THESTAR

FORMATION

NEWSLETTER

An electronic publication dedicated to early stellar/planetary evolution and molecular clouds
No. 328 — 16 April 2020

Editor: Bo Reipurth (reipurth@ifa.hawaii.edu)

The Star Formation Newsletter
Editor: Bo Reipurthreipurth@ifa.hawaii.edu
Ayop i.

more metamorphosed, the now-eroded limestone had become coarsely crystalline, like marble, and the fossils werebarely recognizable as such. The analogy to the texturalsequence in chondrites was obvious. I later wrote a paper
on metamorphism in chondrites.

John Woodin conversation with Bo Reipurth

Q: Today we take metamorphism in chondrites as a given,
but at the time the idea ran into some resistance. In 1967
Van Schmus and you combined the metamorphism andchemistry of chondrites into a classification system thatis a general tool today. Was that what finally convinced
the community about metamorphism?
A: I learned that colleague Randall Van Schmus had madethe same discovery, and we collaborated in a program to
study as many chondrite thin sections as we could findand classify the degree of metamorphism each displayed.
The paper we published has become widely cited, and it
convinced most workers.
Q: Later you derived the cooling rates in differentiated bodies in the early solar system. What was the method you
used and what rates did you find?

Q: You got your PhD in 1958 from the Massachusetts Institute of Technology on an analysis of over a hundred thinsections cut from stony meteorites. What were your results?

A: In the 1960s, while I was post-doc’ing with Edward
Anders in Chicago, I got interested in iron meteorites
and read up on metallurgy. Clearly these meteorites had
formed during melting in small bodies, when molten metallic nickel-iron in the parent material separated from silicate magma and sank to the centers of the planetesimals.
As these cooled, the Fe-Ni phase diagram predicts thatthe solidified metal started out as the alloy taenite. With
continued cooling, crystals of low-nickel kamacite would
have precipitated from the higher-nickel taenite. As the
kamacite crystals grew they had to push the Ni they were
rejecting back into the remaining taenite, where it formed
high-Ni zones. Nickel moved by solid-state diffusion fromthese zones into the residual lower-Ni taenite. I studied
the final frozen-in Ni profiles in a series of iron meteorites,
using an electron-probe microanalyzer. I called them Mprofiles because they resembled that letter, with the highNi zones forming its shoulders and the low-Ni residual
taenite forming the trough. The size of the M-profiles
had to depend on the rate at which the metal cooled. Mprofiles remained larger if the cooling was too slow for diffusion to allow Ni to flow in and fill the troughs. I studied
the relationship between M-profile sizes and the amountof Ni that made it into the troughs.

A: Nobody had studied stony meteorites microscopicallyfor many years. I’d always had a romance about astronomy, so I opted for that as my minor subject at MIT, notentirely to the liking of my thesis committee. This led tosome Harvard astronomy courses, and acquaintance withFred Whipple.
A happy circumstance led mineralogy Prof Cliff Frondel toshow me a chest of old thin sections which had been cut
from a collection of meteorites by J. Lawrence Smith in
the 19th century. These were no more than a curiosity inthe mineralogy department, so he was glad to lend themto me to examine at my leisure. Which I did, borrowing
time from my thesis topic, which was ring dikes in the
New Hampshire White Mountains and a study of theirpetrology by a new technique of rapid chemical analysis.
The latter program did not go well, and as my interest
in it waned, the siren song of chondrites and chondrules
grew louder. Eventually my thesis advisor, Gordon J. F.
Macdonald, realized this and allowed me to switch mythesis topic to the petrology and origin of chondrites. It
was obvious to me that there was a textural spectrum
ranging from sharply defined chondrules embedded in finegrained matrix to crystalline rocks with indistinct boundaries between chondrules and their surroundings. Macdonald drew my attention to a paper by G. Bain at Amherst
College, who had studied a band of fossiliferous limestonethat stretched through Vermont. At one end, where therock had not been buried deeply, it contained sharply defined fossil invertebrates. At the other end, where therock had been more deeply buried and thus hotter andCalculating the effect of cooling in such a system is an interesting problem in differential equations. I was neverstrong in mathematics, but happily I learned early onthat you can cheat and use iterative numerical calculations
to bypass formal math, and I became proficient in FORTRAN programming. Modeling the formation of the ironmeteorite M-profiles in this fashion, using experimentallydetermined diffusion coefficients, I found that most of the3meteorites I studied cooled at about 10C per million years;
while others cooled more slowly, about 1C per million
years. To relate cooling rates to the sizes of the planetary bodies the meteorites resided in required calculating
planetary heat loss rates as a function of size, but this was
not too hard; the problem of heat diffusion in a planet
is analogous to the problem of nickel diffusion in taenite.
The 10C/myr meteorites cooled in bodies 50-90 km in radius, the 1C/myr meteorites from bodies 130-260 km in
radius. Those are asteroidal dimensions.

set to work to study as many of those rock-ettes as we
could in the time we had. Which was not much: NASA
had decreed that on January 5, 1970, all of the lunar sample investigators were to convene in Houston, Texas, andpresent the results of their studies. Just 109 days after I
picked up our sample.
Petrographers study rocks in thin sections: slivers of rockabout 30 micrometers thick (a human hair is about thatdiameter) mounted on glass microscope slides, which are
created by a rather tedious process of diamond sawing,
grinding, and polishing on the surfaces of spinning laps.
We made our own thin sections in our laboratory, 1676 ofthem, and studied them microscopically and in our electron microprobe. We learned that about half of the Mare
Tranquillitatis regolith consists of soil breccias, which arevolumes of fine lunar soil that had been crammed together
and lithified by meteoroid impacts. About 5% of the particles were glasses: rock or soil that had been melted by
the energy of an impact, which then cooled rapidly byradiation into space. Another 40% of the particles were
crystalline igneous rocks. It might seem they would all besimilar representatives of the basaltic rock that underlies
Tranquillity Base, so the job of describing them would be
simple, but that was not to be the case. Studies had shownthat the debris from a cratering impact can travel great
distances, so the soil particles that were collected at any
point on the moon may have come from many different
far-flung sources. Most of the igneous particles consistedof hardened basaltic lava (it had long been evident thatthe lunar maria must have been filled with lava); but manyvarieties of lava, differing in chemistry and texture.

Q: In 1969 the Allende meteorite fell in Mexico, and Ursula Marvin and you published the first analysis. Why is
Allende so important in meteoritics?
A: I believe it’s because Allende was the first carbonaceouschondrite to be widely distributed to scientists for study.
Carbonaceous chondrites are important because they havenot experienced the degree of heating and metamorphismthat I just talked about. Metamorphism has wiped out
much of the evidence of early solar system events that wewant to learn about. Allende allowed us to see it better.
Q: In the early 1970s you were able to get and study lunar
soil from the Apollo missions. This led to an unexpected
and important new insight into the Moon. Please tell about
the circumstances of this work.
A: In the early 1960s, NASA wanted scientists to study the
samples that they expected to be collected on the moonin the Apollo program, and they issued an invitation toqualified individuals to submit proposals to be lunar sample investigators. My history, described above, qualified
me. By that time I was working at the Smithsonian Astrophysical Observatory in Cambridge, Mass. (where I
spent the rest of my career) under Fred Whipple, who had
encouraged me to set up a meteorite laboratory there. I
submitted a proposal to NASA, and recruited two freshlyminted Ph.Ds, John Dickey from Princeton University and
Ben Powell from Columbia, to work with me. They werejoined in my group by Ursula Marvin, a mineralogist andx-ray diffraction expert, who was already at SAO.

However, another 3-4% of the igneous particles were something quite different and unexpected. They were white andanorthositic in chemical composition. Anorthosite is an igneous rock type rare on earth; an important anorthosite
occurrence is in the Adirondack Mountains of New York.
Anorthositic rocks consist principally of the mineral anorthite (CaAl2 Si2 O9 ). No previous work had predicted thatthe moon would contain this surprising rock type.

In September 1969 approved lunar investigators were calledto Houston to receive the samples that had been allocatedto them, and I received two sieved samples of the lunar regolith (pulverized cratering debris that covered the moon).
The most important sample turned out to be 11 gramsof coarse lunar fines larger than 1-millimeter in size andmostly smaller than 2-mm. When my group examined it
under a binocular microscope, we found to our surprisethat it was not just a pulverized mineral dust, as I had
pessimistically assumed it would be. Once rinsed in organic solvents, the coarse fines could be seen to consist of
tiny miniature rocks, each with a distinctive texture andassemblage of minerals. We realized we had hundreds ofseparate and distinct lunar samples on our hands! So we

Where might this light-colored component of anorthositic
particles have come from? That question was not so hardto answer. The Apollo lander Eagle had set down on
the edge of dark mare-basalt-filled Mare Tranquillitatis,
only about 50 kilometers from the beginning of the lightcolored lunar highlands or terrae. Impacts on the terra
regolith surely would have scattered some of it over into
the mare regolith. This must have been the source of theanorthositic fragments in our sample.
Did this unexpected composition hold for all of the lightcolored terra rock that covered most of the moon, or justthat corner of it? An earlier NASA unmanned mission to
the moon, Surveyor 7, appeared to hold the answer to thatquestion. Surveyor 7 carried a device, the alpha-scattering
4

surface analyzer, which used the phenomenon of Rutherford scattering to measure the chemical composition of thesurface on the ejecta blanket of the crater Tycho, whosedramatic rays circle the moon. Tycho is in lunar terramaterial far removed from Tranquillity Base. The result
was consistent with an anorthositic composition for terramaterial there too.

stand it. Sadly, I failed. I wish I had time to try it overagain.

on it pushes subcrustal rock aside, making room for theload to sink. Isostasy will allow a mountain range to standonly if the mountains are lighter (less dense) than the rockbeneath them so they can ‘’float’ in it. The light (specificgravity 2.9) lunar crust can float 3 kilometers above thedenser interior (moon’s overall specific gravity = 3.35), as
is observed, only if the crustal thickness is about 25 kilometers. That’s lot of anorthosite!

Q: You have had a lifelong interest in the interface between
cosmochemistry and astrophysics, and have worked on andwritten extensively about this fertile area. Yet, the two
communities still are quite separate. Why do you thinkthat is, and how can we break down the barrier?

It’s a tough problem. You need to answer several central
questions: why do some of the chondrules have olivine-richcompositions, similar to the average composition of chondrites, while in other cases the top of the igneous crystallization sequence (spoken of above), got skipped over
Generalizing boldly, it seemed clear to us that a high- during chondrule cooling, so that those melt droplets crysalbedo anorthosite-rich crustal layer covers the whole moon, tallized little or no olivine, and they were left with more
atop whatever lies beneath, except where giant impacts feldspar-rich compositions? What hydrodynamic process
have blasted holes (mare basins) through it, which filled size-sorted the chondrules after they were formed, reservwith basaltic lava.
ing millimeter-scale objects for the asteroid belt and somehow
disposing of larger silicate objects? I have wondered
The principle of isostasy (crustal buoyancy) allows theifthemighty gravity field of nearby Jupiter played somethickness of this layer to be estimated. Rock has plastic
role
in
the things that happened.
properties over long periods of time, meaning a heavy load

A: I guess the problem is that their subject matter andcultures are just too disparate. The person who worked
hardest to solve this problem was astrophysicist A. G. W.
How could this layer of rare anorthite-rich rock have formed? Cameron, who beginning in 1962 organized a series of GorThe experimentally determined sequence of minerals that don Research Conferences on the Physics and Chemistry
crystallize from a cooling silicate melt rich in magnesium of Space. Al always made a point of mixing practitioners ofand iron predicts that the mineral olivine appears first, fol- as many relevant disciplines as possible into his programs.
lowed by pyroxenes and calcic feldspar, then sodic feldspar. I was flattered to be on the first such program (“Formation
Olivine is dense, and it would tend to sink to the floor of a and Properties of Chondrules”). BTW, George Herbig also
volume of magma during crystallization. On the other spoke at this conference. I don’t know how to break down
hand, crystallizing calcic feldspar (anorthite) is lighter, the barrier. Maybe cosmochemists find astrophysics too
and under some circumstances it would tend to float rather arcane and difficult, and astrophysicists disrespect cosmothan sink, accumulating at the top of the cooling magma. chemistry as pedestrian. I’ve heard a physicist say “science
Such a process of separating minerals seems to be the only is largely physics; everything else is stamp collecting”.
possible explanation for the concentration of anorthosite
in the crust of the moon.
How much magma would have been needed to form thecrust by this process of crystal fractionation? Assuming aplausible bulk chemical composition for the moon, it turns
out most or all of the moon must have melted in order for
25 kilometers of anorthite crystals to float to the top. I
later coined the term ’magma ocean’ to describe this hugequantity of magma, and the term has caught on.
That’s the story I told in my talk at the First Lunar Science Conference, and people found it convincing. Several other research groups had noticed and described theanorthositic particles in the lunar soil sample, but they
didn’t pursue their meaning.
Q: The formation of chondrules has been the subject ofmuch of your work. What are some of the key issues?
A: Chondrules contain a mine of information about theearly solar nebula, and I made it my life’s work to under5

Abstracts of recently accepted papers

1. Characterising lognormal fractional-Brownian-motion density fields with a Convolu-

tional Neural Network
M L Bates1 , A P Whitworth1 and O D Lomax1,2
School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, UK; 2 ESTEC, Keplerlaan 1, 2201 AZ
Noordwijk, Netherlands

