1. On the Number of Stars in the Sun‘s Birth Cluster, by Sota Arakawa, Eiichiro Kokubo
The Sun is thought to be formed within a star cluster. The coexistence of 26Al-rich and 26Al-poor calcium--aluminum-rich inclusions indicates that a
direct injection of 26Al-rich materials from a nearby core-collapse supernova should occur in the first 105 years of the solar system. Therefore, at least
one core-collapse supernova should occur within the duration of star formation in the Sun's birth cluster. Here we revisit the number of stars in the Sun'sbirth cluster from the point of view of the probability for acquiring at least one core-collapse supernova within the finite duration of star formation in thebirth cluster. We find that the number of stars in the birth cluster can be significantly larger than that previously considered, depending on the durationof star formation. (A&A 670, A105 (2023))

2. The physical and chemical processes in protoplanetary disks: constraints on thecomposition of comets, by Yuri Aikawa, Satoshi Okuzumi, Klaus Pontoppidan
We review the recent observations of protoplanetary disks together with relevant theoretical studies with an emphasis on the evolution of volatiles. In
the last several years Atacama Large Millimeter/submillimeter Array (ALMA) provided evidence of grain growth, gas-dust decoupling, and substructures such as rings and gaps in the dust continuum. Molecular line observations revealed radial and vertical distributions of molecular abundances
and also provided significant constraints on the gas dynamics such as turbulence. While sub-millimeter and millimeter observations mainly probe thegas and dust outside the radius of several au, ice and inner warm gas are investigated at shorter wavelengths. Gas and dust dynamics are key toconnecting these observational findings. One of the emerging trends is inhomogeneous distributions of elemental abundances, most probably due todust-gas decoupling. (COMETS III, in press.)

3. Dust processing in protoplanetary envelopes as the origin of hot minerals in comets, by
Mohamad Ali-Dib
Crystalline silicates are found in a large number of comets. These pose a long-standing conundrum for solar system formation models as they can only
be created in the inner hot disk at temperatures higher than 800 K, and there is no obvious mechanism to transport them out into the comets formation
region. Here we propose that these particles could have formed inside the hydrostatic envelopes surrounding young protoplanets still embedded in the
protoplanetary disk. Using a simplified 1D model we investigate the thermal structure of these envelopes, and find that for core masses ranging from0.08 to 1.5 M_Earth, located anywhere between 1 and 30 AU, the temperature and pressure at the base of the envelopes are high enough to quickly
vaporize silicate particles of various sizes. Moreover, if the grain abundance is at least solar, these envelopes become fully convective, allowing for dust
ejection across the Bondi radius back into the disk. Amorphous silicates are hence thermally processed into crystalline particles in these envelopes, andthen transported back to disk through convective diffusion to be finally incorporated into the cometary building blocks. (MNRAS in press)

4. Lyman-alpha Scattering Models Trace Accretion and Outflow Kinematics in T Tauri Systems,by Nicole Arulanantham et al.
T Tauri stars produce broad Lyman-alpha emission lines that contribute ∼88% of the total UV flux incident on the inner circumstellar disks. Lyman-alphaphotons are generated at the accretion shocks and in the protostellar chromospheres and must travel through accretion flows, winds and jets, theprotoplanetary disks, and the interstellar medium before reaching the observer. This trajectory produces asymmetric, double-peaked features that carrykinematic and opacity signatures of the disk environments. To understand the link between the evolution of Lyman-alpha emission lines and the disks
themselves, we model HST-COS spectra from targets included in Data Release 3 of the Hubble UV Legacy Library of Young Stars as Essential Standards(ULLYSES) program. We find that resonant scattering in a simple spherical expanding shell is able to reproduce the high velocity emission line wings,
providing estimates of the average velocities within the bulk intervening H I. The model velocities are significantly correlated with the K band veiling,
indicating a turnover from Lyman-alpha profiles absorbed by outflowing winds to emission lines suppressed by accretion flows as the hot inner disk isdepleted. Just 30% of targets in our sample have profiles with red-shifted absorption from accretion flows, many of which have resolved dust gaps. At thisstage, Lyman-alpha photons may no longer intersect with disk winds along the path to the observer. Our results point to a significant evolution of
Lyman-alpha irradiation within the gas disks over time, which may lead to chemical differences that are observable with ALMA and JWST. (ApJ in press)

