4 6 0 0 6 2 4 4 4 3 0 0 3 3 3 4 3 2 4 3? 4 3 4 3 4 4 4 4 3 3 4 4 4 4 2 1 1 2 15 4 4 15 0 1 2 1980 8 4 4 4 4 4 3 4 2 4 4 2 4 6 0 0 6 4 2 4 1 2 2 1 4 4 4 2 3 3 3 4 3 4 4

More information

20 15 14.6 15.3 14.9 15.7 16.0 15.7 13.4 14.5 13.7 14.2 10 10 13 16 19 22 1 70,000 60,000 50,000 40,000 30,000 20,000 10,000 0 2,500 59,862 56,384 2,000 42,662 44,211 40,639 37,323 1,500 33,408 34,472

More information

I? 3 1 3 1.1?................................. 3 1.2?............................... 3 1.3!................................... 3 2 4 2.1........................................ 4 2.2.......................................

More information

1 (1) (2)

1 (1) (2) 1 2 (1) (2) (3) 3-78 - 1 (1) (2) - 79 - i) ii) iii) (3) (4) (5) (6) - 80 - (7) (8) (9) (10) 2 (1) (2) (3) (4) i) - 81 - ii) (a) (b) 3 (1) (2) - 82 - - 83 - - 84 - - 85 - - 86 - (1) (2) (3) (4) (5) (6)

More information

第1章 国民年金における無年金

第1章 国民年金における無年金 1 2 3 4 ILO ILO 5 i ii 6 7 8 9 10 ( ) 3 2 ( ) 3 2 2 2 11 20 60 12 1 2 3 4 5 6 7 8 9 10 11 12 13 13 14 15 16 17 14 15 8 16 2003 1 17 18 iii 19 iv 20 21 22 23 24 25 ,,, 26 27 28 29 30 (1) (2) (3) 31 1 20

More information

Contents 1 Jeans (

Contents 1 Jeans ( Contents 1 Jeans 2 1.1....................................... 2 1.2................................. 2 1.3............................... 3 2 3 2.1 ( )................................ 4 2.2 WKB........................

More information

(2010 Sep April) Titan s global crater population: A new assessment Neish & Lorenz, PSS in-press Distant secondary craters from Lyot crater, Mar

(2010 Sep April) Titan s global crater population: A new assessment Neish & Lorenz, PSS in-press Distant secondary craters from Lyot crater, Mar 2011.5.12 D1 1 (2010 Sep.-2011 April) Titan s global crater population: A new assessment Neish & Lorenz, PSS in-press Distant secondary craters from Lyot crater, Mars, and implications for surface ages

More information

表1票4.qx4

表1票4.qx4 iii iv v 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 22 23 10 11 24 25 26 27 10 56 28 11 29 30 12 13 14 15 16 17 18 19 2010 2111 22 23 2412 2513 14 31 17 32 18 33 19 34 20 35 21 36 24 37 25 38 2614

More information

1. : 1.5 2. ( ): 2.5 3. : 1 ( ) / minimum solar nebula model ( ) http://antwrp.gsfc.nasa.gov/apod/ap950917.html ( ) http://www-astro.physics.ox.ac.uk/~wjs/apm_grey.gif ( ) SDSS : d 2 r i dt 2 ÿ j i

More information

スケーリング理論とはなにか? - --尺度を変えて見えること--

スケーリング理論とはなにか?  - --尺度を変えて見えること-- ? URL: http://maildbs.c.u-tokyo.ac.jp/ fukushima mailto:hukusima@phys.c.u-tokyo.ac.jp DEX-SMI @ 2006 12 17 ( ) What is scaling theory? DEX-SMI 1 / 40 Outline Outline 1 2 3 4 ( ) What is scaling theory?