1E-mail contact: matthew.bates at astro.cf.ac.uk
In attempting to quantify statistically the density structure of the interstellar medium, astronomers have considereda variety of fractal models. Here we argue that, to properly characterise a fractal model, one needs to define precisely
the algorithm used to generate the density field, and to specify – at least – three parameters: one parameter constrains
the spatial structure of the field; one parameter constrains the density contrast between structures on different scales;
and one parameter constrains the dynamic range of spatial scales over which self-similarity is expected (either due
to physical considerations, or due to the limitations of the observational or numerical technique generating the inputdata). A realistic fractal field must also be noisy and non-periodic. We illustrate this with the exponentiated fractional
Brownian motion (xfBm) algorithm, which is popular because it delivers an approximately lognormal density field, andfor which the three parameters are, respectively, the power spectrum exponent, β, the exponentiating factor, S, andthe dynamic range, R. We then explore and compare two approaches that might be used to estimate these parameters:
Machine Learning and the established ∆-Variance procedure. We show that for 2 ≤ β ≤ 4 and 0 ≤ S ≤ 3, a suitablytrained Convolutional Neural Network is able to estimate objectively both β (with root-mean-square error ǫβ ∼ 0.12)
and S (with ǫS ∼ 0.29). ∆-variance is also able to estimate β, albeit with a somewhat larger error (ǫβ ∼ 0.17) andwith some human intervention, but is not able to estimate S.
Accepted by Monthly Notices of the Royal Astronomical Society
https://arxiv.org/pdf/2002.05506

2. A kinematically hot population of young stars in the solar neighbourhood
A.S. Binks1 , R.D. Jeﬀries1 and N.J. Wright1
1

Astrophysics Group, School of Chemistry and Physics, Keele University, UK

E-mail contact: a.s.binks1 at keele.ac.uk
In the last three decades several hundred nearby members of young stellar moving groups (MGs) have been identified,
but there has been less systematic effort to quantify or characterise young stars that do not belong to previously
identified MGs. Using a kinematically unbiased sample of 225 lithium-rich stars within 100 pc, we find that only
50±10 per cent of young (<∼125 Myr), low-mass (0.5 < M/M⊙ < 1.0) stars, are kinematically associated with known
MGs. Whilst we find some evidence that six of the non-MG stars may be connected with the Lower Centaurus-Crux
association, the rest form a kinematically “hotter” population, much more broadly dispersed in velocity, and withno obvious concentrations in space. The mass distributions of the MG members and non-MG stars is similar, but
the non-MG stars may be older on average. We briefly discuss several explanations for the origin of the non-MG
population.
Accepted by MNRAS
http://arxiv.org/pdf/2003.13369

3. Probing the magnetospheric accretion region of the young pre-transitional disk system

DoAr 44 using VLTI/GRAVITY

J. Bouvier1 , K. Perraut1 , J.-B. Le Bouquin1 , G. Duvert1 , C. Dougados1 , W. Brandner2 , M. Benisty1,3 ,J.-P. Berger1 and E. Alécian16Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France; 2 Max Planck Institute for Astronomy, Königstuhl
17, 69117 Heidelberg, Germany; 3 Unidad Mixta Internacional Franco-Chilena de Astronomía (CNRS, UMI 3386),
Univ. Chile, Chile
1

E-mail contact: jerome.bouvier at univ-grenoble-alpes.fr
Young stellar objects are thought to accrete material from their circumstellar disks through their strong stellar magnetospheres. We aim to directly probe the magnetospheric accretion region on a scale of a few 0.01 au in a youngstellar system using long-baseline optical interferometry. We observed the pre-transitional disk system DoAr 44 with
VLTI/GRAVITY on two consecutive nights in the K-band. We computed interferometric visibilities and phases in
the continuum and in the BrG line in order to constrain the extent and geometry of the emitting regions. We resolve
the continuum emission of the inner dusty disk and measure a half-flux radius of 0.14 au. We derive the inclinationand position angle of the inner disk, which provides direct evidence that the inner and outer disks are misalignedin this pre-transitional system. This may account for the shadows previously detected in the outer disk. We showthat BrG emission arises from an even more compact region than the inner disk, with an upper limit of 0.047 au (5Rstar). Differential phase measurements between the BrG line and the continuum allow us to measure the astrometricdisplacement of the BrG line-emitting region relative to the continuum on a scale of a few tens of microarcsec, corresponding to a fraction of the stellar radius. Our results can be accounted for by a simple geometric model where the
BrG line emission arises from a compact region interior to the inner disk edge, on a scale of a few stellar radii, fully
consistent with the concept of magnetospheric accretion process in low-mass young stellar systems.
Accepted by Astronomy & Astrophysics
http://arxiv.org/pdf/2004.00848

4 Hunting for hot corinos and WCCC sources in the OMC-2/3 filament
M. Bouvier1 , A. López-Sepulcre1,2 , C. Ceccarelli1,3 , C. Kahane1 , M. Imai4 et al.
Univ. Grenoble Alpes, CNRS, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG), 38000 Grenoble,
France; 2 Institut de Radioastronomie Millimétrique (IRAM), 300 rue de la Piscine, 38406 Saint-Martin-D’Hères,France; 3 CNRS, IPAG, F-38000 Grenoble, France; 4 Department of Physics, The University of Tokyo, 7-3-1, Hongo,
Bunkyo-ku, Tokyo 113-0033, Japan1

E-mail contact: mathilde.bouvier at univ-grenoble-alpes.fr
Context. Solar-like protostars are known to be chemically rich, but it is not yet clear how much their chemicalcomposition can vary and why. So far, two chemically distinct types of Solar-like protostars have been identified:
hot corinos, which are enriched in interstellar Complex Organic Molecules (iCOMs), such as methanol (CH3 OH) or
dimethyl ether (CH3 OCH3 ), and Warm Carbon Chain Chemistry (WCCC) objects, which are enriched in carbon
chain molecules, such as butadiynyl (C4 H) or ethynyl radical (CCH). However, none of these have been studied so far
in environments similar to that in which our Sun was born, that is, one that is close to massive stars.
Aims. In this work, we search for hot corinos and WCCC objects in the closest analogue to the Sun’s birth environment,
the Orion Molecular Cloud 2/3 (OMC-2/3) filament located in the Orion A molecular cloud.
Methods. We obtained single-dish observations of CCH and CH3 OH line emission towards nine Solar-like protostars
in this region. As in other, similar studies of late, we used the [CCH]/[CH3 OH] abundance ratio in order to determine
the chemical nature of our protostar sample.
Results. Unexpectedly, we found that the observed methanol and ethynyl radical emission (over a few thousands au
scale) does not seem to originate from the protostars but rather from the parental cloud and its photo-dissociation
region, illuminated by the OB stars of the region.
Conclusions. Our results strongly suggest that caution should be taken before using [CCH]/[CH3 OH] from single-dishobservations as an indicator of the protostellar chemical nature and that there is a need for other tracers or highangular resolution observations for probing the inner protostellar layers.
Accepted by A&A
http://arxiv.org/pdf/2003.06198

7

5. A new proxy to estimate the cosmic-ray ionisation rate in dense cores
S. Bovino1 , S. Ferrada-Chamorro1 , A. Lupi2 , D.R.G. Schleicher1 , and P. Caselli3
Departamento de Astronomía, Facultad Ciencias Físicas y Matemáticas, Universidad de Concepción, Av. Esteban
Iturra s/n Barrio Universitario, Casilla 160, Concepción, Chile; 2 Scuola Normale Superiore, Piazza dei Cavalieri 7,
Pisa, IT-56126 Italy; 3 Centre for Astrochemical Studies, Max-Planck-Institute for Extraterrestrial Physics, Giessenbachstrasse 1, 85748, Garching, Germany
1E-mail contact: stefanobovino at udec.cl
Cosmic rays are a global source of ionisation, and the ionisation fraction represents a fundamental parameter in theinterstellar medium. Ions couple to magnetic fields, affect the chemistry, and the dynamics of star-forming regions
as well as planetary atmospheres. However, the cosmic-ray ionisation rate represents one of the bottlenecks for
astrochemical models, and its determination is one of the most puzzling problems in astrophysics. While for diffuse
clouds reasonable values have been provided from H3 + observations, for dense clouds, due to the lack of rotationaltransitions, this is not possible, and estimates are strongly biased by the employed model. We present here an analyticalexpression, obtained from first principles, to estimate the cosmic-ray ionisation rate from observational quantities. The
theoretical predictions are validated with high-resolution three-dimensional numerical simulations and applied to thewell known core L1544; we obtained an estimate of ζ2 ∼ 2–3 × 10−17 s−1 . Our results and the analytical formulae
provided represent the first model-independent, robust tool to probe the cosmic-ray ionisation rate in the densest partof star-forming regions (on spatial scales of R ≤ 0.05 pc). An error analysis is presented to give statistical relevanceto our study.
Accepted by MNRAS Letters
http://arxiv.org/pdf/2003.05416

6. An imaging line survey of OMC-1 to OMC-3
N. Brinkmann1 , F. Wyrowski1 , J. Kauﬀmann2 , D. Colombo1 , K.M. Menten1 et al.
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany; 2 Haystack Observatory,
Massachusetts Institute of Technology, Westford, MA 01886, USA
1E-mail contact: brinkmann at mpifr-bonn.mpg.de
Aims. Our aim is to identify the dominant molecular cooling lines and characteristic emission features in the 1.3 mm
window of distinct regions in the northern part of the Orion A molecular cloud. By defining and analysing templateregions, we also intend to help with the interpretation of observations from more distant sources which cannot beeasily spatially resolved.
Methods. We analyse an imaging line survey covering the area of OMC-1 to OMC-3 from 200.2 to 281.8 GHz obtainedwith the PI230 receiver at the APEX telescope. Masks are used to define regions with distinct properties (e.g. column
density or temperature ranges) from which we obtain averaged spectra. Lines of 29 molecular species (55 isotopologues)
are fitted for each region to obtain the respective total intensity.
Results. We find that strong sources like Orion KL have a clear impact on the emission on larger scales. Although not
spatially extended, their line emission contributes substantially to spectra averaged over large regions. Conversely, theemission signatures of dense, cold regions like OMC-2 and OMC-3 (e.g. enhanced N2 H+ emission and low HCN/HNC
ratio) seem to be difficult to pick up on larger scales, where they are eclipsed by signatures of stronger sources. In
all regions, HCO+ appears to contribute between 3% and 6% to the total intensity, the most stable value for all
bright species. N2 H+ shows the strongest correlation with column density, but not with typical high-density tracers
like HCN, HCO+, H2 CO, or HNC. Common line ratios associated with UV illumination, CN/HNC and CN/HCO+ ,show ambiguous results on larger scales, suggesting that the identification of UV illuminated material may be morechallenging. The HCN/HNC ratio may be related to temperature over varying scales.
Accepted by A&A
http://arxiv.org/pdf/2003.06842

8

7. The Planetary Luminosity Problem: “Missing Planets” and the Observational Conse-

quences of Episodic Accretion
Sean Brittain1 , Joan R. Najita2 , Ruobing Dong3 and Zhaohuan Zhu4
Clemson University, 118 Kinard Laboratory, Clemson, SC 29634, USA; 2 National Optical Astronomical Observatory,
950 North Cherry Avenue, Tucson, AZ 85719, USA; 3 Department of Physics and Astronomy, University of Victoria,
Victoria BC V8P 1A1, Canada; 4 Department of Physics and Astronomy, University of Nevada, Las Vegas, 4505 S.
Maryland Pkwy, Las Vegas, NV 89154, USA

1E-mail contact: sbritt at clemson.edu
The high occurrence rates of spiral arms and large central clearings in protoplanetary disks, if interpreted as signposts ofgiant planets, indicate that gas giants form commonly as companions to young stars (< few Myr) at orbital separationsof 10–300 au. However, attempts to directly image this giant planet population as companions to more mature stars(> 10 Myr) have yielded few successes. This discrepancy could be explained if most giant planets form “cold start,”i.e., by radiating away much of their formation energy as they assemble their mass, rendering them faint enough toelude detection at later times. In that case, giant planets should be bright at early times, during their accretion phase,and yet forming planets are detected only rarely through direct imaging techniques. Here we explore the possibility
that the low detection rate of accreting planets is the result of episodic accretion through a circumplanetary disk.
We also explore the possibility that the companion orbiting the Herbig Ae star HD 142527 may be a giant planet
undergoing such an accretion outburst.
Accepted by ApJ
https://arxiv.org/pdf/2003.11980

8. The GRAVITY young stellar object survey. II. First spatially resolved observations of

the CO bandhead emission in a high-mass YSO
A. Caratti o Garatti1,2,3 , R. Fedriani1,3,4 , R. Garcia Lopez1,2,3 , M. Koutoulaki1,3,5 , K. Perraut6 , H. Linz2 ,W. Brandner2 , P. Garcia7,8,9 and L. Klarmann et al.2
Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, D02 XF86 Dublin, Ireland; 2 MPIA, Königstuhl
17, Heidelberg, Germany, D-69117; 3 University College Dublin, School of Physics, Belfield, Dublin 4, Ireland; 4
Dept of Space, Earth & Environment, Chalmers Univ. of Technology, SE-412 93 Gothenburg, Sweden; 5 ESO, KarlSchwarzschild-Str. 2, D-85748, Garching, Germany; 6 Univ. Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France;
7
Universidade do Porto - Faculdade de Engenharia, Rua Dr. Roberto Frias, 4200-465 Porto, Portugal; 8 CENTRA,
Instituto Superior Tecnico, Av. Rovisco Pais, 1049-001 Lisboa, Portugal; 9 ESO, Casilla 19001, Santiago 19, Chile
1