5. Unbound stars hold the key to young star cluster history, by Arunima Arunima, SusannePfalzner, Amith Govind
Aims. GAIA delivers the positions and velocities of stars at unprecedented precision. Therefore, for star clusters, there exists much higher confidence inwhether a specific star is a member of a particular group. However, membership determination is still challenging for young star clusters. At ages 2-10Myr, the gas is expelled, leading to cluster expansion, while many former members become unbound. We aim to assess the accuracy of the methods
used to distinguish between bound and unbound cluster members. After identifying the most suitable technique, we wish to understand which of the two
populations provides more insights into the initial configuration and the dynamic history of a cluster. Methods. Here, we perform N-body simulations of
the dynamics of such young star clusters. We investigate how cluster dynamics and observational limitations affect the recovered information about thecluster from a theoretical perspective. Results. We find that the much-used method of distance and velocity cutoffs for membership determination often
leads to false negatives and positives alike. Often observational studies focus on the stars remaining bound. However, they quickly lose the memory of
the pre-gas expulsion phase due to interactions with other cluster members. Our study shows that the unbound stars hold the key to charting a cluster's
dynamic history. Backtracking unbound stars can provide the original cluster size and determine the time of gas expulsion. This information is lost in thebound population. In addition, former members are often better indicators for disc lifetimes or initial binary fractions. We apply the backtracking analysis,
with varying success, to the clusters: Upper Scorpius and NGC 6530. For highly substructured clusters such as Upper Scorpius, backtracking to theindividual subcluster centres will provide better results in the future (abridged). (AAp in press)

6. Millimetre and sub-millimetre spectroscopy of doubly deuterated acetaldehyde (CHD2CHO) andfirst detection towards IRAS 16293-2422, by J. Ferrer Asensio et al.
The abundances of deuterated molecules with respect to their main isotopologue counterparts have been determined to be orders of magnitude higher
than expected from the cosmic abundance of deuterium relative to hydrogen. The increasing number of singly and multi-deuterated species detections
helps us to constrain the interplay between gas-phase and solid-state chemistry and to understand better deuterium fractionation in the early stages ofstar formation. Acetaldehyde is one of the most abundant complex organic molecules (COMs) in star-forming regions and its singly deuterated
isotopologues have already been observed towards protostars. A spectroscopic catalogue for astrophysical purposes is built for doubly deuterated
acetaldehyde CHD2CHO from measurements in the laboratory. Submillimetre wave transitions were measured for the non-rigid doubly deuterated
acetaldehyde CHD2CHO displaying hindered internal rotation of its asymmetrical CHD2 methyl group. A line position analysis is carried out allowing us
to reproduce 853 transition frequencies with a weighted root mean square standard deviation of 1.7, varying 40 spectroscopic constants. A
spectroscopic catalogue for astrophysical purposes is built from the analysis results. Using this catalogue we were able to detect for the first timeCHD2CHO towards the low-mass protostellar system IRAS 16293-2422 utilizing data from the ALMA Protostellar Interferometric Line Survey. The firstdetection of the CHD2CHO species allows for the derivation of its column density with a value of 1.3x10^15 cm^-2 and an uncertainty of 10-20%. The
resulting D2/D ratio of ~20% is found to be coincident with D2/D ratios derived for other complex organic molecules towards IRAS~16293-2422,
pointing at a common formation environment with enhanced deuterium fractionation. (A&A 670, A177 (2023))

7. Chemical modeling of Orion Nebula Cluster disks: evidence for massive, compact gas diskswith ISM-like gas-to-dust ratios, by Ryan D. Boyden, Josh A. Eisner
The stellar cluster environment is expected to play a central role in the evolution of circumstellar disks. We use thermochemical modeling to constrain the
dust and gas masses, disk sizes, UV and X-ray radiation fields, viewing geometries, and central stellar masses of 20 Class II disks in the Orion Nebula
Cluster (ONC). We fit a large grid of disk models to 350 GHz continuum, CO J=3−2, and HCO+ J=4−3 ALMA observations of each target, and we introduce a
procedure for modeling interferometric observations of gas disks detected in absorption against a bright molecular cloud background. We find that the ONC
disks are massive and compact, with typical radii <100 AU, gas masses ≥10−3 M⊙, and gas-to-dust ratios ≥100. The ISM-like gas-to-dust ratios derived fromour modeling suggest that compact, externally-irradiated disks in the ONC are less prone to gas-phase CO depletion than the massive and extended gas
disks that are commonly found in nearby low-mass star-forming regions. The presence of massive gas disks indicates that external photoevaporation may
have only recently begun operating in the ONC, though it remains unclear whether other cluster members are older and more evaporated than the ones inour sample. Finally, we compare our dynamically-derived stellar masses with the stellar masses predicted from evolutionary models and find excellent
agreement. Our study has significantly increased the number of dynamical mass measurements in the mass range ≤0.5 M⊙, demonstrating that the ONC is
an ideal region for obtaining large samples of dynamical mass measurements towards low-mass M-dwarfs. (ApJ in press)