More information

V懇_2017.key

V懇_2017.key z > 4 Radio-loud 2 Z. -Q. Shen VLBI 2017 @ J1427+3312; z = 6.1 160 pc Frey et al. 2008 Figure 1. VLBI images at 1.6 GHz of three very high-redshift q left), J1427+3312 (z = 6.12, middle), and J1429+5447

More information

SuperMassive Black Holes

SuperMassive Black Holes Hello! Galaxy Morphology, Galaxies Near and Far SuperMassive Black Holes and all that Ajit Kembhavi IUCAA, Pune Galaxy Morphology, Galaxies Near and Far SuperMassive Black Holes and all that Ajit Kembhavi

More information

ΤΕΙ Ιονίων Νήσων - Εργαστηριακές Ασκήσεις στα Γεωγραφικά Συστήματα Πληροφοριών

ΤΕΙ Ιονίων Νήσων - Εργαστηριακές Ασκήσεις στα Γεωγραφικά Συστήματα Πληροφοριών 1 71 71 71 71 71 71 71 71 71 71 73 1 71 7 1 71 71 71 71 71 71 71 7):1 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 7-1 71 71 71 71 71 71 71 71 71 71 71 71 71

More information

yasi10.dvi

yasi10.dvi 2002 50 2 259 278 c 2002 1 2 2002 2 14 2002 6 17 73 PML 1. 1997 1998 Swiss Re 2001 Canabarro et al. 1998 2001 1 : 651 0073 1 5 1 IHD 3 2 110 0015 3 3 3 260 50 2 2002, 2. 1 1 2 10 1 1. 261 1. 3. 3.1 2 1

More information

Microsoft PowerPoint _nakagawa_kagoshima.ppt [互換モード]

Microsoft PowerPoint _nakagawa_kagoshima.ppt [互換モード] Mira 型変光星プロジェクト現状とKVN の利用 A.Nakagawa, T.Kurayama (Kagoshima University) Mira Project Observation Current Status KVN + VERA 大マゼラン雲 (LMC) のミラ型変光星周期光度関係 実視等級を元に得られた関係 距離に対してLMCの厚みは小さくすべて同じ距離にあるとみなせるため実視等級を利用できる

More information

hν 688 358 979 309 308.123 Hz α α α α α α No.37 に示す Ti Sa レーザーで実現 術移転も成功し 図 9 に示すよ うに 2 時間は連続測定が可能な システムを実現した Advanced S o l i d S t a t e L a s e r s 2016, JTu2A.26 1-3. 今後は光周波 数比計測装置としてさらに改良 を加えていくとともに

More information

(ASIAA)

(ASIAA) 2016.11.07 (ASIAA) Dogs.. Introduction Dust Obscured Galaxies IR-bright DOGs Introduction Dust Obscured Galaxies i - [22] > 7.0 (AB mag) (Toba, Nagao et al. 2015) This study IR-bright DOGs HSC+WISE (Final

More information

1 Kinect for Windows M = [X Y Z] T M = [X Y Z ] T f (u,v) w 3.2 [11] [7] u = f X +u Z 0 δ u (X,Y,Z ) (5) v = f Y Z +v 0 δ v (X,Y,Z ) (6) w = Z +

1 Kinect for Windows M = [X Y Z] T M = [X Y Z ] T f (u,v) w 3.2 [11] [7] u = f X +u Z 0 δ u (X,Y,Z ) (5) v = f Y Z +v 0 δ v (X,Y,Z ) (6) w = Z + 3 3D 1,a) 1 1 Kinect (X, Y) 3D 3D 1. 2010 Microsoft Kinect for Windows SDK( (Kinect) SDK ) 3D [1], [2] [3] [4] [5] [10] 30fps [10] 3 Kinect 3 Kinect Kinect for Windows SDK 3 Microsoft 3 Kinect for Windows