E-mail contact: alessio at cp.dias.ie
The inner regions of the discs of high-mass young stellar objects (HMYSOs) are still poorly known due to the small
angular scales and the high visual extinction involved. We deploy near-infrared (NIR) spectro-interferometry toprobe the inner gaseous disc in HMYSOs and investigate the origin and physical characteristics of the CO bandhead
emission (2.3–2.4 µm). We present the first GRAVITY/VLTI observations at high spectral (R=4000) and spatial(mas) resolution of the CO overtone transitions in NGC 2024 IRS 2. The continuum emission is resolved in allbaselines and is slightly asymmetric, displaying small closure phases (≤8◦ ). Our best ellipsoid model provides a disc
inclination of 34◦ ±1◦ , a disc major axis position angle (P A) of 166◦ ±1◦ , and a disc diameter of 3.99±0.09 mas (or1.69±0.04 au, at a distance of 423 pc). The small closure phase signals in the continuum are modelled with a skewed
rim, originating from a pure inclination effect. For the first time, our observations spatially and spectrally resolve thefirst four CO bandheads. Changes in visibility, as well as differential and closure phases across the bandheads aredetected. Both the size and geometry of the CO-emitting region are determined by fitting a bidimensional Gaussian
to the continuum-compensated CO bandhead visibilities. The CO-emitting region has a diameter of 2.74±0.08
0.07 mas(1.16±0.03 au), and is located in the inner gaseous disc, well within the dusty rim, with inclination and P A matching
the dusty disc geometry, which indicates that both dusty and gaseous discs are coplanar. Physical and dynamical gas
conditions are inferred by modelling the CO spectrum. Finally, we derive a direct measurement of the stellar mass ofM∗ ∼14.7+2−3.6 M⊙ by combining our interferometric and spectral modelling results.
Accepted by A&A (635, L12)https://arxiv.org/pdf/2003.05404
99. Relative Alignment between Dense Molecular Cores and Ambient Magnetic Field: The

Synergy of Numerical Models and Observations
Che-Yu Chen1 , Erica A. Behrens2 , Jasmin E. Washington1 , Laura M. Fissel3,4, Rachel K. Friesen3,5 etal.
Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA; 2 Department of Astronomy,
Ohio State University, Columbus, OH 43210, USA; 3 National Radio Astronomy Observatory, Charlottesville, VA
22904, USA; 4 Department of Physics, Engineering Physics and Astronomy, Queen’s University, Kingston, ON K7L
3N6, Canada
1E-mail contact: cc6pg at virginia.edu
The role played by magnetic field during star formation is an important topic in astrophysics. We investigate thecorrelation between the orientation of star-forming cores (as defined by the core major axes) and ambient magnetic
field directions in 1) a 3D MHD simulation, 2) synthetic observations generated from the simulation at different viewing
angles, and 3) observations of nearby molecular clouds. We find that the results on relative alignment between coresand background magnetic field in synthetic observations slightly disagree with those measured in fully 3D simulation
data, which is partly because cores identified in projected 2D maps tend to coexist within filamentary structures, while
3D cores are generally more rounded. In addition, we examine the progression of magnetic field from pc- to core-scalein the simulation, which is consistent with the anisotropic core formation model that gas preferably flow along themagnetic field toward dense cores. When comparing the observed cores identified from the GBT Ammonia Survey(GAS) and Planck polarization-inferred magnetic field orientations, we find that the relative core-field alignment has aregional dependence among different clouds. More specifically, we find that dense cores in the Taurus molecular cloud
tend to align perpendicular to the background magnetic field, while those in Perseus and Ophiuchus tend to haverandom (Perseus) or slightly parallel (Ophiuchus) orientations with respect to the field. We argue that this feature of
relative core-field orientation could be used to probe the relative significance of the magnetic field within the cloud.
Accepted by MNRAS
http://arxiv.org/pdf/2003.11033

10. Accretion in low-mass members of the Orion Nebula Cluster with young transition disks
R. M. G. de Albuquerque1,2,3 , J. F. Gameiro1,2 , S. H. P. Alencar4 , J. J. G. Lima1,2 , C. Sauty3,5 and C.
Melo6
Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, PT4150-762 Porto,
Portugal; 2 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Rua do Campo
Alegre 687, PT4169-007 Porto, Portugal; 3 Laboratoire Univers et Théories, Observatoire de Paris, Université PSL,
CNRS, Université de Paris, 92190 Meudon, France; 4 Departamento de Física - ICEx-UFMG, Av. Antônio Carlos,
6627, 30270-901 Belo Horizonte, MG, Brazil; 5 LUPM, Université de Montpellier, UMR 5299 CNRS/IN2P3, cc072,
place Eugène Bataillon, 34090 Montpellier, France; 6 European Southern Observatory, Alonso de Córdova 3107,
Vitacura, Región Metropolitana, Chile
1

E-mail contact: Raquel.Albuquerque at astro.up.pt
Although the Orion Nebula Cluster is one of the most studied clusters in the solar neighborhood, the evolution of
the very low-mass members (M∗ < 0.25 M⊙) has not been fully addressed due to their faintness. Our goal is toverify if some young and very low-mass objects in the Orion Nebula Cluster show evidence of ongoing accretion using
broadband VLT/X-Shooter spectra. For each target, we determined the corresponding stellar parameters, veiling,observed Balmer jump, and accretion rates. Additionally, we searched for the existence of circumstellar disks throughavailable on-line photometry. We detected accretion activity in three young stellar objects in the Orion Nebula
Cluster, two of them being in the very low-mass range. We also detected the presence of young transition disks withages between 1 and 3.5 Myr.
Accepted by A&A
https://arxiv.org/pdf/2003.09511

1011. An ALMA/NOEMA study of gas dissipation and dust evolution in the 5 Myr-old

HD141569A hybrid disc

E. Di Folco1 , J. Péricaud1 , A. Dutrey1 , J.-C. Augereau2 , E. Chapillon3 , S. Guilloteau1 , V. Piétu3 and
A. Boccaletti4
Laboratoire d’Astrophysique de Bordeaux, Université de Bordeaux, CNRS, B18N, Allée Geoffroy Saint-Hilaire,
33615, Pessac, France; 2 Univ. Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France; 3 IRAM, 300 rue de lapiscine, F-38406 Saint Martin d’Hères, France; 4 LESIA, Observatoire de Paris, PSL Research Univ., CNRS, Univ.
Paris Diderot, Sorbonne Paris Cité, UPMC Paris 6, Sorbonne Univ., 5 place Jules Janssen, 92195 Meudon CEDEX,France1E-mail contact: emmanuel.di-folco at u-bordeaux.fr
Context. The study of gas-rich debris discs is fundamental to characterising the transition between protoplanetary
discs and debris discs.
Aims. We determine the physical parameters of the brightest gas-rich debris disc orbiting HD 141569A. Methods. We analyse images from the NOrthern Extended Millimeter Array (NOEMA) and the Atacama Large Millimeter/submillimeter Array (ALMA) in 12 CO , 13 CO J=2→1, and 13 CO J=1→0 transitions. We incorporate ALMA
archival data of the 12 CO J=3→2 transition and present continuum maps at 0.87 mm, 1.3 mm, and 2.8 mm. We use
simple parametric laws with the Diskfit code and MCMC exploration to characterise the gas disc parameters andreport a first attempt to characterise its chemical content with IRAM-30m.
Results. The continuum emission is equally shared between a compact (<∼50 au) and a smooth, extended dust component (∼ 350 au). Large millimetre grains seem to dominate the inner regions, while the dust spectral index is
marginally larger in the outer region. The 12 CO is optically thick, while 13 CO is optically thin with τ13 CO ∼ 0.15
(C18 O is not detected). The 13 CO surface density is constrained to be one order of magnitude smaller than aroundyounger Herbig Ae stars, and we derive a gas mass M12 CO = 10−1 M⊕ . We confirm the presence of a small CO
cavity (RCO = 17 ± 3 au), and find a possibly larger radius for the optically thin 13 CO J=2→1 transition (35 ± 5 au).
We show that the observed CO brightness asymmetry is coincident with the complex ring structures discovered with
VLT/SPHERE in the inner 90 au. The 12 CO temperature T0 (100 au) ∼ 30 K is lower than expected for a Herbig A0star, and could be indicative of subthermal excitation.
Conclusions. With the largest amount of dust and gas among hybrid discs, HD 141569A shows coincident characteristics of both protoplanetary discs (central regions), and debris discs at large distance. Together with its morphologicalcharacteristics and young age, it appears to be a good candidate to witness the transient phase of gas dissipation, with
an apparently large gas-to-dust ratio (G/D > 100) favouring a faster evolution of dust grains.
Accepted by Astronmy & Astrophysics
https://www.aanda.org/articles/aa/full_html/2020/03/aa32243-17/aa32243-17.html

12. A Multiple Power Law Distribution for Initial Mass Functions
Christopher Essex1 , Shantanu Basu1 , Janett Prehl2 and Karl Heinz Hoﬀmann2
1

The University of Western Ontario, London, Canada.; 2 Technische Universitat Chemnitz, Chemnitz, Germany.

E-mail contact: basu at uwo.ca
We introduce a new multi-power-law distribution for the Initial Mass Function (IMF) to explore its potential properties.
It follows on prior work that introduced mechanisms accounting for mass accretion in star formation, developed within
the framework of general evolution equations for the mass distribution of accreting and non-accreting (proto)stars.
This paper uses the same fundamental framework to demonstrate that the interplay between a mass-dependent and atime-dependent step-like dropout rate from accretion leads to IMFs that exhibit multiple power laws for an exponential
mass growth. While the mass-dependent accretion and its dropout is intrinsic to each star, the time-dependent dropout
might be tied to a specific history such as the rapid consumption of nebular material by nearby stars or the sweeping
away of some material by shock waves. The time-dependent dropout folded into the mass-dependent process of starformation is shown to have a significant influence on the IMFs.
Accepted by MNRAS
http://www.astro.uwo.ca/~basu/

1113. A ringed pole-on outflow from DO Tauri revealed by ALMA
Manuel Fernández López1 , Luis A. Zapata2 , Luis F. Rodríguez2 , María M. Vazzano1 , Andrés E.
Guzmán3 and Rosario López4
Instituto Argentino de Radioastronomía, CONICET, 1894, Villa Elisa, Buenos Aires, Argentina; 2 Instituto deRadioastronomía y Astrofísica, UNAM, P.O. Box 3-72, 58090, Morelia, Michoacán, México; 3 National Astronomical Observatory of Japan, NINS, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; 4 Departament d’Astronomia i
Meteorologia (IEEC-UB), ICC, U. de Barcelona, Martí i Franquès 1, E-08028 Barcelona, Spain
1

E-mail contact: manferna at gmail.com
We present new ALMA Band 6 observations including the CO (2-1) line and 1.3 mm continuum emission from thesurroundings of the young stellar object DO Tauri. The ALMA CO molecular data show three different series ofrings at different radial velocities. These rings have radii around 220 au and 800 au. We make individual fits to therings and note that their centers are aligned with DO Tauri and its optical high-velocity jet. In addition, we noticethat the velocity of these structures increases with the separation from the young star. We discuss the data under
the hypothesis that the rings represent velocity cuts through three outflowing shells that are possibly driven by awide-angle wind, dragging the environment material along a direction close to the line of sight (i= 19◦ ). We estimate
the dynamical ages, the mass, the momentum and the energy of each individual outflow shell and those of the whole
outflow. The results are in agreement with those found in outflows from Class II sources. We make a rough estimate
for the size of the jet/wind launching region, which needs to be of ≤ 15 au. We report the physical characteristics
of DO Tauri’s disk continuum emission (almost face-on and with a projected major axis in the north-south direction)and its velocity gradient orientation (north-south), indicative of disk rotation for a 1-2 M⊙ central star. Finally weshow an HST [SII] image of the optical jet and report a measurement of its orientation in the plane of the sky.
Accepted by ApJ
https://arxiv.org/pdf/2003.01148

14. Dust depleted inner disks in a large sample of transition disks through long-baseline

ALMA observations
Logan Francis1 and Nienke van der Marel1
1

University of Victoria, Department of Physics and Astronomy, 3800 Finnerty Road, Victoria, Canada

