Star Formation Newsletter No. 367 #49-65

花輪 知幸 (千葉大)fiflfi49. Effect of Dust Evaporation and Thermal Instability on Temperature Distribution in a Protoplanetary Disk,Pavlyuchenkov et al. Astronomy Reports, 67, 470
50. Chemical clocks and their time zones: understanding the [s/Mg]--age relation with birth radii, Ratcliffe et al.
MN
51. Survival of fossil elds during the pre-main sequence evolution of intermediate-mass stars, Schleicher et al.
A&Ap
52. The high-quality single-cloud reddening curve sample Dark Dust III: Scrutinizing extinction curves in theMilky Way, Siebenmogen et al.
53. Gaia21bty: An EXor lightcurve exhibiting an FUor spectrum, MN
54. Early Planet Formation in Embedded Disks (eDisk) V: Possible Annular Substructure in a Circumstellar Disk in
the Ced110 IRS4 System, Sai et al. ApJ
55. How large is a disk - what do protoplanetary disk gas sizes really mean? Trapman et al. ApJ
56. The GAPS program at TNG XLVII: The unusual formation history of V1298 Tau. Turrini et al. A&Ap
57. Do all gaps in protoplanetary discs host planets? Tzouvanou et al. A&Ap
58. Flow of gas detected from beyond the laments to protostellar scales in Barnard 5, Valdivia-Mena et al. A&Ap
59. Rocky sub-Neptunes formed by pebble accretion: Rain of rock from polluted envelopes, Vazan & Ormel,
A&Ap, 676, L8
60. Direct images and spectroscopy of a giant protoplanet driving spiral arms in MWC 758 , Wagner et al. NatureAstronomy
61. ALMA and VLBA views on the out ow associated with an O-type protostar in G26.50+0.28, Wu et al. A&Ap
62. PLANETESIMAL ACCRETION AT SHORT ORBITAL PERIODS, Wallace & Quinn, ApJ
63. Spirals and Clumps in V960 Mon: Signs of Planet Formation via Gravitational Instability around an FU Ori
Star? Weber et al. ApJ, 952, L17
64. Early Planet Formation in Embedded Disks (eDisk). IV. The Ringed and Warped Structure of the Disk aroundthe Class I Protostar L1489 IRS, Yamato et al. ApJ, 951, 11
65. Submillimeter Observations of Magnetic Fields in Massive Star-forming Region W75N, Zeng et al. ApJ

64. Early Planet Formation in Embedded Disks (eDisk). IV. The Ringed and Warped
Structure of the Disk around the Class I Protostar L1489 IRS, Yamato et al. ApJ, 954, 11

Mdisk = 8.9M
<latexit sha1_base64="Sm+qLwR7+T7iCq2G/fu8lmf9+nE=">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</latexit>

i = 71°
Fig. 11.3mm0.1” 分解能d = 146 pc

Far side: south

Fig. 213CO 2-1
C18O 2-1,SO 65-54

Fig. 313CO 2-1
C18O 2-1,SO 65-54

Fig. 7 C18O

Fig. 8Fig. 10
他に 12CO, DCN, H2CO, c-C3H2を検出
SiO, CH3OHは未検出

54 Early Planet Formation in Embedded Disks (eDisk) V: Possible Annular Substructure
in a Circumstellar Disk in the Ced110 IRS4 System, Sai et al. ApJ, 954, 67
Fig. 1. 1.3 mm continuum, 0.05” (d =189pc)

Fig. 2 IRS4A

Fig. 3 IRS4B

2つのモデル
・点源と2つのガウス型
南側が少し明るい

Tpeak = 79 K
<latexit sha1_base64="lcI3SfWPPfK3UPT0+xJWVi/Jycs=">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</latexit>

Tpeak = 9 K<latexit sha1_base64="HTH4qFynmmvdkev/IcUU+t/+TU4=">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</latexit>

Fig. 8リング
モデルの重ね合わせ
・点源とガウス型とリングの重ね合せFig. 4. C18O

Fig. 7SO

13CO, 12CO は C18Oと類似だが光学的に厚いFig. 11 rotation curve. IRS4A

60 Direct images and spectroscopy of a giant protoplanet driving spiral arms in MWC 758
Wagner et al. Nature Astronomy, July 2023
MWC 758 (d=156 pc, age=3.5±2 Myr, SpT=A8Ve)

Large Binocular
Telescope Interferometer
8-14 μm, 3-5 μm<latexit sha1_base64="doALIncX6PO/4qcrLGlFSzZtNFI=">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</latexit>

theory: Mcompanion
Dong+18 ALMA. 0.87 mm

MJupこの星の近くには
MWC 758a 0.11”
MWC 758b. 幻
MWC 758 CCI. Background61. ALMA and VLBA views on the out ow associated with an O-type protostar in G26.50+0.28,
Wu et al. A&Apfl

G26.50+0.28 (also known as IRAS 18360-0537), d = 6.3 + 0.5 - 0.4 kph

63. Spirals and Clumps in V960 Mon: Signs of Planet Formation via Gravitational
Instability around an FU Ori Star? Weber et al. ApJL, 952, L17V960 Mon. 2014年からOutburst.

Kospal+21d = 2189±281 pc

65 Submillimeter Observations of Magnetic
Fields in Massive Star-forming Region W75N,Zeng et al. ApJ

SMA. 345 GHz

52 The high-quality single-cloud reddening curve
sample Dark Dust III: Scrutinizing extinction
curves in the Milky Way.

49. Effect of Dust Evaporation and Thermal Instability on Temperature Distribution in a
Protoplanetary Disk, Pavlyuchenkov et al. Astronomy Reports

59. Rocky sub-Neptunes formed by pebble accretion: Rain of rock from polluted envelopes, Vazan et al. A&ApPebble accretion で形成された惑星にはSi蒸気が含まれている。時刻が経過し、温度が下がるとSiが固化して中心へ落下する。この時に解放されるエネルギーにより、惑星は一時的に膨らむはず。

53. Gaia21bty: An EXor lightcurve exhibiting an FUor spectrum
EXor の光度変化に FUor のスペクトル

Gaia Alert で見つかった