More information

provider_020524_2.PDF

provider_020524_2.PDF 1 1 1 2 2 3 (1) 3 (2) 4 (3) 6 7 7 (1) 8 (2) 21 26 27 27 27 28 31 32 32 36 1 1 2 2 (1) 3 3 4 45 (2) 6 7 5 (3) 6 7 8 (1) ii iii iv 8 * 9 10 11 9 12 10 13 14 15 11 16 17 12 13 18 19 20 (2) 14 21 22 23 24

More information

untitled

untitled masato@icrr.u-tokyo.ac.jp 996 Start 997 998 999 000 00 00 003 004 005 006 007 008 SK-I Accident Partial Reconstruction SK-II Full reconstruction ( SK-III ( ),46 (40%) 5,8 (9%),9 (40%) 5MeV 7MeV 4MeV(plan)

More information

The Physics of Atmospheres CAPTER :

The Physics of Atmospheres CAPTER : The Physics of Atmospheres CAPTER 4 1 4 2 41 : 2 42 14 43 17 44 25 45 27 46 3 47 31 48 32 49 34 41 35 411 36 maintex 23/11/28 The Physics of Atmospheres CAPTER 4 2 4 41 : 2 1 σ 2 (21) (22) k I = I exp(

More information

H22 BioS t (i) treat1 treat2 data d1; input patno treat1 treat2; cards; ; run; 1 (i) treat = 1 treat =

H22 BioS t (i) treat1 treat2 data d1; input patno treat1 treat2; cards; ; run; 1 (i) treat = 1 treat = H BioS t (i) treat treat data d; input patno treat treat; cards; 3 8 7 4 8 8 5 5 6 3 ; run; (i) treat treat data d; input group patno period treat y; label group patno period ; cards; 3 8 3 7 4 8 4 8 5

More information

* n x 11,, x 1n N(µ 1, σ 2 ) x 21,, x 2n N(µ 2, σ 2 ) H 0 µ 1 = µ 2 (= µ ) H 1 µ 1 µ 2 H 0, H 1 *2 σ 2 σ 2 0, σ 2 1 *1 *2 H 0 H

* n x 11,, x 1n N(µ 1, σ 2 ) x 21,, x 2n N(µ 2, σ 2 ) H 0 µ 1 = µ 2 (= µ ) H 1 µ 1 µ 2 H 0, H 1 *2 σ 2 σ 2 0, σ 2 1 *1 *2 H 0 H 1 1 1.1 *1 1. 1.3.1 n x 11,, x 1n Nµ 1, σ x 1,, x n Nµ, σ H 0 µ 1 = µ = µ H 1 µ 1 µ H 0, H 1 * σ σ 0, σ 1 *1 * H 0 H 0, H 1 H 1 1 H 0 µ, σ 0 H 1 µ 1, µ, σ 1 L 0 µ, σ x L 1 µ 1, µ, σ x x H 0 L 0 µ, σ 0

More information

The faint young Sun paradox Early Mars ( Ga) on Mars wet and warm climate? Valley networks(carr, 1996) The warm climate cannot be sustained (Ka

The faint young Sun paradox Early Mars ( Ga) on Mars wet and warm climate? Valley networks(carr, 1996) The warm climate cannot be sustained (Ka Warming of early Mars induced by CO 2 ice clouds Kobe University, the 21st century COE program Microsymposium, Climate and Meteorology on Mars Friday, June 17, 2005 Chihiro Mitsuda (Hokkaido Univ.) Tokuta

More information

Microsoft PowerPoint - TMTinst_ _summerschool_akiyama

Microsoft PowerPoint - TMTinst_ _summerschool_akiyama 1 2 3 4 5 6 7 8 9 10 590nm 2200nm 0 1.739 1.713 5 1.708 1.682 10 1.678 1.652 0-10 0.061061 0.061061 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 1.0 x1.0 0.5 x0.5 0.2 x0.2 0.1 x0.1 bg/30ms

More information

i ii iii iv v vi vii ( ー ー ) ( ) ( ) ( ) ( ) ー ( ) ( ) ー ー ( ) ( ) ( ) ( ) ( ) 13 202 24122783 3622316 (1) (2) (3) (4) 2483 (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) 11 11 2483 13