E-mail contact: loganfrancis3 at uvic.ca
Transition disks with large inner dust cavities are thought to host massive companions. However, the disk structure
inside the companion orbit and how material flows toward an actively accreting star remain unclear. We present ahigh resolution continuum study of inner disks in the cavities of 38 transition disks. Measurements of the dust massfrom archival Atacama Large Millimeter/Submillimeter Array observations are combined with stellar properties andspectral energy distributions to assemble a detailed picture of the inner disk. An inner dust disk is detected in 18
of 38 disks in our sample. Of the 14 resolved disks, 9 are significantly misaligned with the outer disk. The nearinfrared excess is uncorrelated with the mm dust mass of the inner disk. The size-luminosity correlation known for
protoplanetary disks is recovered for the inner disks as well, consistent with radial drift. The inner disks are depleted
in dust relative to the outer disk and their dust mass is uncorrelated with the accretion rates. This is interpreted as
the result of radial drift and trapping by planets in a low α (∼ 10−3 ) disk, or a failure of the α-disk model to describe
angular momentum transport and accretion. The only disk in our sample with confirmed planets in the gap, PDS 70,
has an inner disk with a significantly larger radius and lower inferred gas-to-dust ratio than other disks in the sample.
We hypothesize that these inner disk properties and the detection of planets are due to the gap having only been
opened recently by young, actively accreting planets.
Accepted by ApJ
https://arxiv.org/pdf/2003.00079

15. Formation of single-moon systems around gas giants
Yuri I. Fujii1,2 and Masahiro Ogihara3
1

Institute for Advanced Research, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, 464-8601, Japan; 212Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, 464-8602, Japan; 3 Division of
Science, National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, 181-8588 Tokyo, Japan
E-mail contact: yuri.f at nagoya-u.jp
Several mechanisms have been proposed to explain the formation process of satellite systems, and relatively large
moons are thought to be born in circumplanetary disks. Making a single-moon system is known to be more difficult
than multiple-moon or moonless systems. We aim to find a way to form a system with a single large moon, such as
Titan around Saturn. We examine the orbital migration of moons, which change their direction and speed dependingon the properties of circumplanetary disks. We modeled dissipating circumplanetary disks with taking the effect oftemperature structures into account and calculated the orbital evolution of Titan-mass satellites in the final evolution
stage of various circumplanetary disks. We also performed N-body simulations of systems that initially had multiple
satellites to see whether single-moon systems remained at the end. The radial slope of the disk-temperature structure
characterized by the dust opacity produces a patch of orbits in which the Titan-mass moons cease inward migrationand even migrate outward in a certain range of the disk viscosity. The patch assists moons initially located in theouter orbits to remain in the disk, while those in the inner orbits fall onto the planet. We demonstrate for the firsttime that systems can form that have only one large moon around giant planet. Our N-body simulations suggest
satellite formation was not efficient in the outer radii of circumplanetary disks.
Accepted by A&A Letters
http://arxiv.org/pdf/2003.05052

16. Do subsequent outbursts of the same EXor source present similar features?
Teresa Giannini1 , Alessio Giunta2 , Dario Lorenzetti1 , Giuseppe Altavilla1,2 , Simone Antoniucci1 , Francesco
Strafella3 and Vincenzo Testa1
INAF-Osservatorio Astronomico di Roma, via Frascati 33, I-00078 Monte Porzio Catone, Italy; 2 ASI - Agenzia
Spaziale Italiana - Via del Politecnico, 00133 Roma, Italy; 3 Dipartimento di Matematica e Fisica, Universitá delSalento, 73100 Lecce, Italy
1E-mail contact: teresa.giannini at inaf.it
V1118 Ori is a classical EXor source whose light curve has been monitored over the past thirty years (although notcontinuously). It underwent a powerful outburst in 2005, followed by ten years of quiescence and a less intense outburst
in 2015. In 2019, a new intense brightness increase was observed (∆g ∼ 3 mag). This new accretion episode offers theopportunity to compare the photometric and spectroscopic properties of different outbursts of the same source. This
allows one to highlight differences and similarities among different events by removing any possible bias related tothe intrinsic properties of the star-disk system. We discovered the 2019 V1118 Ori outburst by examining the g-band
light curve acquired by the Zwicky Transient Facility and followed the decreasing phase with the Rapid Eye Mounttelescope in the griz bands. Two near-infrared spectra were also acquired at different brightness stages with the Large
Binocular Telescope. The last event shows the following characteristics: 1) amplitude similar than in 2015 and lower
than in 2005; 2) duration less than one year as in previous events; 3) rise (decline) speed of 0.018 (0.031) mag/day,which is different from previous cases; 4) a gradual blueing of the [g − r] color is observed over time, while the [r − i]color remains roughly unchanged; 5) with few exceptions, the near-infrared lines (mainly H I recombination) are thesame observed in 2015; 6) the mass accretion rate peaks at Ṁacc ∼ 10−7 M⊙ yr−1 and decreases in about a month
down to a few 10−8 M⊙ yr−1 . Our analysis shows that the comparison of data from different outbursts of the same
source is a non-trivial exercise, which allows obtaining important clues useful to drive theoretical efforts towards a
better understanding of the EXor phenomenon.
Accepted by A&A
http://arxiv.org/pdf/2003.13383

17. Giant star-forming clumps?
R.J. Ivison1 , J. Richard2 , A.D. Biggs1, M.A. Zwaan1 , E. Falgarone3 et al.
European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching, Germany; 2 Univ Lyon, Univ
Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, F-69230, Saint-Genis-Laval,
France; 3 Laboratoire de Physique de l’ENS, ENS, Université PSL, CNRS, Sorbonne Université, Université Paris1

13

Diderot, Paris, France
E-mail contact: rji at roe.ac.uk
With the spatial resolution of the Atacama Large Millimetre Array (ALMA), dusty galaxies in the distant Universe
typically appear as single, compact blobs of dust emission, with a median half-light radius, ≈1 kpc. Occasionally,strong gravitational lensing by foreground galaxies or galaxy clusters has probed spatial scales 1–2 orders of magnitude
smaller, often revealing late-stage mergers, sometimes with tantalising hints of sub-structure. One lensed galaxy inparticular, the Cosmic Eyelash at z = 2.3, has been cited extensively as an example of where the interstellar medium
exhibits obvious, pronounced clumps, on a spatial scale of ≈100 pc. Seven orders of magnitude more luminous than
giant molecular clouds in the local Universe, these features are presented as circumstantial evidence that the blue
clumps observed in many z ∼ 2–3 galaxies are important sites of ongoing star formation, with significant masses ofgas and stars. Here, we present data from ALMA which reveal that the dust continuum of the Cosmic Eyelash is infact smooth and can be reproduced using two Sérsic profiles with effective radii, 1.2 and 4.4 kpc, with no evidence ofsignificant star-forming clumps down to a spatial scale of ≈80 pc and a star-formation rate of <3 M⊙ yr−1 .
Accepted by MNRAS
http://arxiv.org/pdf/2003.07863

18. Discovery of new members of the nearby young stellar association in Cepheus
A. Klutsch1,2,4 , A. Frasca2 , P. Guillout3 , D. Montes4 , F.-X. Pineau3 et al.
Institut für Astronomie und Astrophysik, Eberhard Karls Universität, Sand 1, D-72076 Tübingen, Germany; 2 INAFOsservatorio Astrofisico di Catania, via S. Sofia 78, I-95123 Catania, Italy; 3 Observatoire Astronomique, Universitéde Strasbourg & CNRS, UMR 7550, 11 rue de l’Université, F-67000 Strasbourg, France; 4 Departamento de Física dela Tierra y Astrofísica and IPARCOS-UCM (Instituto de Física de Partículas y del Cosmos de la UCM), Facultad deCiencias Físicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain
1

E-mail contact: klutsch at astro.uni-tuebingen.de
Young field stars are hardly distinguishable from older ones because their space motion rapidly mixes them with thestellar population of the Galactic plane. Nevertheless, a careful target selection allows for young stars to be spottedthroughout the sky.
We aim to identify additional sources associated with the four young comoving stars that we discovered towards the
CO Cepheus void and to provide a comprehensive view of the Cepheus association.
Based on multivariate analysis methods, we have built an extended sample of 193 young star candidates, which are
the optical and infrared counterparts of ROSAT All-Sky Survey and XMM-Newton X-ray sources. From optical
spectroscopic observations, we measured their radial velocity with the cross-correlation technique. We derived theiratmospheric parameters and projected rotational velocity with the code ROTFIT. We applied the subtraction of
inactive templates to measure the lithium equivalent width, from which we infer their lithium abundance and age.
Finally, we studied their kinematics using the second Gaia data release.
Our sample is mainly composed of young or active stars and multiple systems. We identify two distinct populations ofyoung stars that are spatially and kinematically separated. Those with an age between 100 and 300 Myr are mostly
projected towards the Galactic plane. In contrast, 23 of the 37 sources younger than 30 Myr are located in the CO
Cepheus void, and 21 of them belong to the stellar kinematic group that we previously reported in this sky area. We
report a total of 32 bona fide members and nine candidates for this nearby (distance = 157±10 pc) young (age =10–20 Myr) stellar association. According to the spatial distribution of its members, the original cluster is alreadydispersed and partially mixed with the local population of the Galactic plane.
Accepted by A&A
http://arxiv.org/pdf/2003.12155

19. Unbiased Monte Carlo continuum radiative transfer in optically thick regions
Anton Krieger1 and Sebastian Wolf1
1

University of Kiel, Institute of Theoretical Physics and Astrophysics, Leibnizstrasse 15, 24118 Kiel, Germany

E-mail contact: akrieger at astrophysik.uni-kiel.de14

Radiative transfer describes the propagation of electromagnetic radiation through an interacting medium. This process
is often simulated by the use of the Monte Carlo method, which involves the probabilistic determination and trackingof simulated photon packages. In the regime of high optical depths, this approach encounters difficulties since a proper
representation of the various physical processes can only be achieved by considering high numbers of simulated photon
packages. As a consequence, the demand for computation time rises accordingly and thus practically puts a limiton the optical depth of models that can be simulated. Here we present a method that aims to solve the problem ofhigh optical depths in dusty media, which relies solely on the use of unbiased Monte Carlo radiative transfer. For
that end, we identified and precalculated repeatedly occuring and simulated processes, stored their outcome in a
multidimensional cumulative distribution function, and immediately replaced the basic Monte Carlo transfer during
a simulation by that outcome. During the precalculation, we generated emission spectra as well as deposited energy
distributions of photon packages traveling from the center of a sphere to its rim. We carried out a performance testof the method to confirm its validity and gain a boost in computation speed by up to three orders of magnitude. We
then applied the method to a simple model of a viscously heated circumstellar disk, and we discuss the necessity offinding a solution for the optical depth problem with regard to a proper temperature calculation. We find that the
impact of an incorrect treatment of photon packages in highly optically thick regions extents even to optically thinregions, thus, changing the overall observational appearance of the disk.
Accepted by A&A
https://www.aanda.org/articles/aa/pdf/2020/03/aa37355-19/aa37355-19.html

20. Angular Momenta, Magnetization, and Accretion of Protostellar Cores
Aleksandra Kuznetsova1 , Lee Hartmann1 , and Fabian Heitsch2
Department of Astronomy, University of Michigan, 1085 S. University Ave., Ann Arbor, MI 48109; 2 Department of
Physics and Astronomy, University of North Carolina - Chapel Hill

1

E-mail contact: kuza at umich.edu
Building on our previous hydrodynamic study of the angular momenta of cloud cores formed during gravitational
collapse of star-forming molecular gas in our previous work, we now examine core properties assuming ideal magnetohydrodynamics (MHD). Using the same sink-patch implementation for the Athena MHD code, we characterize thestatistical properties of cores, including the mass accretion rates, specific angular momenta, and alignments between
the magnetic field and the spin axis of the core on the 0.1 pc scale. Our simulations, which reproduce the observed
relation between magnetic field strength and gas density, show that magnetic fields can help collimate low density flows
and help seed the locations of filamentary structures. Consistent with our previous purely hydrodynamic simulations,stars (sinks) form within the heterogeneous environments of filaments, such that accretion onto cores is highly episodic
leading to short-term variability but no long-term monotonic growth of the specific angular momenta. With statistical characterization of protostellar cores properties and behaviors, we aim to provide a starting point for building
more realistic and self-consistent disk formation models, helping to address whether magnetic fields can prevent thedevelopment of (large) circumstellar disks in the ideal MHD limit.
Accepted by ApJ
http://arxiv.org/pdf/2003.13697

21. The disk of 2MASS 15491331−3539118 = GQ Lup C as seen by HST and WISE
C. Lazzoni1,2 , R. Gratton1 , J.M. Alcalá3 , S. Desidera1 , A. Frasca4 et al.
INAF — Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122, Padova, Italy; 2 Dipartimento di
Fisica a Astronomia “G. Galilei”, Universita’ di Padova, Via Marzolo, 8, 35121 Padova, Italy; 3 INAF — Osservatorio
Astronomico di Capodimonte, Salita Moiariello 16, 80131 Napoli, Italy; 4 INAF — Osservatorio Astronomico di
Catania, Via Santa Sofia, 78, Catania, Italy
1E-mail contact: cecilia.lazzoni at inaf.it
Very recently, a second companion on wider orbit has been discovered around GQ Lup. This is a low-mass accretingstar partially obscured by a disk seen at high inclination. If detected, this disk may be compared to the known disk
around the primary. We detected this disk on archive HST and WISE data. The extended spectral energy distribution
provided by these data confirms the presence of accretion from Hα emission and UV excess, and shows an IR excess
15attributable to a warm disk. In addition, we resolved the disk on the HST images. This is found to be roughly alignedwith the disk of the primary. Both of them are roughly aligned with the Lupus I dust filament containing GQ Lup.
Accepted by A&A
http://arxiv.org/pdf/2003.00743

