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The Star Formation Newsletter 311
43~51

Bo (,;u,1/NAOJ)

43

A Lagrangian Model for Dust Evolution in Protoplanetary Disks: Formation ofWet and Dry Planetesimals at Different Stellar Masses

44

NU Ori: a hierarchical triple system with a strongly magnetic B-type star

45

Rings and gaps in protoplanetary disks: planets or snowlines?

46

The magnetic fields of intermediate-mass T Tauri stars : I. Magnetic detections
and fundamental stellar parameters

47

How do disks and planetary systems in high-mass open clusters differ from thosearound field stars?

48Physical and Chemical Conditions of the Protostellar Envelope and theProtoplanetary Disk in HL Tau

49

NGC 1893: a young open cluster rich in multi-type variable stars

50

Diffusion and Concentration of Solids in the Dead Zone of a Protoplanetary Disk

51

Planck Cold Clumps in the λ Orionis Complex. II. Environmental Effects on CoreFormation

45 (1)}U:- ALMAÁÏÑ .HTwqÃêæî/ÝæÃÞúëõ«¨Ä²Ì·=>HT%¾¦§«VÍWĆĆ(e.g., Isella+16 for HD163296)- COÃÞúëõ«¨·ªÐ¾º¼HT0'ÃNÁÄÀÐÀ¦(COÃ×ñāêāæÎe<Á0³Ò·Ì)XO½º·¯¾/Ôªº·¯¾:
im-1v½COÃradial 8À¿ÕÇ·- HT¥Ñ½ÍS½¬Ò, HTÀ±ÃêæîLùíþ½ÍS½¬Ò=> 1 Myr Ã9¡Ã- ½gap«ÓÒ¯¾ÕS½¬Ò
¶±¼¤HD163296½ËÐÓ·CO gapÄHTgª¿§ªÔªÐÀ¦\±·=<õĀóÖÙþ

HD163296
12CO13COC18O
ya
Isella + 16ÏÑ=>ÞúëõÄ&TÃHT½S½¬Ò

45 (2)

M`: DALI code (Bruderer+12;13)=> .HTwqªÐÃLine flux ÕI³Òcode
- êæîÃ5, /×ñāêāæ, /ÃÀ¿Õ- ¨Òùíþ: Ýæ/êæî[4<, TÃ5)q^Ãùíþ: HD163296 (Isella+16)Õr Ò- Model A (“gap model”)AÃflsÄ2(0.85)
Þúëõ(r1,r2,r3)½êæîÃ[4<Õ0.01, 0.014, 0.17
ÝæÃ[4<Õ0.4, 0.29, 0.56
- Model B (“snowline model ”),¬ÀêæîÃ#(fls)ÕêæîÃÞúëõ½0.01 ¾±·, Ä0.99

Fig.1 êæîya(230 GHz)Ã8, ùíþ¾f=> ¿¹ÐÃùíþÍfÕl³Ò

­

45 (3)

Fig.2 COÃ=<8Ã@8ùíþÄÞúëõ(h{)Ã |½=<«*±¼¦ÒÞúëõÃ |½¤ÝæÃe<«R±¤=<Õ*°µÒ=> fÄ¶§Àº¼¦À¦Ê¾ÌÒ¾¤ÞúëõÃCOÃd7ÕHTÃN¾³ÒÁÄbJ«Ef¾±¼ÄCOÃ ¦ ~/K<Ãíăé«E

48 (1)
HL-tauÃSMAfą13CO, C18O, SO, 1.3 mm , ALMAf: HCO+ ¶Ó¾IRAM 30mjC- âāòßîÀÚøëäûā: ~0.”8 x 0.”5 æáăþ => áõüădisk (>3km/s)- :«º·L: ~6.”5 x 4.”3 =>infalling envelope ( <Á¦Ò)Y- HCO+Ã <LÕáõüădisk½óØëî=>1.4 MoÃDT- 13CO, C18OÃ=<õĀóÖÙþÕáõüă+ÚāöĀăõùíþ½fit=>diskÃÝæ: 2-40 x 10-4 Mo, ÚāöĀăõÃÝæ: 2.9 x 10-3 Mo- Disk Ãdust ; 1-3 x 10-3 Mo (OkÏÑ)=> gas-to-dust ratio <10, ÚāöĀăõÏÑÍ106°¦
Ýæ or CO depletion Ã"~GÕ³Ò

48 (2)¯Ó¸®ALMA ¥¾SMA

Fig. 1,2
yaÃ÷ëõ¾
/{Ã÷ëõ13CO, C18OÄÚāöĀăõÕîÿăæHCO+ÄoutflowÃQ$ÁÍ Æ¼¦ÒHCO+½áõüăfit (model º¼) => DT=1.4 MoSOÄêæîpeakªÐ´Ó¼©Ñ¤]Âredshift <=outflowªÐÃ3ªĆ

48 (3)SPARX¾¦§âăïÕº¼
13CO, C18OÃùíþÕLDisk ÃÝæ/êæîÕv
gas-to-dust_«6°¦- Ýæ¶Ó ÃZc«%½ÄÀ­¤COdepletion« %ªĆ

51 (1)ĂJCMT/SCUBA-2Õn¦·ÛýÛā(Ã/â×Ãst40ÃPGCC (Planck Galactic Cold Clump)TdβR

N(H2)

n(H2)

Mcore

λ Orionis

16 K

1.7

0.08 pc

9.5e22 cm-2

2.9e5 cm-3

1.0 Mo15

Orion A

14 K

2.1

0.11 pc

2.3e23 cm-2

3.5e5 cm-3

2.4 Mo74

Orion B

14 K

2.0

0.16 pc

3.8e23 cm-2

15.6e5 cm-3

2.7 Mo30ÜéĀà(PlanckãăöÙ)x
λ Orionis½ÄðÝìØôóØăïñëß«¦¼¦ÒThese core properties in the λ Orionis cloud can be attributed to thephotodissociation and external heating by the nearby H II region, which may
prevent the PGCCs from forming gravitationally bound structures andeventually disperse them. These results support the idea of negative stellar
feedback on core formation.

λ OriÃ/â×

51 (2)λ Ori

R: Planck 353 GHz
G: IRAS 100μm
B: HαContour:Planck 857 GHz£:PGCC (850μm ¥ÑĄ¢: PGCC (850μm À±)
~380 pc
/z~1.4 x 104 Moâāî×: 850μm
Back ground : WISE 12 μm¦ºÅ¦f±·Ï§Á¨¼P±­!º·íăéÄÈÉ¯Ó¸®
(OrionA,BÄ×ăÜÙô«D)

51 (3)λ OriðÝìØôóØăïñëß«¦¼¦Ò¾Fº¼¦Òmp£: Orion B£: Orion A£: λ Oriâ×Ã«åăāç
ÏÑÍ6°¦

DªÐ+Á$ª§Á»Ó¼e<« ­Àº¼¦Ò(,TªÐÃ?)À¿