8. Orbital Migration of Protoplanets in a Marginally Gravitationally Unstable Disk. II. Migration,
Merging, and Ejection, by Alan P. Boss
Protoplanets formed in a marginally gravitationally unstable (MGU) disk by either core accretion or disk instability will be subject to dynamicalinteractions with massive spiral arms, possibly resulting in inward or outward orbital migration, mergers with each other, or even outright ejection fromthe protoplanetary system. The latter process has been hypothesized as a possible formation scenario for the unexpectedly high frequency of unboundgas giant exoplanets (free floating planets, FFP). Previous calculations with the EDTONS fixed grid three dimensional (3D) hydrodynamics code found that
protoplanets with masses from 0.01 M⊕ to 3 MJup could undergo chaotic orbital evolutions in MGU disks for ∼ 1000 yrs without undergoing monotonic
inward or outward migration. Here the Enzo 2.5 adaptive mesh refinement (AMR) 3D hydrodynamics code is used to follow the formation and orbital
evolution of protoplanets in MGU disks for up to 2000 yrs. The Enzo results confirm the basic disk fragmentation results of the EDTONS code, as well as
the absence of monotonic inward or outward orbital migration. In addition, Enzo allows protoplanet mergers to occur, unlike EDTONS, resulting in asignificant decrease in the number of protoplanets that survive for 1000 to 2000 yrs in the Enzo models. These models also imply that gas giants shouldbe ejected frequently in MGU disks that fragment into large numbers of protoplanets, supporting ejection as a possible source mechanism for theobserved FFPs.

9. Herbig Stars: A Quarter Century of Progress, by Sean D. Brittain et al.
Herbig Ae/Be stars are young contracting stars on the radiative track in the HR diagram on their way to the main sequence. These stars provide a
valuable link between high and low mass stars. Here we review the progress that has been made in our understanding of these fascinating objects andtheir disks since the last major review on this topic published in 1998. We begin with a general overview of these stars and their properties. We thendiscuss the accretion of circumstellar material onto these stars. Next we discuss the dust and gas properties of the circumstellar disk before exploring
the evidence for planet formation in these disks. We conclude with a brief discussion of future prospects for deepening our understanding of thesesources and propose a new working definition of Herbig Ae/Be stars. (to be published in Space Science Reviews)

10. Longterm Stability of Planetary Systems formed from a Transitional Disk, by Rory Bowens et al.
Transitional disks are protoplanetary disks with large and deep central holes in the gas, possibly carved by young planets. Dong, R., & Dawson, R. 2016, ApJ,
825, 7 simulated systems with multiple giant planets that were capable of carving and maintaining such gaps during the disk stage. Here we continue theirsimulations by evolving the systems for 10 Gyr after disk dissipation and compare the resulting system architecture to observed giant planet properties,
such as their orbital eccentricities and resonances. We find that the simulated systems contain a disproportionately large number of circular orbits comparedto observed giant exoplanets. Large eccentricities are generated in simulated systems that go unstable, but too few of our systems go unstable, likely due toour demand that they remain stable during the gas disk stage to maintain cavities. We also explore whether transitional disk inspired initial conditions canaccount for the observed younger ages of 2:1 resonant systems orbiting mature host stars. Many simulated planet pairs lock into a 2:1 resonance during thegas disk stage, but those that are disrupted tend to be disrupted early, within the first 10 Myr. Our results suggest that systems of giant planets capable ofcarving and maintaining transitional disks are not the direct predecessors of observed giant planets, either because the transitional disk cavities have a
different origin or another process is involved, such as convergent migration that pack planets close together at the end of the transitional disk stage.