22. Most Stars (and Planets?) Are Born in Intense Radiation Fields
Eve J. Lee1,2 & Philip F. Hopkins1
TAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USA; 2 Department of Physics
and McGill Space Institute, McGill University, 3550 rue University, Montreal, QC, H3A 2T8, Canada

1E-mail contact: evelee at physics.mcgill.ca
Protostars and young stars are strongly spatially “clustered” or “correlated” within their natal giant molecular clouds(GMCs). We demonstrate that such clustering leads to the conclusion that the incident bolometric radiative flux upona random young star/disc is enhanced (relative to volume-averaged fluxes) by a factor which increases with the total
stellar mass of the complex. Because the Galactic cloud mass function is top-heavy, the typical star in our Galaxy
experienced a much stronger radiative environment than those forming in well-observed nearby (but relatively small)clouds, exceeding fluxes in the Orion Nebular Cluster by factors of >∼30. Heating of the circumstellar disc arounda median young star is dominated by this external radiation beyond ∼50AU. And if discs are not well-shielded byambient dust, external UV irradiation can dominate over the host star down to sub-AU scales. Another consequenceof stellar clustering is an extremely broad Galaxy-wide distribution of incident flux (spanning >10 decades), with half
the Galactic star formation in a substantial “tail” towards even more intense background radiation. We also showthat the strength of external irradiation is amplified super-linearly in high-density environments such as the Galactic
centre, starbursts, or high-redshift galaxies.
Accepted by MNRAS Letters
http://arxiv.org/pdf/2003.03390

23. ALMA observations of NGC 6334S − I:

Forming massive stars and cluster in subsonic and transonic filamentary clouds
Shanghuo Li1,2,3 , Qizhou Zhang2 , Hauyu Baobab Liu4 , Henrik Beuther5 , Aina Palau6 , Josep Miquel.
Girart7 , Howard Smith2 , Joseph L. Hora2 , Yuxing Lin8 , Keping Qiu9 , Shaye Strom2 , Junzhi Wang1 ,Fei Li1,3 and Nannan Yue3,10
Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China; 2Center for Astrophysics, Harvard & Smithsonian , 60 Garden Street, Cambridge, MA 02138, USA; 3 University ofChinese Academy of Sciences, 19A Yuquanlu, Beijing 100049, China; 4 Academia Sinica Institute of Astronomy andAstrophysics, P.O. Box 23-141, Taipei 106, Taiwan; 5 Max Planck Institute for Astronomy, Konigstuhl 17, 69117
Heidelberg, Germany; 6 Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, P.O.
Box 3-72, 58090, Morelia, Michoacán, México; 7 Institut de Ciències de l’Espai (IEEC-CSIC), Campus UAB, Carrer
de Can Magrans s/n, 08193 Cerdanyola del Vallès, Catalonia, Spain; 8 Max-Planck Institute für Radio Astronomy,
Auf dem Hügel 69, 53121, Bonn, Germany; 9 School of Astronomy and Space Science, Nanjing University, 163 Xianlin
Avenue, Nanjing 210023, China; 10 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012
1

E-mail contact: shanghuo.li at gmail.com
We present Atacama Large Millimeter/submillimeter Array (ALMA) and Karl G. Jansky Very Large Array (JVLA)
observations of the massive infrared dark cloud NGC 6334S (also known as IRDC G350.56+0.44), located at thesouthwestern end of the NGC 6334 molecular cloud complex. The H13 CO+ and the NH2 D lines covered by the ALMA
observations at a ∼3 arcsec angular resolution (∼0.02 pc) reveal that the spatially unresolved non-thermal motions
are predominantly subsonic and transonic, a condition analogous to that found in low-mass star-forming molecular
clouds. The observed supersonic non-thermal velocity dispersions in massive star forming regions, often reported in
the literature, might be significantly biased by poor spatial resolutions that broaden the observed line widths due tounresolved motions within the telescope beam. Our 3 mm continuum image resolves 49 dense cores, whose masses
range from 0.17 to 14 M⊙ . The majority of them are resolved with multiple velocity components. Our analyses ofthese gas velocity components find an anti-correlation between the gas mass and the virial parameter. This implies16that the more massive structures tend to be more gravitationally unstable. Finally, we find that the external pressurein the NGC 6334S cloud is important in confining these dense structures, and may play a role in the formation ofdense cores, and subsequently, the embedded young stars.
Accepted by ApJ
https://arxiv.org/pdf/2003.13534

24. Planet-induced Vortices with Dust Coagulation in Protoplanetary Disks
Ya-Ping Li1 , Hui Li1 , Shengtai Li1 , Tilman Birnstiel2,3 , Joanna Dra̧żkowska2 and Sebastian Stammler2
Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA; 2 University Observatory, Faculty of Physics, Ludwig-Maximilians-Universität München, Scheinerstr. 1, 81679 Munich, Germany; 3 Exzellenzcluster
ORIGINS, Boltzmannstr. 2, D-85748 Garching, Germany
1E-mail contact: leeyp2009 at gmail.com
In this work, we study how the dust coagulation/fragmentation will influence the evolution and observational appearances of vortices induced by a massive planet embedded in a low viscosity disk by performing global 2D high-resolutionhydrodynamical simulations. Within the vortex, due to its higher gas surface density and steeper pressure gradients,
dust coagulation, fragmentation and drift (to the vortex center) are all quite efficient, producing dust particles ranging
from micron to ∼1.0 cm, as well as overall high dust-to-gas ratio (above unity). In addition, the dust size distribution
is quite non-uniform inside the vortex, with the mass weighted average dust size at the vortex center (∼4.0 mm) beinga factor of ∼10 larger than other vortex regions. Both large (∼mm) and small (tens of micron) particles contributestrongly to affect the gas motion within the vortex. As such, we find that the inclusion of dust coagulation has asignificant impact on the vortex lifetime and the typical vortex lifetime is about 1000 orbits. After the initial gaseous
vortex is destroyed, the dust spreads into a ring with a few remaining smaller gaseous vortices with a high dust concentration and a large maximum size (∼mm). At late time, the synthetic dust continuum images for the coagulationcase show as a ring inlaid with several hot spots at 1.33 mm band, while only distinct hot spots remain at 7.0 mm.
Accepted by ApJL
http://arxiv.org/pdf/2003.06522

25. Discovery of two nearby post-T Tauri stellar associations
Jiaming Liu1 , Min Fang2 , and Chao Liu3,4
1

Key Lab of Optical Astronomy, National Astronomical Observatories, CAS, Beijing 100101, China; 2 Department of
Astronomy, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA; 3 Key Lab of Space Astronomy
and Technology, National Astronomical Observatories, CAS, Beijing, 100101, China; 4 University of Chinese Academyof Sciences, Beijing 100049, China
E-mail contact: liuchao at nao.cas.cn
In this work we report the discovery of 2 new stellar associations in close vicinity of the Sun at roughly 180 and
150 pc. These two associations, named as u Tau assoc and e Tau assoc, were detected based on their clustering ina multi-dimensional parameter space including α, δ, µα , µδ and ̟ of Gaia. The fitting of pre-main-sequence model
isochrones in their color-magnitude diagrams suggests that the two associations are of about 50 Myr old and the groupmembers lower than ∼0.8 M⊙ are at the stage of post-T Tauri.
Accepted by AJ

http://arxiv.org/pdf/2003.11725

26. The nature of a primary jet within a circumbinary disc outflow in a young stellar system
Chris Lynch1 and Michael D. Smith1
1

Centre for Astrophysics & Planetary Science, The University of Kent, Canterbury, Kent CT2 7NH, U.K

E-mail contact: m.d.smith at kent.ac.uk
Most stars form in binaries, and both stars may grow by accreting material from a circumbinary disc onto their own

17

discs. We suspect that in many cases a wide molecular wind will envelope a collimated atomic jet emanating from close
to an orbiting young star. This so-called Circumbinary Scenario is explored here in order to find common identifiable
properties. The dynamical set up is studied with three dimensional simulations with chemistry and cooling included.
We extract the properties on scales of order 100 AU and compare to the Co-Orbital Scenario in which the wind and jet
sources are in orbit. We find that the rapid orbital motion generates a wide ionised sheath around the jet core with alarge opening angle at the base. This is independent of the presence of the surrounding molecular outflow. However,
the atomic jet is recollimated beyond ∼ 55 AU when the molecular outflow restricts the motion of the ambient medium
which, in turn, confines the jet. These physical properties are related to the optical Hα imaging, providing a means ofdistinguishing between models. The high excitation sheath and recollimation region can be explored on these scales
through the next generation of instruments. However, in general, the amount and location of the ionised material,
whether in the knots or the sheath, will depend on several parameters including the orbital period, axis alignment andpulse amplitude.
Accepted by Monthly Notices of the Royal Astronomical Society
http://arxiv.org/pdf/2003.01806

27. Different Modes of Star Formation II: Gas Accretion Phase of Initially Subcritical Star-

Forming Clouds

Masahiro N. Machida1,2 and Shantanu Basu2
1

Department of Earth and Planetary Sciences, Faculty of Sciences, Kyushu University, Fukuoka, Fukuoka 819-0395,
Japan; 2 Department of Physics and Astronomy, The University of Western Ontario, London, ON N6A 3K7, Canada
E-mail contact: machida.masahiro.018 at m.kyushu-u.ac.jp
The accretion phase of star formation is investigated in magnetically-dominated clouds that have an initial subcriticalmass-to-flux ratio. We employ nonideal magnetohydrodynamic simulations that include ambipolar diffusion and ohmic
dissipation. During the early prestellar phase the mass-to-flux ratio rises toward the critical value for collapse, andduring this time the angular momentum of the cloud core is reduced significantly by magnetic braking. Once a protostar
is formed in the core, the accretion phase is characterized by the presence of a small amount of angular momentum
but a large amount of magnetic flux in the near-protostellar environment. The low angular momentum leads to avery small (or even nonexistent) disk and weak outflow, while the large magnetic flux can lead to an interchange
instability that rapidly removes flux from the central region. The effective magnetic braking in the early collapse
phase can even lead to a counter-rotating disk and outflow, in which the rotation direction of the disk and outflow is
opposite to that of the infalling envelope. The solutions with a counter-rotating disk, tiny disk, or nonexistent disk
(direct collapse) are unique outcomes that are realized in collapse from magnetically-dominated clouds with an initialsubcritical mass-to-flux ratio.
Accepted by MNRAS
https://arxiv.org/pdf/2003.03078

28. Distribution of Water Vapor in Molecular Clouds. II
Gary J. Melnick1 , Volker Tolls1 , Ronald L. Snell2 , Michael J. Kaufman3 , Edwin A. Bergin4 et al.
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 66, Cambridge, MA 02138, USA; 2 Dept ofAstronomy, University of Massachusetts, Amherst, MA 01003, USA; 3 Dept of Physics and Astronomy, San José State
University, San Jose, CA 95192, USA; 4 Dept of Astronomy, The University of Michigan, 500 Church Street, Ann
Arbor, MI 48109, USA
1E-mail contact: vtolls at cfa.harvard.edu
The depth-dependent abundance of both gas-phase and solid-state water within dense, quiescent, molecular clouds isimportant to both the cloud chemistry and gas cooling. Where water is in the gas phase, it’s free to participate in
the network of ion-neutral reactions that lead to a host of oxygen-bearing molecules, and its many ortho and para
energy levels make it an effective coolant for gas temperatures greater than 20 K. Where water is abundant as ice
on grain surfaces, and unavailable to cool the gas, significant amounts of oxygen are removed from the gas phase,suppressing the gas-phase chemical reactions that lead to a number of oxygen-bearing species, including O2 . Models

18

of FUV-illuminated clouds predict that the gas-phase water abundance peaks in the range AV ∼ 3 and 8 mag of thecloud surface, depending on the gas density and FUV field strength. Deeper within such clouds, water is predicted
to exist mainly as ice on grain surfaces. More broadly, these models are used to analyze a variety of other regions,
including outflow cavities associated with young stellar ob

29.

30.