More information

untitled

untitled World topography Most earthquakes occur in subduction zones Trench-Arc-Backarc system Landward side Seaward side Back- Fore- (Widiyantoro et al., 1999 EPSL) Seismicity cross section across Japan trench

More information

J. Jpn. Inst. Light Met. 65(6): 224-228 (2015)

J. Jpn. Inst. Light Met. 65(6): 224-228 (2015) 65 62015 224 228 ** Journal of The Japan Institute of Light Metals, Vol. 65, No. 6 (2015), 224 228 2015 The Japan Institute of Light Metals Investigation of heat flow behavior on die-casting core pin with

More information

2 (March 13, 2010) N Λ a = i,j=1 x i ( d (a) i,j x j ), Λ h = N i,j=1 x i ( d (h) i,j x j ) B a B h B a = N i,j=1 ν i d (a) i,j, B h = x j N i,j=1 ν i

2 (March 13, 2010) N Λ a = i,j=1 x i ( d (a) i,j x j ), Λ h = N i,j=1 x i ( d (h) i,j x j ) B a B h B a = N i,j=1 ν i d (a) i,j, B h = x j N i,j=1 ν i 1. A. M. Turing [18] 60 Turing A. Gierer H. Meinhardt [1] : (GM) ) a t = D a a xx µa + ρ (c a2 h + ρ 0 (0 < x < l, t > 0) h t = D h h xx νh + c ρ a 2 (0 < x < l, t > 0) a x = h x = 0 (x = 0, l) a = a(x,

More information

Spacecraft Propulsion Using Solar Energy Spacecraft with Magnetic Field Light from the Sun Solar Wind Thrust Mirror Solar Sail Thrust production by li

Spacecraft Propulsion Using Solar Energy Spacecraft with Magnetic Field Light from the Sun Solar Wind Thrust Mirror Solar Sail Thrust production by li 2004.3.28 物理学会シンポジウム 磁気プラズマセイル の可能性と 深宇宙探査への挑戦 宇宙航空研究開発機構 船木一幸 Spacecraft Propulsion Using Solar Energy Spacecraft with Magnetic Field Light from the Sun Solar Wind Thrust Mirror Solar Sail Thrust production

More information

untitled

untitled SPring-8 RFgun JASRI/SPring-8 6..7 Contents.. 3.. 5. 6. 7. 8. . 3 cavity γ E A = er 3 πε γ vb r B = v E c r c A B A ( ) F = e E + v B A A A A B dp e( v B+ E) = = m d dt dt ( γ v) dv e ( ) dt v B E v E

More information

Influence of Material and Thickness of the Specimen to Stress Separation of an Infrared Stress Image Kenji MACHIDA The thickness dependency of the temperature image obtained by an infrared thermography

More information

untitled

untitled 1 2 3 4 5 130mm 32mm UV-irradiation UV-cationic cure UV-cationic cure UV-cationic cure Thermal cationic Reaction heat cure Thermal cationic Cation Reaction heat cure Cation (a) UV-curing of

More information

untitled

untitled 27.2.9 TOF-SIMS SIMS TOF-SIMS SIMS Mass Spectrometer ABCDE + ABC+ DE + Primary Ions: 1 12 ions/cm 2 Molecular Fragmentation Region ABCDE ABCDE 1 15 atoms/cm 2 Molecular Desorption Region Why TOF-SIMS?

