ALMA Science Highlights 2018 Low-mass Star Formation and - PowerPoint PPT Presentation

1 ALMA Science Highlights 2018 Low-mass Star Formation and Protoplanetry Disk Kazuya Saigo (NAOJ) Dec. 26 2018 ALMA/45m/ASTE Users Meeting 2018

2 DSHARP Protoplanetary Disks The ALMA Large Program in Cycle 4 Disk Substructures at High Angular Resolution Project High resolution (~0.035” or 5au) survey 240 GHz (1.25 mm) continuum 12 CO J =2-1 line emission from 20 nearby, bright, and large PP disks. Almost all PP disks have substructures. DSHARP I: Andrews, S. M et al. 2018arXiv181204040 II: Huang, J. et al. 2018arXiv181204041 III: Huang, J. et al. 2018 arXiv:1812.04143 IV: Kurtovic N. et al. arXiv:1812.04536 V: Birnstiel, T. et al. 2018arXiv181204043 VI: Dullemond, C. P . et al. 2018arXiv181204044 VII: Zhang, S. al. 2018arXiv181204045 VIII:Guzmán, V. V. et al. 2018arXiv181204046 IX: Isella, A. et al. 2018arXiv181204047 X: Pérez, L. M. et al. 2018arXiv181204049

3 DSHARP Protoplanetary Disks Formation models of such substructures 1. Dust trapping in radial pressure bumps Dullemond et al. (2018 paper VI ) find all ring structures are consistent with dust trapping model. 2. Gravitational interaction with planets Zhang et al. (2018 paper VII ) reproduced the observed ring of AS 209 by single planet model. 2D Simulation Single Planet + low viscosity 3. Opacity gap by snowlines of major volatiles Some of the gaps roughly coincide with the location of snowlines of major volatiles. But this model contradicts diversity? 4. Gravitational Instability Formation mechanism is an open question.

4 Asymmetries structure in PP Disks Asymmetric structures are shaped by the gravitational interaction with unseen planets? PP Disk around MWC 758 PP Disk around HD 163296 off-centered cavity+ 2 clumps + rings + arms Ring + asymmetric structure Isella et al. 2018 arXiv181204047 Dong 2018 ApJ, 860, 124 ( DSHARP IX) Mayama et al. (2018) ： misaligned PP disk around J16042165-2130284 Pérez, L. M. et al. 2018 arXiv181204049: misaligned PP disk around HD143006 ect.

5 Kinematic Evidence for Embedded Protoplanets I Pinte et al. 2018 ApJL, 860, L13P ~15% deviation from Keplerian rotation in the PP disk around HD 163296. Perturbation by ~ 2 M Jup mass proto-planet at R ~ 260 au ?

6 Kinematic Evidence for Embedded Protoplanets II Teague et al. 2018 ApJL, 860L, L12T Azimuthally averaged velocity structure indicates the embedded three ptoto-planets in the PP disk around HD 163296. Deviation from Keplerian rotation model (3 proto-planets ) C 18 O(2-1)

7 Sub-structures in Protostellar Disk Protostellar disks in the main acretion phase also have sub-structures. Class I protostar WL 17 Class I protostar GY 91 ALMA 3mm Sheehan and Eisner 2017; 2018

8 Discovery of Jupter Mass protostar Protostar IRAS 15398–3359 ALMA observation of very young objects M * <~0.2M 8 Low Luminosity? or no IR emission Embedded in the cloud core 0.007M 8 Yen et al. 2018 88 young objects in Lupus Yoko Oya et al. 2018 L483 Tokuda et al. 2018 MC27/L1521F Tien-Hao Hsieh et al. 2018 IRAS 16253-2429(protobrown dwarf?) Aso et al. 2018 Very young protostars in Serpens Main Kawabe et al. 2018 Oph. Sorce A/Source X , , Offset position (arcsec) Okoda et al. 2018 ApJL, 864, L25

9 Dust size diagnosis by Polarization Stephens et al. 2017 Dust grain size Bacciotti et al 2018 HL Tau: 100μm (Stephens et al. 2017) DG Tau: 100μm (Bacciotti et al 2018) CW Tau: 50-70μm (Bacciotti et al 2018) HD142527 Southern Region: <100μm Northern Region: >150μm (Ohashi et al. 2018) (see Kataoka et al. 2016a, 2016b, 2017)

10 Magnetic Structure in Protostellar envelopes Class 0 Protostar B335 proto-binary L1448 IRS2 Kwon et al. 2018 Maury et al. 2018 Polarization observation toward protostars Sadavoy et al. (2018) Class 1 Protobinary IRAS16293-2422 Harris et al. (2018) Class 0 Protobinary VLA1623, Class 1 Protostar L1527 Alves et al. (2018) Class 0 Protobinary BHB07-11 Cox et al. 2018 10 protostars Perseus Molecular Cloud

Protostellar Jet: 11 Kinematic and Magnetic and Structures Protostellar outflow/jet HH211 Line Polarization (SiO) Very High Resolution Image 0.03 arcsec resolution ( ∼ 7au) Line polarization is attributed to the Goldreich- Kylafis effect in the presence of magnetic field. toroidal fields? If this polarization vector is perpendicular to the magnetic field * It depends on physical condition. Revised 2018 12/26 Lee Chin-Fei et al. 2018, Lee Chin-Fei et al. 2018 ApJ, 865, 9 Nature Communications

Protostellar Jet: 12 Kinematic and Magnetic and Structures Protostellar outflow/jet HH211 Line Polarization (SiO) Very High Resolution Image 0.03 arcsec resolution ( ∼ 7au) Line polarization is attributed to the Goldreich- Kylafis effect in the presence of magnetic field. toroidal fields? ↑ If this polarization vector is perpendicular to the magnetic field. (Note that it depends on physical condition.) Revised 2018 12/26 Lee Chin-Fei et al. 2018, Lee Chin-Fei et al. 2018 ApJ, 865, 9 Nature Communications

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Discovery of shock heated filaments 14 in the low mass protstellar core MC27/L1521F 12CO (2-1) Shock Heated Filament (width <~a few x 10au, T>~60K) Decay process ? turbulence or internal motions Δv ~ a few km/s => sub-sonic? Tokuda et al. 2018