31. Deciphering the 3-D Orion Nebula-I: Expanding Shells in the Huygens Region
C. R. O’Dell1 and N. P. Abel2
1

Vanderbilt University; 2 Clermont College, University of Cincinnati; 3 University of Kentucky

E-mail contact: N71932 at comcast.net
Based on imaging and spectroscopic data, we develop a 3-D model for the Huygens Region of the Orion Nebula.
θ1 Ori C, the hottest star in the Trapezium, is surrounded by a wind-blown Central Bubble that opens SW into the
Extended Orion Nebula. Outside of this feature lies a layer of ionized gas at about 0.4 pc from θ1 Ori C. Both of thesefeatures are moving rapidly away from θ1 Ori C with an expansion age for the Central Bubble of only 15,000 yrs.
Accepted by Astrophysical Journal
http://arxiv.org/pdf/2003.01840

32. Census of young stellar population in the Galactic H II region Sh2-242
Alik Panja1 , Soumen Mondal1 , Somnath Dutta2 , Santosh Joshi3 , Sneh Lata3 et al.
1
S.N. Bose National Centre for Basic Sciences, Kolkata 700106, India; 2 Institute of Astronomy and Astrophysics,
Academia Sinica, Taipei 10617, Taiwan; 3 Aryabhatta Research Institute of Observational Sciences, Nainital 263002,
India

E-mail contact: alik.panja at gmail.com
We present here identification and characterization of the young stellar population associated with an active starforming site Sh2-242. We used our own new optical imaging and spectroscopic observational data, as well as several
archival catalogs, e.g., Pan-STARRS 1, Gaia DR2, IPHAS, WIRCam, 2MASS, and Spitzer. Slit spectroscopic results
confirm the classification of the main ionizing source BD+26 980 as an early-type star of spectral type B0.5 V. The
spectrophotometric distance of the star is estimated as 2.08±0.24 kpc, which confirms the source as a member of thecluster. An extinction map covering a large area (diameter ∼50′ ) is generated with H and K photometry toward theregion. From the map, three distinct locations of peak extinction complexes (AV ≈ 7–17 mag) are identified for thevery first time. Using the infrared color excess, a total of 33 Class I and 137 Class II young objects are classified
within the region. The IPHAS photometry reveals classification of 36 Hα emitting sources, which might be class II
objects. Among 36 Hα emitting sources, 5 are already identified using infrared excess emission. In total, 201 young
objects are classified toward S242 from this study. The membership status of the young sources is further windowedwith the inclusion of parallax from the Gaia DR2 catalog. Using the optical and infrared color-magnitude diagrams,
the young stellar objects are characterized with an average age of ∼1 Myr and the masses in the range 0.1–3.0 M⊙ .
The census of the stellar content within the region is discussed using combined photometric and spectroscopic data.
Accepted by AJ
http://arxiv.org/pdf/2003.09581

33. A Semi-Automated Computational Approach for Infrared Dark Cloud Localization: A

Catalog of Infrared Dark Clouds
Jyothish Pari1 and Joseph L. Hora1

1

Center for Astrophysics | Harvard & Smithsonian, 60 Garden St, MS-65, Cambridge, MA 02138-1516 USA

E-mail contact: jhora at cfa.harvard.edu
The field of computer vision has greatly matured in the past decade, and many of the methods and techniques canbe useful for astronomical applications. One example is in searching large imaging surveys for objects of interest,
especially when it is difficult to specify the characteristics of the objects being searched for. We have developed amethod using contour finding and convolution neural networks (CNNs) to search for Infrared Dark Clouds (IRDCs)
in the Spitzer Galactic plane survey data. IRDCs can vary in size, shape, orientation, and optical depth, and areoften located near regions with complex emission from molecular clouds and star formation, which can make the
IRDCs difficult to reliably identify. False positives can occur in regions where emission is absent, rather than froma foreground IRDC. The contour finding algorithm we implemented found most closed figures in the mosaic and we20

developed rules to filter out some of the false positive before allowing the CNNs to analyze them. The method wasapplied to the Spitzer data in the Galactic plane surveys, and we have constructed a catalog of IRDCs which includes
additional parts of the Galactic plane that were not included in earlier surveys.
Accepted by PASP
https://arxiv.org/pdf/2003.01122

34. Molecular clumps disguising their star formation efficiency per freefall time: What we

can do not to be fooled
Geneviève Parmentier1
1

Astronomisches Rechen-Institut, Zentrum für Astronomie Heidelberg, Germany

E-mail contact: gparm at ari.uni-heidelberg.de
The presence of a volume density gradient in molecular clumps allow them to raise their star formation rate compared
to what they would experience were their gas uniform in density. This higher star formation rate yields in turn ahigher value for the star formation efficiency per freefall time that we measure. The measured star formation efficiency
per freefall time ǫff,meas of clumps is therefore plagued by a degeneracy, as two factors contribute to it: one is thedensity gradient of the clump gas, the other is the intrinsic star formation efficiency per freefall time ǫff,int with which
the clump would form stars should there be no gas density gradient. This paper presents a method allowing one torecover the intrinsic efficiency of a centrally-concentrated clump. It hinges on the relation between the surface densities
in stars and gas measured locally from clump center to clump edge. Knowledge of the initial density profile of theclump gas is not required. A step-by-step description of the method is provided as a tool in hand for observers. Once
ǫff,int has been estimated, it can be compared with its measured, clump-averaged, counterpart ǫff,meas to quantify the
impact that the initial gas density profile of a clump has had on its star formation history.
Accepted by ApJ
https://arxiv.org/pdf/2003.01613

35. Do fragmentation and accretion affect the stellar Initial Mass Function?
R. Riaz1 , D.R.G. Schleicher1 , S. Vanaverbeke2 , Ralf S. Klessen3,4
1
Departamento de Astronomía, Facultad Ciencias Físicas y Matemáticas, Universidad de Concepción, Av. Esteban
Iturra s/n Barrio Universitario, Casilla 160-C, Concepción, Chile; 2 Centre for mathematical Plasma-Astrophysics,
Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Heverlee, Belgium; 3 Universität Heidelberg,
Zentrum für Astronomie, Institut für Theoretische Astrophysik, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany; 4
Universität Heidelberg, Interdisziplinäres Zentrum für Wissenschaftliches Rechnen, Im Neuenheimer Feld 205, 69120
Heidelberg, Germany

E-mail contact: rriaz at astro-udec.cl
While the stellar Initial Mass Function (IMF) appears to be close to universal within the Milky Way galaxy, it isstrongly suspected to be different in the primordial Universe, where molecular hydrogen cooling is less efficient andthe gas temperature can be higher by a factor of 30. In between these extreme cases, the gas temperature varies
depending on the environment, metallicity and radiation background. In this paper we explore if changes of thegas temperature affect the IMF of the stars considering fragmentation and accretion. The fragmentation behavior
depends mostly on the Jeans mass at the turning point in the equation of state where a transition occurs from anapproximately isothermal to an adiabatic regime due to dust opacities. The Jeans mass at this transition in theequation of state is always very similar, independent of the initial temperature, and therefore the initial mass of thefragments is very similar. Accretion on the other hand is strongly temperature dependent. We argue that the latterbecomes the dominant process for star formation efficiencies above 5–7%, increasing the average mass of the stars.
Accepted by MNRAS
http://arxiv.org/pdf/2003.07639

2136. Dust dynamics and vertical settling in gravitoturbulent protoplanetary discs
A. Riols1 , B. Roux1 , H. Latter2 , G. Lesur1
Univ. Grenoble Alpes, CNRS, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG), F-38000, Grenoble,
France; 2 DAMTP, University of Cambridge, Centre for Mathematical Sciences, Wilberforce Road, Cambridge CB30WA, UK1

E-mail contact: antoine.riols at univ-grenoble-alpes.fr
Gravitational instability (GI) controls the dynamics of young massive protoplanetary discs. Apart from facilitating
gas accretion on to the central protostar, it must also impact on the process of planet formation: directly throughfragmentation, and indirectly through the turbulent concentration of small solids. To understand the latter process,it is essential to determine the dust dynamics in such a turbulent flow. For that purpose, we conduct a series of
3D shearing box simulations of coupled gas and dust, including the gas’s self-gravity and scanning a range of Stokes
numbers, from 0.001 to ∼0.2. First, we show that the vertical settling of dust in the midplane is significantly impededby gravitoturbulence, with the dust scale-height roughly 0.6 times the gas scale height for centimetre grains. This isa result of the strong vertical diffusion issuing from (a) small-scale inertial-wave turbulence feeding off the GI spiralwaves and (b) the larger-scale vertical circulations that naturally accompany the spirals. Second, we show that at
R = 50 AU concentration events involving sub-metre particles and yielding order 1 dust to gas ratios are rare and last
for less than an orbit. Moreover, dust concentration is less efficient in 3D than in 2D simulations. We conclude that
GI is not especially prone to the turbulent accumulation of dust grains. Finally, the large dust scale-height measured
in simulations could be, in the future, compared with that of edge-on discs seen by ALMA, thus aiding detection andcharacterisation of GI in real systems.
Accepted by MNRAS
http://arxiv.org/pdf/2003.01167

37. Disk structure around the Class I protostar L1489 IRS revealed by ALMA: a warped

disk system

Jinshi Sai1,2,3 , Nagayoshi Ohashi2,3 , Kazuya Saigo4 , Tomoaki Matsumoto5 , Yusuke Aso3,6 , Shigehisa
Takakuwa3,7 , Yuri Aikawa1 , Ippei Kurose1 , Hsi-Wei Yen3 , Kohji Tomisaka8 , Kengo Tomida9 and Masahiro
N. Machida10
Department of Astronomy, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo
113-0033, Japan; 2 Subaru Telescope, National Astronomical Observatory of Japan, 650 North A’ohoku Place, Hilo, HI
96720, USA; 3 Academia Sinica Institute of Astronomy and Astrophysics, 11F of Astro-Math Bldg, 1, Sec 4., Roosevelt
Rd, Taipei 10617, Taiwan; 4 Chile Observatory, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka,
Tokyo 181-8588, Japan; 5 Faculty of Humanity and Environment, Hosei University, Fujimi, Chiyoda-ku, Tokyo 1028160, Japan; 6 Korea Astronomy and Space Science Institute (KASI), 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055,
Republic of Korea; 7 Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima
University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065, Japan; 8 National Astronomical Observatory of Japan,
Osawa, 2-21-1, Mitaka, Tokyo 181-8588, Japan; 9 Department of Earth and Space Science, Osaka University, Toyonaka,
Osaka 560-0043, Japan; 10 Department of Earth and Planetary Sciences, Faculty of Sciences, Kyushu University,
Fukuoka, Fukuoka 819-0395, Japan1

E-mail contact: jsai at asiaa.sinica.edu.tw
We have observed the Class I protostar L1489 IRS with the Atacama Millimeter/submillimeter Array (ALMA) in
Band 6. The C18 O J =2–1 line emission shows flattened and non-axisymmetric structures in the same direction as its
velocity gradient due to rotation. We discovered that the C18 O emission shows dips at a radius of ∼200–300 au whilethe 1.3 mm continuum emission extends smoothly up to r ∼ 400 au. At the radius of the C18 O dips, the rotational
axis of the outer portion appears to be tilted by ∼15◦ from that of the inner component. Both the inner and outercomponents with respect to the C18 O dips exhibit the r−0.5 Keplerian rotation profiles until r ∼ 600 au. These results
not only indicate that a Keplerian disk extends up to ∼600 au but also that the disk is warped. We constructed athree dimensional warped disk model rotating at the Keplerian velocity, and demonstrated that the warped disk model
reproduces main observed features in the velocity channel maps and the PV diagrams. Such a warped disk system
can form by mass accretion from a misaligned envelope. We also discuss a possible disk evolution scenario based on
22comparisons of disk radii and masses between Class I and Class II sources.
Accepted by ApJ
https://arxiv.org/pdf/2003.07067.pdf

38. Tidal and general relativistic effects in rocky planet formation at the substellar mass

limit using N-body simulations

Mariana B. Sánchez1,2 , Gonzalo C. de Elía1,2 and Juan J. Downes3
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N (1900),
La Plata, Argentina; 2 Instituto de Astrofísica de La Plata, CCT La Plata-CONICET-UNLP, Paseo del Bosque S/N(1900), La Plata, Argentina; 3 Centro Universitario Regional del Este, Universidad de la República, AP 264, Rocha
27000, Uruguay
1E-mail contact: msanchez at fcaglp.unlp.edu.ar
Recent observational results show that very low mass stars and brown dwarfs are able to host close-in rocky planets.
Low-mass stars are the most abundant stars in the Galaxy and the formation efficiency of their planetary systems isrelevant in the computation of a global probability of finding Earth-like planets inside habitable zones. Tidal forces
and relativistic effects are relevant in the latest dynamical evolution of planets around low-mass stars and their effecton the planetary formation efficiency still needs to be addressed. Our goal is to evaluate the impact of tidal forces
and relativistic effects on the formation of rocky planets around a star close to the substellar mass limit, in termsof the resulting planetary architectures and its distribution according to the corresponding evolving habitable zone.
Thus, we performed a set of N-body simulations spanning the first 100 Myr of the evolution of two systems composed
respectively by 224 embryos with a total mass 0.25 M⊕ and 74 embryos with a total mass 3 M⊕ around a central
object of 0.08 M⊙ . For these two scenarios, we compared the planetary architectures that result from simulations
that are purely gravitational with those from simulations that include the early contraction and spin-up of the central
object, the distortions and dissipation tidal terms and general relativistic effects. We found that including these effects
allows the formation and survival of a close-in population located in the habitable zone of the system. This meansthat both effects are relevant during the formation of rocky planets and their early evolution around stars close to thesubstellar mass limit, in particular when low-mass planetary embryos are involved.
Accepted by Astronomy and Astrophysics
https://arxiv.org/pdf/2003.07509

39. On the structure and mass delivery towards circumplanetary discs
Matthäus Schulik1 , Anders Johansen1 , Bertram Bitsch2 , Elena Lega3 , Michiel Lambrechts1
1
Lund Observatory, Box 43, Sölvegatan 27, SE-22100 Lund, Sweden; 2 Max-Planck Institut für Astronomie, Königsstuhl
17, 69117 Heidelberg, Germany; 3 Laboratoire Lagrange, UMR7293, Université de la Côte d’Azur, Boulevard de laObservatoire, 06304 Nice Cedex 4, France