More information

4 19

4 19 I / 19 8 1 4 19 : : f(e, J), f(e) Phase mixing Landau Damping, violent relaxation : 2 2 : ( ) http://antwrp.gsfc.nasa.gov/apod/ap950917.html ( ) http://www-astro.physics.ox.ac.uk/~wjs/apm_grey.gif

More information

178 5 I 1 ( ) ( ) 10 3 13 3 1 8891 8 3023 6317 ( 10 1914 7152 ) 16 5 1 ( ) 6 13 3 13 3 8575 3896 8 1715 779 6 (1) 2 7 4 ( 2 ) 13 11 26 12 21 14 11 21

178 5 I 1 ( ) ( ) 10 3 13 3 1 8891 8 3023 6317 ( 10 1914 7152 ) 16 5 1 ( ) 6 13 3 13 3 8575 3896 8 1715 779 6 (1) 2 7 4 ( 2 ) 13 11 26 12 21 14 11 21 I 178 II 180 III ( ) 181 IV 183 V 185 VI 186 178 5 I 1 ( ) ( ) 10 3 13 3 1 8891 8 3023 6317 ( 10 1914 7152 ) 16 5 1 ( ) 6 13 3 13 3 8575 3896 8 1715 779 6 (1) 2 7 4 ( 2 ) 13 11 26 12 21 14 11 21 4 10 (

More information

chap1_MDpotentials.ppt

chap1_MDpotentials.ppt simplest Morse : simplest (1 Well-chosen functional form is more useful than elaborate fitting strategies!! Phys. Rev. 34, 57 (1929 ( 2 E ij = D e 1" exp("#(r ij " r e 2 r ij = r i " r j r ij =r e E ij

More information

mt_4.dvi

mt_4.dvi ( ) 2006 1 PI 1 1 1.1................................. 1 1.2................................... 1 2 2 2.1...................................... 2 2.1.1.......................... 2 2.1.2..............................

More information

The Phase Behavior of Monooleoylglycerol-Water Systems Mivoshi Oil & Fat Co.. Ltd. Faculty of Science and Technology, Science University of Tokyo Inst

The Phase Behavior of Monooleoylglycerol-Water Systems Mivoshi Oil & Fat Co.. Ltd. Faculty of Science and Technology, Science University of Tokyo Inst The Phase Behavior of Monooleoylglycerol-Water Systems Mivoshi Oil & Fat Co.. Ltd. Faculty of Science and Technology, Science University of Tokyo Institute of Colloid and Interface Science, Science University

More information

75 unit: mm Fig. Structure of model three-phase stacked transformer cores (a) Alternate-lap joint (b) Step-lap joint 3 4)

75 unit: mm Fig. Structure of model three-phase stacked transformer cores (a) Alternate-lap joint (b) Step-lap joint 3 4) 3 * 35 (3), 7 Analysis of Local Magnetic Properties and Acoustic Noise in Three-Phase Stacked Transformer Core Model Masayoshi Ishida Kenichi Sadahiro Seiji Okabe 3.7 T 5 Hz..4 3 Synopsis: Methods of local

More information

dy = sin cos y cos () y () 1 y = sin 1 + c 1 e sin (3) y() () y() y( 0 ) = y 0 y 1 1. (1) d (1) y = f(, y) (4) i y y i+1 y i+1 = y( i + ) = y i

dy = sin cos y cos () y () 1 y = sin 1 + c 1 e sin (3) y() () y() y( 0 ) = y 0 y 1 1. (1) d (1) y = f(, y) (4) i y y i+1 y i+1 = y( i + ) = y i 007 8 8 4 1 1.1 ( ) (partial differential equation) (ordinary differential equation) 1 dy = f(, y) (1) 1 1 y() (1) y() (, y) 1 dy = sin cos y cos () y () 1 y = sin 1 + c 1 e sin (3) 1 1 5 y() () y() y(

More information

プラズマ核融合学会誌11月【81‐11】/小特集5

プラズマ核融合学会誌11月【81‐11】/小特集5 Japan Atomic Energy Agency, Ibaraki 311-0193, Japan 1) Kyoto University, Uji 611-0011, Japan 2) National Institute of Advanced Industrial Science and Technology, Tsukuba 305-8569, Japan 3) Central Research

More information