11. The evolution of phase space densities in star-forming regions, by George A. Blaylock-Squibbs& Richard J. Parker
The multi-dimensional phase space density (both position and velocity) of star-forming regions may encode information on the initial conditions of starand planet formation. Recently, a new metric based on the Mahalanobis distance has been used to show that hot Jupiters are more likely to be foundaround exoplanet host-stars in high 6D phase space density, suggesting a more dynamic formation environment for these planets. However, later work
showed that this initial result may be due to a bias in the age of hot Jupiters and the kinematics of their host stars. We test the ability of the Mahalanobis
distance and density to differentiate more generally between star-forming regions with different morphologies by applying it to static regions that areeither substructured or smooth and centrally concentrated. We find that the Mahalanobis distance is unable to distinguish between different
morphologies, and that the initial conditions of the N-body simulations cannot be constrained using only the Mahalanobis distance or density.
Furthermore, we find that the more dimensions in the phase space the less effective the Mahalanobis density is at distinguishing between different initialconditions. We show that a combination of the mean three-dimensional (x, y, z) Mahalanobis density and the Q-parameter for a region can constrain its
initial virial state. However this is due to the discriminatory power of the Q-parameter and not from any extra information imprinted in the Mahalanobis
density. We therefore recommend continued use of multiple diagnostics for determining the initial conditions of star-forming regions, rather thanrelying on a single multi-dimensional metric.

12. SOFIA and ALMA Investigate Magnetic Fields and Gas Structures in Massive Star Formation:
The Case of the Masquerading Monster in BYF 73, by Peter J. Barnes et al.
We present SOFIA+ALMA continuum and spectral-line polarisation data on the massive molecular cloud BYF 73, revealing important details about themagnetic field morphology, gas structures, and energetics in this unusual massive star formation laboratory. The 154μm HAWC+ polarisation map
finds a highly organised magnetic field in the densest, inner 0.55×0.40 pc portion of the cloud, compared to an unremarkable morphology in thecloud's outer layers. The 3mm continuum ALMA polarisation data reveal several more structures in the inner domain, including a pc-long, ∼500
M⊙ "Streamer" around the central massive protostellar object MIR 2, with magnetic fields mostly parallel to the east-west Streamer but oriented
north-south across MIR 2. The magnetic field orientation changes from mostly parallel to the column density structures to mostly perpendicular, atthresholds Ncrit = 6.6×1026 m −2, ncrit = 2.5×1011 m −3, and Bcrit = 42±7 nT. ALMA also mapped Goldreich-Kylafis polarisation in 12CO across the cloud,which traces in both total intensity and polarised flux, a powerful bipolar outflow from MIR 2 that interacts strongly with the Streamer. The magnetic
field is also strongly aligned along the outflow direction; energetically, it may dominate the outflow near MIR 2, comprising rare evidence for amagnetocentrifugal origin to such outflows. A portion of the Streamer may be in Keplerian rotation around MIR 2, implying a gravitating mass
1350±50 M⊙ for the protostar+disk+envelope; alternatively, these kinematics can be explained by gas in free fall towards a 950±35 M⊙ object. The
high accretion rate onto MIR 2 apparently occurs through the Streamer/disk, and could account for ∼33% of MIR 2's total luminosity via gravitationalenergy release. (ApJ in press)星形成の初期条件
星団の姿に残っているか？質量分離、内部構造(substructure)による⽐較、

Mahalanobis distance<latexit sha1_base64="C40gclYS7S92KsQ7F4DNvbhGZBU=">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</latexit>

à例-- auto-correlation, two-point correlation function
à degree of subsctructure
e.g., breaks in the two-point correlation function
corresponded to the Jeans length (Simon 1997)

Mahalanobis distance：特定の配位ｘが平均とどれくらい離れているかを測る-- minimum spanning tree (MST)

ここで、μは、-- Q-parameter (Cartwright & Whitworth 04)µ~ = (x̄1 , x̄2 , x̄3 , . . . , x̄N )(x, y, z)<latexit sha1_base64="bUcO3tKm22nZB65ezxFRVbzpBDs=">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</latexit>(x, y, z, vx , vy , vz )

ß分散の多次元版<latexit sha1_base64="RvRuHQ+b2vROgogIWX8ZFJeRwcg=">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</latexit>

Sは共分散⾏列、S-1はその逆⾏列。

-- ΛMSR (Allison+09)

vx<latexit sha1_base64="geIl+DGs1/xCnUlaKGoevwsKEUk=">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</latexit>