E-mail contact: schulik at astro.lu.se
Circumplanetary discs (CPDs) form around young gas giants and are thought to be the sites of moon formation as wellas an intermediate reservoir of gas that feeds the growth of the gas giant. How the physical properties of such CPDs
are affected by the planetary mass and the overall opacity is relatively poorly understood. In order to clarify this, we
use the global radiation hydrodynamics code FARGOCA, with a grid structure that allows resolving the planetarygravitational potential sufficiently well for a CPD to form. We then study the gas flows and density/temperature
structures that emerge as a function of planet mass, opacity and potential depth. Our results indicate interesting
structure formation for Jupiter-mass planets at low opacities, which we subsequently analyse in detail. Using an
opacity level that is 100 times lower than that of ISM dust, our Jupiter-mass protoplanet features an envelope thatis sufficiently cold for a CPD to form, and a free-fall region separating the CPD and the circumstellar disc emerges.
Interestingly, this free-fall region appears to be a result of supersonic erosion of outer envelope material, as opposed tothe static structure formation that one would expect at low opacities. Our analysis reveals that the planetary spiralarms seem to pose a significant pressure barrier that needs to be overcome through radiative cooling in order for gas tofree-fall onto the CPD. The circulation inside the CPD is near-keplerian and modified by the presence of CPD spiral23

arms. For high opacities we recover results from the literature, finding an essentially featureless hot envelope. With
this work, we demonstrate the first simulation and analysis of a complete detachment process of a protoplanet fromits parent disc in a 3D radiation hydrodynamics setting.
Accepted by A&A
http://arxiv.org/pdf/2003.13398

40. Effects of scattering, temperature gradients, and settling on the derived dust propertiesof observed protoplanetary disks
Anibal Sierra1 & Susana Lizano1

1

Instituto de Radioastronomía y Astrofísica, UNAM, Apartado Postal 3-72, 58089 Morelia Michoacán, México

E-mail contact: a.sierra at irya.unam.mx
It is known that the millimeter dust thermal emission of protoplanetary disks is affected by scattering, such thatfor optically thick disks the emission decreases with respect to the pure absorption case and the spectral indices canreach values below 2. The latter can also be obtained with temperature gradients. Using simple analytical models ofradiative transfer in thin slabs, we quantify the effect of scattering, vertical temperature gradients, and dust settlingon the emission and spectral indices of geometrically thin face-on accretion disks around young stars. We find that invertically isothermal disks with large albedo (ων >∼ 0.6), the emergent intensity can increase at optical depths between
10−2 and 10−1 . We show that dust settling has important effects on the spectral indices in the optically thick regime,
since the disk emission mainly traces small dust grains in the upper layers of the disk. The λ=870 µm emission ofthese small grains can hide large grains at the disk mid plane when the dust surface density is larger than ∼3.21 g
cm−2 . Finally, because of the change of the shape of the spectral energy distribution, optically thick disks at 1.3 mm
and grains with sizes between 300 µm < amax < 1 mm have a 7 mm flux ∼60% higher than the extrapolation fromhigher millimeter frequencies, assumed when scattering is neglected. This effect could provide an explanation to theexcess emission at λ=7 mm reported in several disks.
Accepted by ApJ
http://arxiv.org/pdf/2003.02982

41. Chandra Resolves the Double FU Orionis System RNO 1B/1C in X-rays
Stephen L. Skinner1 and Manuel Güdel2
Center for Astrophysics and Space Astronomy (CASA), Univ. of Colorado, Boulder, CO, USA 80309-0389; 2 Dept.
of Astrophysics, Univ. of Vienna, Türkenschanzstr. 17, A-1180 Vienna, Austria

1E-mail contact: stephen.skinner at colorado.edu
We present new Chandra X-ray observations of the close pair of young stars RNO 1B and 1C (6′′ separation) locatedin the L1287 cloud. RNO 1B erupted in 1978–1990 and is classified as an FU Orionis star (FUor). RNO 1C also
shows most of the properties of an FUor but no eruption has yet been seen. Only a few dozen FUors are known andthe presence of two such objects with a small angular separation is rare, suggesting a common origin. Both stars
were faintly detected by Chandra and we summarize their X-ray properties within the framework of other previously
detected FUors. We also report other X-ray detections in L1287 including the deeply-embedded young star RNO
1G, the jet-like radio source VLA 3, and an enigmatic hard flaring source with no 2MASS counterpart that was only
detected in the second of two Chandra exposures.
Accepted by AJ
http://arxiv.org/pdf/2003.07944

42. Local Molecular Gas toward the Aquila Rift Region
Yang Su1 , Ji Yang1,2 , Qing-zeng Yan1 , Yan Gong1,3 , Zhiwei Chen1 et al.
1

Purple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, Nanjing24210034, China; 2 School of Astronomy and Space Science, University of Science and Technology of China, 96 JinzhaiRoad, Hefei 230026, China
E-mail contact: yangsu at pmo.ac.cn
×+02M⊙ )
We present the results of a ∼250 square degrees CO mapping (+26◦ < l < +50◦ and −5◦ < b < +5◦ ) toward theAquila Rift region at a spatial resolution of ∼50′′ and a grid spacing of 30′′ . The high dynamic range CO maps with aspectral resolution of ∼0.2 km s−1 display highly structured molecular cloud (MC) morphologies with valuable velocity
information, revealing complex spatial and dynamical features of the local molecular gas. In combination with the
MWISP CO data and the Gaia DR2, distances of the main MC structures in the local ISM are well determined toward
the Aquila Rift. We find that the total MC mass within 1 kpc is about >4.1 × 105 M⊙ in the whole region. In fact, themass of the molecular gas is dominated by the W40 giant molecular cloud (GMC) at ∼474 pc (∼1.4 × 105 M⊙ ) andthee 1.1adomplex t8M3643.

44. Collision between Molecular Clouds I. The effect of the cloud virial ratio in head-on

collisions
Tabassum S Tanvir1,2 , James E Dale2
Research School of Astronomy and Astrophysics, The Australian National University, Cotter Rd, Weston Creek, ACT 2611, Australia; 2 Centre for Astrophysics Research, University of Hertfordshire, College Lane, AL10 9AB,
Hatfield, UK
1E-mail contact: tabassum.tanvir at anu.edu.au
In a series of papers we investigate the effect of collisions between turbulent molecular clouds on their structure,
evolution and star formation activity. In this paper we look into the role of the clouds’ initial virial ratios. Threedifferent scenarios were examined: both clouds initially bound, one cloud bound and one unbound, and both clouds
initially unbound. Models in which one or both clouds are bound generate filamentary structures aligned along thecollision axis and discernible in position-position and position–velocity space. If neither cloud is bound, no filaments
result. Unlike in previous simulations of collisions between smooth clouds, owing to the substructure created in theclouds by turbulence before the collisions, dissipation of kinetic energy by the collision is very inefficient and in noneof our simulations is sufficient bulk kinetic energy lost to render the clouds bound. Simulations where both clouds arebound created twice as much stellar mass than the bound-unbound model, and both these scenarios produced much
more stellar mass than the simulation in which both clouds are unbound. Each simulation was also compared with acontrol run in which the clouds do not collide. We find the bound-bound collision increases the overall star formation
efficiency by a factor of approximately two relative to the control, but that the bound-unbound collision produces amuch smaller increase, and the collision has very little effect on the unbound–unbound cloud collision.
Accepted by MNRAS
http://arxiv.org/pdf/2003.05010

45. Physical Conditions and Kinematics of the Filamentary Structure in Orion Molecular

Cloud 1

Yu-Hsuan Teng1,2,3 and Naomi Hirano1
1

Institute of Astronomy and Astrophysics, Academia Sinica, 11F of Astronomy-Mathematics Building, National
Taiwan University, No.1, Sec.4, Roosevelt Rd., Taipei 10617, Taiwan; 2 Department of Physics, National Taiwan University, No.1, Sec.4, Roosevelt Rd., Taipei 10617, Taiwan; 3 Center for Astrophysics and Space Sciences, Departmentof Physics, University of California San Diego, 9500 Gilman Drive, La Jolla, CA 92093, USA
E-mail contact: yuteng at ucsd.edu
We have studied the structure and kinematics of the dense molecular gas in the Orion Molecular Cloud 1 (OMC1)
region with the N2 H+ 3–2 line. The 6′ × 9′ (∼ 0.7 × 1.1 pc) region surrounding the Orion KL core has been mappedwith the Submillimeter Array (SMA) and the Submillimeter Telescope (SMT). The combined SMA and SMT image
having a resolution of ∼ 5.4′ (∼ 2300 au) reveals multiple filaments with a typical width of 0.02–0.03 pc. On the basisof the non-LTE analysis using the N2 H+ 3–2 and 1–0 data, the density and temperature of the filaments are estimatedto be ∼ 107 cm−3 and ∼ 15–20 K, respectively. The core fragmentation is observed in three massive filaments, oneof which shows the oscillations in the velocity and intensity that could be the signature of core-forming gas motions.
The gas kinetic temperature is significantly enhanced in the eastern part of OMC1, likely due to the external heatingfrom the high mass stars in M42 and M43. In addition, the filaments are colder than their surrounding regions,suggesting the shielding from the external heating due to the dense gas in the filaments. The OMC1 region consistsof three sub-regions, i.e. north, west, and south of Orion KL, having different radial velocities with sharp velocity
transitions. There is a north-to-south velocity gradient from the western to the southern regions. The observed
velocity pattern suggests that dense gas in OMC1 is collapsing globally toward the high-mass star-forming region,
Orion Nebula Cluster.
Accepted by ApJ
https://arxiv.org/pdf/2003.02459.pdf

26

46. Scattering-induced intensity reduction: large mass content with small grains in the

inner region of the TW Hya disk

Takahiro Ueda1 , Akimasa Kataoka1 and Takashi Tsukagoshi11National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan

E-mail contact: takahiro.ueda at nao.ac.jp
Dust continuum observation is one of the best methods to constrain the properties of protoplanetary disks. Recent
theoretical studies have suggested that the dust scattering at the millimeter wavelength potentially reduces the observed
intensity, which results in an underestimate in the dust mass. We investigate whether the dust scattering indeed reduces
the observed continuum intensity by comparing the ALMA archival data of the TW Hya disk at Band 3, 4, 6, 7 and 9
to models obtained by radiative transfer simulations. We find that the model with scattering by 300 µm-sized grains
well reproduces the observed SED of the central part of the TW Hya disk while the model without scattering is also
consistent within the errors of the absolute fluxes. To explain the intensity at Band 3, the dust surface density needs
to be ∼10 g cm−2 at 10 au in the model with scattering, which is 26 times more massive than previously predicted.
The model without scattering needs 2.3 times higher dust mass than the model with scattering because it needs lower
temperature. At Band 7, scattering reduces the intensity by ∼35% which makes the disk looks optically thin eventhough it is optically thick. Our study suggests the TW Hya disk is still capable of forming cores of giant planets at
where the current solar system planets exist.
Accepted by ApJ
http://arxiv.org/pdf/2003.09353

47. ALMA 0.88 mm Survey of Disks around Planetary-mass Companions
Ya-Lin Wu1 , Brendan P. Bowler1 , Patrick D. Sheehan2 , Sean M. Andrews3 , Gregory J. Herczeg4 et al.
McDonald Observatory and the Department of Astronomy, University of Texas at Austin, Austin, TX 78712, USA;
Center for Interdisciplinary Exploration and Research in Astrophysics and Department of Physics and Astronomy,
Northwestern University, 2145 Sheridan Road, Evanston, IL 60208-3112, USA; 3 Harvard-Smithsonian Center for
Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; 4 Kavli Institute for Astronomy and Astrophysics,
Peking University, Beijing 100871, People’s Republic of China
1

2E-mail contact: yalinwu at utexas.edu
Characterizing the physical properties and compositions of circumplanetary disks can provide important insights into
the formation of giant planets and satellites. We report ALMA 0.88 mm (Band 7) continuum observations of six
planetary-mass (10–20 MJup) companions: CT Cha b, 1RXS 1609 b, ROXs 12 b, ROXs 42B b, DH Tau b, and FU
Tau b. No continuum sources are detected at the locations of the companions down to 3σ limits of 120–210 µJy.
Given these non-detections, it is not clear whether disks around planetary-mass companions indeed follow the disk
flux-host mass trend in the stellar regime. The faint radio brightness of these companion disks may result from a
combination of fast radial drift and a lack of dust traps. Alternatively, as disks in binary systems are known to havesignificantly lower millimeter fluxes due to tidal interactions, these companion disks may instead follow the relationshipof moderate-separation binary stars. This scenario can be tested with sensitive continuum imaging at rms levels of<∼1 µJy.
Accepted by AJ
http://arxiv.org/pdf/2003.08658

48. Application of Convolutional Neural Networks to Identify Stellar Feedback Bubbles in

CO Emission

Duo Xu1 , Stella S. R. Oﬀner1 , Robert Gutermuth2 and Colin Van Oort3
Department of Astronomy, The University of Texas at Austin, Austin, TX 78712, USA;; 2 Department of Astronomy,
University of Massachusetts, Amherst, MA 01003, USA; 3 University of Vermont, Burlington, VT 05405, USA

