星形成セミナー#374 1-14

⼤橋聡史（国⽴天⽂台）

••••••••••••••A Unified Model for Bipolar Outflows from Young Stars: Kinematic and Mixing Structures in HH 30
Evolution of the relation between the mass accretion rate and the stellar and disk mass from brown dwarfs to stars
JWST MIRI MRS Images Disk Winds, Water, and CO in an Edge-On Protoplanetary Disk
An ALMA molecular inventory of warm Herbig Ae disks: I. Molecular rings, asymmetries and complexity in theHD 100546 disk
An ALMA molecular inventory of warm Herbig Ae disks: II. Abundant complex organics and volatile sulphur in
the IRS 48 disk
JWST observations of 13CO2 ice: Tracing the chemical environment and thermal history of ices in protostellar
envelopes
The dynamical evolution of star-forming regions measured with INDICATE
Deep Paβ Imaging of the Candidate Accreting Protoplanet AB Aur b
ALMA-IMF XI: The sample of hot core candidates A rich population of young highmass proto-stars unveiled by
the emission of methyl formate
Protoplanet collisions: new scaling laws from SPH simulations
Thermal processing of primordial pebbles in evolving protoplanetary disks
FAUST XII. Accretion streamers and jets in the VLA 1623–2417 protocluster
An Automated Chemical Exploration of NGC 6334I at 340 au Resolution
The 3D structure of disc-instability protoplanets

JWST MIRIでoutflowの観測• H2 outflowが200 auまで広がっていて,opening angleは35°(MHD windと⼀致)• [Ne II], [Ne III], [Ni II], [Fe II], [Ar II], and[S III]はjetを観測• H2O and COはr ~ 90 -190 auで検出、inner diskの散乱によるもの• PAH 11.3 umは散乱光と⼀致（T-Tauriで初)円盤の寿命やaccretion、質量損失に制限がつけられるかもCycle 1 GO program “Mapping Inclined
Disk Astrochemical Signatures (MIDAS).”

CO: T = 1500 K, logN = 17.5 cm-2
H2O: T = 850 K, logN = 15.0 cm-2

Assuming the H2 emission is optically thin, the wind
contains a gas mass of MH2 ~ 5.4 × 10−7M⊙, corresponding toa mass flux of ~ 6.5 × 10−9 M⊙ yr−1.
The Huα emission was used to estimate a mass accretion
rate of Macc = 2 × 10−11 M⊙ yr−1, although we
note that this is likely an underestimate due to scatteringand extinction along the line-of-sight and uncertainties
in the size of the line emitting region

Herbig Ae transition disks are fruitful targets due to the thermal sublimation of complex organic
molecule (COM) and likely H2O-rich ices in these disks.
the first robust detections of H132CO, 34SO, 33SO and c−H2COCH2 (ethylene oxide)
there are spatial offsets between different molecular families, including between the COMs and sulphurbearing species, with the latter being more azimuthally extended and radially located further from the star.

The abundances of the newly detected COMs relative to CH3OH are higher than the expected
protostellar ratios, which implies some degree of chemical processing of the inherited ices during the disklifetime

IRS 48の⽅がchemically richでCOMsやSが豊富
Dust trapが関係しているかもIRS 48HD 100546

CO以外はdustとcospatial (HCO+やHCNなどのシンプル分⼦も）、CS & CCHはnon-detection

(ただし、HD 100546の⽅がmassiveでwarm)• H2COとHCO+はdust peakでdepressしてる• CH3OHとSO/SO2は若⼲半径が異なる• SOとSO2はH2O & H2Sのsublimationとphotodissociatationだと思っていたが違うかも(CH3OHとH2Oは⼀致）• 乱流が関係しているかも？？
••••••COMsやS系分⼦が豊富なのはH2OやCOMs-rich iceのsublimation
O系分⼦やCOMsは特に低いHCO+はlower X-ray or gas phase H2O(destroyer of HCO+)
CNやCCHの未検出はC/O<1を⽰唆
Nの⼀番のcariierはNOH2CS(H2COのS系）が未検出。 H2CSとCSが似た分布を他円盤で⽰すので<100 Kでもガス中で形成を⽰唆

S系分⼦について
In IRS 48 SO, SO2 and CS are detected but OCS and H2CS are not
In IRS 48 SO is the most abundant S-bearing volatile detected with peak column density
ratios of SO2/SO of ≈ 26%, CS/SO of ≈ 0.2%, OCS/SO of < 0.3% and, H2CS/SO of < 1.0%.

コメットや原始星との⽐較
SO2, OCS and H2CS are all lower in abundance relative to SO in this disk

円盤でのS系分⼦の組成は原始星や彗星(67P)とは⼤きく異なる。
⼀つのアイディアは、Sがuv照射によってよりrefractoryな物質に変化（硫⻩同素体）

OCS + S ! S2 + CO<latexit sha1_base64="FJVdHfPMVzsG9p/l5hBxkHMzr34=">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</latexit>

S2がダストから脱離するとOと反応して気相でSOやSO2が⽣成できる

UV radiationによる円盤での化学進化が重要？

JWST NIRSpec data of the 4.39 μm asymmetricstretching mode of 13CO2 ice for five protostars

合計で5成分のガウス関数でfittingできる

contributions from cold H2O-rich andCH3OH-rich polar ices, cold CO-rich apolarices, and warm pure CO2 ice at 80 K