これらは、基本、空間３次元分布に関する⽅法論、
Gaia等が提供する⾼空間解像度の６Dデータによる⽅法
Mahalanobis density ß Mahalanobis distance (Mahalanobis 1936)-- 速度と距離（次元の違うものを⽐較）-- これは⼩惑星衝突クレーターの分類、太陽⿊点の分類に使われた。
-- Winter+ 20
host stars in high phase space densities are more likely to have hot
Jupiter planets (M > 50 ME and a < 0.2 au)
N体計算-- Kira integrator (Starlab package)-- 1000 体、10Myr
3 Df-- box-fractal generator +-- fractal dimension Df=1.6 / 3.0-- α=T/|Ω| = 0.1 (subvirialàboundクラスター); 0.9 (supervirialà膨張)-- IMF
Maschberger 2013 IMF

Mahalanobis density：
配位xと配位yの間の距離をMahalanobis
distanceを使って定義、

md,3<latexit sha1_base64="KVYXq3jiyC+QtCrjqTaw70grwiA=">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</latexit>~x でのMahalanobis density<latexit sha1_base64="nVKF1afJkEJuFIgC3iAKR5YpCto=">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</latexit>

Dp： 位相空間の次元
m: xからN番⽬に近い配位へのMahalanobis
distance。
N: 番⽬の数 （この論⽂ではN=20）<latexit sha1_base64="jGghL+zGnunpSzBv7sQM8MuP3kk=">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</latexit>

V (L) / L

Local surface density ratio ΣLDR (Maschberger& Clarke 2011)

11. The evolution of phase spacedensities in star-forming regions,by George A. Blaylock-Squibbs &Richard J. Parker

x<latexit sha1_base64="lzavRyTx6YiUBZjKmvEbs33vSd0=">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</latexit>

Mahalanobis distanceのcluster の星での平均の100realizationでの平均

the discriminatory power of the Q-parameter (Cartwright & Whitworth 2004)<latexit sha1_base64="O4AuZFRy33EA10IhaZ9v0PbQaFs=">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</latexit>

初期分布

Q=

これでは形態、分布を峻別できない。

m̄s̄<latexit sha1_base64="iO40eYCdzuYJ1wj+SNSn1dQGtQc=">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</latexit>m̄は、minimum spanning tree の平均腕の⻑さを(Ntotal A)1/2 /(Ntotal<latexit sha1_base64="gB6d2gP31ZXIHzJVf7BTyJZX/uA=">AAACanichVHLSgMxFD0dX7W+at0o3RRrxVVJxReuRDcutbWtoCIzY9TQeTGTFmrxB9y5EuxKQUT8DDf+gIt+guiughsX3k4HRIt6Q5KTk3tuThLNMYQnGWuElK7unt6+cH9kYHBoeCQ6Git4dtnVeV63Ddvd1lSPG8LieSmkwbcdl6umZvCiVlpr7Rcr3PWEbW3JqsP3TPXIEodCVyVRxV1NdWvm6X40ydLMj0QnyAQgiSA27OgtdnEAGzrKMMFhQRI2oMKjtoMMGBzi9lAjziUk/H2OU0RIW6YsThkqsSUaj2i1E7AWrVs1PV+t0ykGdZeUCaTYE7tjTfbI7tkz+/i1Vs2v0fJSpVlra7mzP3I2nnv/V2XSLHH8pfrTs8Qhlnyvgrw7PtO6hd7WV04umrnlbKo2za7ZC/m/Yg32QDewKm/6zSbP1hGhD8j8fO5OUJhNZxbS85tzyZXV4CvCiGMSM/Tei1jBOjaQ992d4xL10KsSUyaUeDtVCQWaMXwLZeoT3pOMvA==</latexit>s̄ は、星の間隔の平均を、星団の半径で規格化。
<latexit sha1_base64="F4EWKaOJf+RdzXxRSyW8bZ7m6iE=">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</latexit>n/r ↵<latexit sha1_base64="dFDWUhaQUppcYSedVc2jTLQELiE=">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</latexit>

Df = 3, 1.6 ✓<latexit sha1_base64="FwuQEEpWr1jtunbEdo5M3ce4FNg=">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</latexit><latexit sha1_base64="voWlhDqn3dO/r7nkY91Qpv7ILiE=">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</latexit>

3M0⇢p (r) =
4⇡a3

r2
1+ 2
a

Df=1.6 r=1pc
subvirial
10例

◆ 3/2

Df=1.6 r=1pc
supervirial
10例

Mahalanobis distance
Df=1.6フラクタル分布
N体進化
subvirial

supervirial
6D
3D

6D
3D
3D

Mahalanobis density
subvirial

3D

6D

supervirial 3D

6D

the initial conditions of the
N-body simulations cannot
be constrained using only
the Mahalanobis distanceor density.

6D

1) で規格化。

Stellar clustering shapes the architectures ofplanetary systems, by Winter+ Nature 586, 528 (2020)
位相空間密度の違いで分けた系外惑星の頻度分布

共分散⾏列 S (Wikipediaより)
次のような列ベクトルを考える。
<latexit sha1_base64="d3J/rURCRPDDHNt5F7+6EBugqto=">AAACj3icSyrIySwuMTC4ycjEzMLKxs7BycXNw8vHLyAoFFacX1qUnBqanJ+TXxSRlFicmpOZlxpaklmSkxpRUJSamJuUkxqelO0Mkg8vSy0qzszPCympLEiNzU1Mz8tMy0xOLAEKxQtoVcckpSlE1NrG5KSmlWhExBvqKETEG+koxOSk5JcUgzh5MUWZ6RklmvECygZ6BmCggMkwhDKUGaAgIF9gOUMMQwpDPkMyQylDLkMqQx5DCZCdw5DIUAyE0QyGDAYMBUCxWIZqoFgRkJUJlk9lqGXgAuotBapKBapIBIpmA8l0IC8aKpoH5IPMLAbrTgbakgPERUCdCgyqBlcNVhp8NjhhsNrgpcEfnGZVg80AuaUSSCdB9KYWxPN3SQR/J6grF0iXMGQgdOF1cwlDGoMF2K2ZQLcXgEVAvkiG6C+rmv452CpItVrNYJHBa6D7FxrcNDgM9EFe2ZfkpYGpQbMZuIARYIge3JiMMCM9QzM900ATZQcnaFRwMEgzKDFoAMPbnMGBwYMhgCEUaO8Ehm0M+xkOMAkymTPZMTlAlDIxQvUIM6AAJk8AjTGYVQ==</latexit>

X = (X1 , X2 , . . . , Xn )このベクトルの要素が各々分散が有限である確率変数であるとき、( i, j ) の要素が次のような⾏列 Σ を分散共分散⾏列という。

位相空間密度⾼い
位相空間密度低い<latexit sha1_base64="d+hqVlyt212V/Onr1scqvCcOv8c=">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</latexit>⌃ij = E[(Xiµi )(Xj= E(Xi Xj )E(Xi )E(Xj )

ただし、

µj )]

<latexit sha1_base64="20hPqIuaFhMEc5untlGVtpzIOpM=">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</latexit>µi = E(Xi )は、ベクトル X の i 番⽬の要素の期待値である。
すなわち、S は次のような⾏列である。

S

位相空間密度低い

位相空間密度⾼い12. SOFIA and ALMA Investigate Magnetic Fields and Gas Structures in Massive Star Formation:
The Case of the Masquerading Monster in BYF 73, by Peter J. Barnes et al.

I<latexit sha1_base64="tw3IWjtCk1/SRvX8gJM90G0IGqU=">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</latexit>

B⊥

Vera C Low- High-density tracers⽐較<latexit sha1_base64="YDHKnSOzMFz3EY+yxOQC99O6g6U=">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</latexit>

3n0 ⇠ 10 cm

Fissel +2019

3<latexit sha1_base64="PSH5lHAEocfk0XCFcIpENuA58tw=">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</latexit>

0.88pcZeeman measurement (Crutcher 12)n>n0~300cm-3 B//∝n0.65
n<n0 B-field support clouds

ALMA3mmのI
⼤質量星星形成領域での磁場とclumpの関係。
ALMAダスト偏光と分⼦線とSOFIA偏光<latexit sha1_base64="dBEYsQmj4hfetciFC5PNS8WTguQ=">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</latexit>

0.09pcM ⇠ 2 ⇥ 104 M
Barnes + 20192
Ṁ ⇠ 3 ⇥ 10 M yr 1

等⾼線ALMAのI

0.44pc-- BYF 73

PI<latexit sha1_base64="P/bNa3ZCqvzUOchtDdx6UlHRbc4=">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</latexit>

ALMAの偏波

等⾼線SOFIAのI

ALMA3mmのPI12<latexit sha1_base64="Qb656STNgzphB7oQp5Wzpdr+ors=">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</latexit>

COGoldreich-Kylafis

streamer?

outflow

⾊はPI-17.5~+18km/s
グレイはλ3mmのI

等⾼線はI-60~-22km/s

偏光⽅向を90度回転

Histogram of Relative Orientation⇠ < 0 構造と磁場が⊥⇠ > 0 構造と磁場が∥<latexit sha1_base64="+QqbLeQRBv30exoBR1wwExGmbdM=">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</latexit><latexit sha1_base64="uaYedRVmZbIcJDV/3379aYSya7Q=">AAACaHichVFNLwNBGH66vuurOCAujYY4Ne+KrzhIw8WxPqpNkGZ3DSa2u5vdbYPGH3BxRJxIRMTPcPEHHPwEHCtxcfB2u4nQ4J3MzDPPvM87z8zojik9n+gpojQ0NjW3tLZF2zs6u7pjPb1rnl10DZExbNN2c7rmCVNaIuNL3xQ5xxVaQTdFVt9bqO5nS8L1pG2t+geO2CxoO5bclobmM5XZ2JdzlI8lKElBxOuBGoIEwkjbsRtsYAs2DBRRgIAFn7EJDR63daggOMxtosycy0gG+wJHiLK2yFmCMzRm93jc4dV6yFq8rtb0ArXBp5jcXVbGMUKPdEsVeqA7eqaPX2uVgxpVLwc86zWtcPLdxwMr7/+qCjz72P1S/enZxzZmAq+SvTsBU72FUdOXDk8rK7PLI+VRuqJX9n9JT3TPN7BKb8b1kli+QJQ/QP353PVgbTypTiUnlyYSqfnwK1oxhGGM8XtPI4VFpJHhcyVOcIbzyIsSU/qVwVqqEgk1ffgWyvAn+S2LXQ==</latexit>

⾼<latexit sha1_base64="Owa/RmDKvCGcjoVamTHQzMrRTvI=">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</latexit>⇠ = CHRO (log N

XHRO ) で回帰

低Ncrit = 6.6 ⇥ 1022 cm 2<latexit sha1_base64="TQcPMcZYNGcDDEQyLlgguRNg1jM=">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</latexit>

XHROがNcritを与える

D ⇠ 0.087pc<latexit sha1_base64="IyuQ1lGSh5o76r4qD2a1ZWxpqx4=">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</latexit>

N (0 ⇠ 22.5 ) N (67.5 ⇠ 90 )⇠=N (0 ⇠ 22.5 ) + N (67.5 ⇠ 90 )<latexit sha1_base64="N6Mcib1g1F/jtH4fV5Uc/WSHT2U=">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</latexit>

ncrit ⇠ 2 ⇥ 105 cm 3<latexit sha1_base64="jiqFv2cw1kGtW8VlhyJsjf7mMEc=">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</latexit>

Vela Cよりも⾼密度13. Formation of Rocky Super-Earths From A Narrow Ring of Planetesimals, by Konstantin Batygin,
Alessandro Morbidelli
The formation of super-Earths, the most abundant planets in the Galaxy, remains elusive. These planets have masses that typically exceed that of the
Earth by a factor of a few; appear to be predominantly rocky, although often surrounded by H/He atmospheres; and frequently occur in multiples.
Moreover, planets that encircle the same star tend to have similar masses and radii, whereas those belonging to different systems exhibit remarkableoverall diversity. Here, we advance a theoretical picture for rocky planet formation that satisfies the aforementioned constraints: building upon recent
work - which demonstrates that planetesimals can form rapidly at discrete locations in the disk - we propose that super-Earths originate inside rings ofsilicate-rich planetesimals at approximately ~1 AU. Within the context of this picture, we show that planets grow primarily through pairwise collisions
among rocky planetesimals, until they achieve terminal masses that are regulated by isolation and orbital migration. We quantify our model withnumerical simulations and demonstrate that our synthetic planetary systems bear a close resemblance to compact, multi-resonant progenitors of theobserved population of short-period extrasolar planets. Our results thus indicate that the absence of short-period super-Earths within the solar system
can simply be attributed to the comparatively low mass of the primordial planetesimal ring within the protosolar nebula. (Nature Astron. in press)

14. Carbon Depletion in the Early Solar System, by Fabian Binkert, Til Birnstiel
Earth and other rocky objects in the inner Solar System are depleted in carbon compared to objects in the outer Solar System, the Sun, or the ISM. It isbelieved that this is a result of the selective removal of refractory carbon from primordial circumstellar material. In this work, we study the irreversible
release of carbon into the gaseous environment via photolysis and pyrolysis of refractory carbonaceous material during the disk phase of the early Solar
System. We analytically solve the one-dimensional advection equation and derive an explicit expression that describes the depletion of carbonaceous
material in solids under the influence of radial and vertical transport. We find both depletion mechanisms individually fail to reproduce Solar Systemabundances under typical conditions. While radial transport only marginally restricts photodecomposition, it is the inefficient vertical transport that limits
carbon depletion under these conditions. We show explicitly that an increase in the vertical mixing efficiency, and/or an increase in the directly irradiateddisk volume, favors carbon depletion. Thermal decomposition requires a hot inner disk (> 500 K) beyond 3 AU to deplete the formation region of Earth andchondrites. We find FU Ori-type outbursts to produce these conditions such that moderately refractory compounds are depleted. However, such outbursts
likely do not deplete the most refractory carbonaceous compounds beyond the innermost disk region. Hence, the refractory carbon abundance at 1 AU
typically does not reach terrestrial levels. Nevertheless, under specific conditions, we find photolysis and pyrolysis combined to reproduce Solar Systemabundances. (MNRAS in press)

15. Massive pre-main-sequence stars in M17 -- Modelling hydrogen and dust in MYSO disks, byFrank Backs et al.
The young massive-star-forming region M17 contains optically visible massive pre-main-sequence stars that are surrounded by circumstellar disks.
Such disks are expected to disappear when these stars reach the main sequence. The physical and dynamical structure of these remnant disks are poorly
constrained, especially the inner regions where accretion, photo-evaporation, and companion formation and migration may be ongoing. We aim toconstrain the physical properties of the inner parts of the circumstellar disks of massive young stellar objects B243 (6 Msun) and B331 (12 Msun), twosystems for which the central star has been detected and characterized previously despite strong dust extinction. Two-dimensional radiation thermochemical modelling with ProDiMo of double-peaked hydrogen lines of the Paschen and Brackett series observed with X-shooter was used to probe theproperties of the inner disks. Additionally, the dust structure was studied by fitting the optical and near-infrared spectral energy distribution. B243
features a hot gaseous inner disk with dust at the sublimation radius at 3 AU. The disk appears truncated at roughly 6.5 AU; a cool outer disk of gas anddust may be present, but it cannot be detected with our data. B331 also has a hot gaseous inner disk. A gap separates the inner disk from a colder dusty
outer disk starting at up to 100 AU. In both sources the inner disk extends to almost the stellar surface. Chemistry is essential for the ionization ofhydrogen in these disks. The lack of a gap between the central objects and these disks suggests that they accrete through boundary-layer accretion. This
would exclude the stars having a strong magnetic field. Their structures suggest that both disks are transitional in nature, that is to say they are in theprocess of being cleared, either through boundary-layer accretion, photo-evaporation, or through companion activity.

16. Gaia-ESO Survey: massive stars in the Carina Nebula. A new census of OB stars, by S. R. Berlanas et
The Gaia-ESO survey sample of massive OB stars in the Carina Nebula consists of 234 stars. The addition of brighter sources from the Galactic O-Star
Spectroscopic Survey and additional sources from the literature allows us to create the most complete census of massive OB stars done so far in the region.
It contains a total of 316 stars, being 18 of them in the background and four in the foreground. Of the 294 stellar systems in Car OB1, 74 are of O type, 214
are of non-supergiant B type and 6 are of WR or non-O supergiant (II to Ia) spectral class. We identify 20 spectroscopic binary systems with an O-starprimary, of which 6 are reported for the first time, and another 18 with a B-star primary, of which 13 are new detections. The average observed doublelined binary fraction of O-type stars in the surveyed region is 0.35, which represents a lower limit. We find a good correlation between the spectroscopic nqualifier and the projected rotational velocity of the stars. The fraction of candidate runaways among the stars with and without the n-qualifier is 4.4% and2.4%, respectively, although non resolved double-lined binaries can be contaminating the fast rotators sample.