1E-mail contact: xuduo117 at utexas.edu

27

We adopt a deep learning method casi (Convolutional Approach to Shell Identification) and extend it to 3D (casi-3d)
to identify signatures of stellar feedback in molecular line spectra, such as 13 CO. We adopt magneto-hydrodynamics
simulations that study the impact of stellar winds in a turbulent molecular cloud as an input to generate synthetic
observations. We apply the 3D radiation transfer code radmc-3d to model 13 CO (J=1-0) line emission from thesimulated clouds. We train two casi-3d models: ME1 is trained to predict only the position of feedback, while MF
is trained to predict the fraction of the mass coming from feedback in each voxel. We adopt 75% of the synthetic
observations as the training set and assess the accuracy of the two models with the remaining data. We demonstratethat model ME1 identifies bubbles in simulated data with 95% accuracy, and model MF predicts the bubble mass
within 4% of the true value. We test the two models on bubbles that were previously visually identified in Taurus
in 13 CO. We show our models perform well on the highest confidence bubbles that have a clear ring morphology
and contain one or more sources. We apply our two models on the full 98 deg2 FCRAO 13 CO survey of the Taurus
cloud. Models ME1 and MF predict feedback gas mass of 2894 M⊙ and 302 M⊙ , respectively. When including acorrection factor for missing energy due to the limited velocity range of the 13 CO data cube, model ME1 predicts
feedback kinetic energies of 4.0×1046 ergs and 1.5×1047 ergs with/without subtracting the cloud velocity gradient.
Model MF predicts feedback kinetic energy of 9.6×1045 ergs and 2.8×1046 ergs with/without subtracting the cloud
velocity gradient. Model ME1 predicts bubble locations and properties consistent with previous visually identified
bubbles. However, model MF demonstrates that feedback properties computed based on visual identifications are
significantly over-estimated due to line of sight confusion and contamination from background and foreground gas.
Accepted by ApJ
https://arxiv.org/pdf/2001.04506

49. First embedded cluster formation in California molecular cloud
Jin-Long Xu1,2 , Ye Xu3 , Peng Jiang1,2 , Ming Zhu1,2 , Xin Guan1 et al.
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China; 2 CAS Key Laboratory of
FAST, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China; 3 Purple Mountain
Observatory, Chinese Academy of Sciences, Nanjing 210008, China
1E-mail contact: xujl at bao.ac.cn
We performed a multi-wavelength observation toward LkHα 101 embedded cluster and its adjacent 85′ × 60′ region.
The LkHα 101 embedded cluster is the first and only one significant cluster in California molecular cloud (CMC).
These observations have revealed that the LkHα 101 embedded cluster is just located at the projected intersectional
region of two filaments. One filament is the highest-density section of the CMC, the other is a new identified filament
with a low-density gas emission. Toward the projected intersection, we find the bridging features connecting the two
filaments in velocity, and identify a V-shape gas structure. These agree with the scenario that the two filaments arecolliding with each other. Using the Five-hundred-meter Aperture Spherical radio Telescope (FAST), we measured
that the RRL velocity of the LkHα 101 H II region is 0.5 km s−1 , which is related to the velocity component of the
CMC filament. Moreover, there are some YSOs distributed outside the intersectional region. We suggest that thecloud-cloud collision together with the fragmentation of the main filament may play an important role in the YSOs
formation of the cluster.
Accepted by ApJL
http://arxiv.org/pdf/2003.09811

50. In Search for Infall Motion in molecular clumps II: HCO+ (1-0) and HCN (1-0) Obser-

vations toward a Sub-sample of Infall Candidates

Yang Yang1,2 , Zhibo Jiang1,2,3 , Zhiwei Chen1 , Shaobo Zhang1 , Shuling Yu1,2 and Yiping Ao1
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, Jiangsu 210008, People’s Republic of China; 2
University of Science and Technology of China, Chinese Academy of Sciences, Hefei, Anhui 230026, People’s Republicof China; 3 China Three Gorges University, Yichang, Hubei 443002, People’s Republic of China
1E-mail contact: zbjiang at pmo.ac.cn
Gravitational accretion accumulates the original mass, and this process is crucial for us to understand the initial28

phases of star formation. Using the specific infall profiles in optically thick and thin lines, we searched the clumps
with infall motion from the Milky Way Imaging Scroll Painting (MWISP) CO data in previous work. In this study,
we selected 133 sources of them as a sub-sample for further research and identification. The excitation temperaturesof these sources are between 7.0 and 38.5 K, while the H2 column densities are between 1021 and 1023 cm−2 . We haveobserved optically thick lines HCO+ (1-0) and HCN (1-0) using the DLH 13.7-m telescope, and found 56 sources ofthem with blue profile and no red profile in these two lines, which are likely to have infall motions, with the detection
rate of 42%. It suggests that using CO data to restrict sample can effectively improve the infall detection rate. Amongthese confirmed infall sources, there are 43 associated with Class 0/I young stellar objects (YSOs), and 13 are not.
These 13 sources are probably associated with the sources in earlier evolutionary stage. By comparison, the confirmed
sources which are associated with Class 0/I YSOs have higher excitation temperatures and column densities, while
the other sources are colder and have lower column densities. Most infall velocities of the sources we confirmed are
between 10−1 to 100 km s−1 , which is consistent with previous studies.
Accepted by Research in Astronomy and Astrophysics
http://arxiv.org/pdf/2003.07136

51. Transition from ordered pinched to warped magnetic field on a 100 au scale in the Class

0 protostar B335
Hsi-Wei Yen1 , Bo Zhao2 , Patrick Koch1 , Ruben Krasnopolsky1 , Zhi-Yun Li3 , Nagayoshi Ohashi1 , Hsien
Shang1 , Shigehisa Takakuwa4,1 and Ya-Wen Tang1
Academia Sinica Institute of Astronomy and Astrophysics, 11F of Astro-Math Bldg, 1, Sec. 4, Roosevelt Rd, Taipei
10617, Taiwan; 2 Max-Planck-Institut für extraterrestrische Physik (MPE), Garching, Germany, 85748; 3 Astronomy
Department, University of Virginia, Charlottesville, VA 22904, USA; 4 Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065,
Japan

1

E-mail contact: hwyen at asiaa.sinica.edu.tw
We present our observational results of the 0.87 mm polarized dust emission in the Class 0 protostar B335 obtainedwith the Atacama Large Millimeter/submillimeter Array (ALMA) at a 0.′′ 2 (20 au) resolution. We compared ourdata at 0.87 mm with those at 1.3 mm from the ALMA archive. The observed polarization orientations at the two
wavelengths are consistent within the uncertainty, and the polarization percentages are systematically higher at 1.3
mm than 0.87 mm by a factor of ∼1.7, suggesting that the polarized emission originates from magnetically aligned
dust grains. We inferred the magnetic field orientations from the observed polarization orientations. We found thatthe magnetic field changes from ordered and highly pinched to more complicated and asymmetric structures within
the inner 100 au scale of B335, and the magnetic field connects to the center along the equatorial plane as well as
along the directions which are ∼40◦–60◦ from the equatorial plane. We performed non-ideal MHD simulations ofcollapsing dense cores. We found that similar magnetic field structures appear in our simulations of dense cores withthe magnetic field and rotational axis slightly misaligned by 15◦ but not in those with the aligned magnetic field androtational axis. Our results suggest that the midplane of the inner envelope within the inner 100 au scale of B335
could be warped because of the misaligned magnetic field and rotational axis, and the magnetic field could be draggedby the warped accretion flows.
Accepted by ApJ
https://arxiv.org/pdf/2003.04502.pdf

52. HII regions and high-mass starless clump candidates I: Catalogs and properties
S. Zhang1 , A. Zavagno1,2 , J. Yuan3 , H. Liu4,5 , M. Figueira6 et al.
Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France; 2 Institut Universitaire de France (IUF); 3 National
Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012,
China; 4 CASSACA, China-Chile Joint Center for Astronomy, Camino El Observatorio #1515, Las Condes, Santiago,
Chile; 5 Departamento de Astronomía, Universidad de Concepción, Av. Esteban Iturra s/n, Distrito Universitario,
160-C, Chile; 6 National Centre for Nuclear Research, ul. Pasteura 7, 02-093, Warszawa
129

E-mail contact: siju.zhang at lam.fr
The role of ionization feedback on high-mass (>8 M⊙ ) star formation (HMSF) is still highly debated. Questions
remain concerning the presence of nearby HII regions changes the properties of early HMSF and whether HII regions
promote or inhibit the formation of high-mass stars. To characterize the role of HII regions on the HMSF, we study
the properties of a sample of candidates high-mass starless clumps (HMSCs), of which about 90% have masses larger
than 100 M⊙ . These high-mass objects probably represent the earliest stages of HMSF; we search if (and how) theirproperties are modified by the presence of an HII region. We took advantage of the recently published catalog of
HMSC candidates. By cross matching the HMSCs and HII regions, we classified HMSCs into three categories: 1) The
HMSCs associated with HII regions both in the position in the projected plane of the sky and in velocity; 2) HMSCs
associated in the plane of the sky, but not in velocity; and 3) HMSCs far away from any HII regions in the projectedsky plane. We carried out comparisons between associated and nonassociated HMSCs based on statistical analyses ofmultiwavelength data from infrared to radio. Statistical analyses suggest that HMSCs associated with HII regions arewarmer, more luminous, more centrally-peaked and turbulent. We also clearly show, for the first time, that the ratio ofbolometric luminosity to envelope mass of HMSCs (L/M ) could not be a reliable evolutionary probe for early HMSF
due to the external heating effects of the HII regions. More centrally peaked and turbulent properties of HMSCs
associated with HII regions may promote the formation of high-mass stars by limiting fragmentation. High resolution
interferometric surveys toward HMSCs are crucial to reveal how HII regions impact the star formation process inside
HMSCs.
Accepted by A&A
http://arxiv.org/pdf/2003.11433

53. Global 3-D Radiation Magnetohydrodynamic Simulations for FU Ori’s Accretion Disk

and Observational Signatures of Magnetic Fields
Zhaohuan Zhu1 , Yan-Fei Jiang2 and James M. Stone3
Department of Physics and Astronomy, University of Nevada, Las Vegas, 4505 S. Maryland Parkway, Las Vegas, NV
89154, USA; 2 Center for Computational Astrophysics, Flatiron Institute, New York, NY 10010, USA; 3 nstitute forAdvance Study, 1 Einstein Drive, Princeton, NJ, 08540, USA
1E-mail contact: zhaohuan.zhu at unlv.edu
22 pages, 20 figures
FU Ori is the prototype of FU Orionis systems which are outbursting protoplanetary disks. Magnetic fields in FU
Ori’s accretion disks have previously been detected using spectropolarimetry observations for Zeeman effects. We
carry out global radiation ideal MHD simulations to study FU Ori’s inner accretion disk. We find that (1) when thedisk is threaded by vertical magnetic fields, most accretion occurs in the magnetically dominated atmosphere at z∼R,
similar to the “surface accretion” mechanism in previous locally-isothermal MHD simulations. (2) A moderate disk
wind is launched in the vertical field simulations with a terminal speed of ∼300-500 km/s and a mass loss rate of 1-10%
the disk accretion rate, which is consistent with observations. Disk wind fails to be launched in simulations with net
toroidal magnetic fields. (3) The disk photosphere at the unit optical depth can be either in the wind launching region
or the accreting surface region. Magnetic fields have drastically different directions and magnitudes between these
two regions. Our fiducial model agrees with previous optical Zeeman observations regarding both the field directions
and magnitudes. On the other hand, simulations indicate that future Zeeman observations at near-IR wavelengths or
towards other FU Orionis systems may reveal very different magnetic field structures. (4) Due to energy loss by thedisk wind, the disk photosphere temperature is lower than that predicted by the thin disk theory, and the previously
inferred disk accretion rate may be lower than the real accretion rate by a factor of ∼2-3.
Accepted by MNRAS
https://arxiv.org/pdf/1912.01632

54. The resonant drag instability of dust streaming in turbulent protoplanetary disc
V.V. Zhuravlev1
1

Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetskij pr., 13, Moscow 119234,
30

RussiaE-mail contact: zhuravlev at sai.msu.ru
Damping of the previously discovered resonant drag instability (RDI) of dust streaming in protoplanetary disc is studied
using the local approach to dynamics of gas-dust perturbations in the limit of the small dust fraction. Turbulence ina disc is represented by the effective viscosity and diffusivity in equations of motion for gas and dust, respectively. In
the standard case of the Schmidt number (ratio of the effective viscosity to diffusivity) Sc = 1, the reduced descriptionof RDI in terms of the inertial wave (IW) and the streaming dust wave (SDW) falling in resonance with each otherreveals that damping solution differs from the inviscid solution simply by adding the characteristic damping frequency
to its growth rate. RDI is fully suppressed at the threshold viscosity, which is estimated analytically, first, for radial
drift, next, for vertical settling of dust, and at last, in the case of settling combined with radial drift of the dust. In
the last case, RDI survives up to the highest threshold viscosity, with a greater excess for smaller solids. Once Sc 6= 1,
a new instability specific for dissipative perturbations on the dust settling background emerges. This instability ofthe quasi-resonant nature is referred to as settling viscous instability (SVI). The mode akin to SDW (IW) becomesgrowing in a region of long waves provided that Sc > 1 (Sc < 1). SVI leads to an additional increase of the thresholdviscosity.
Accepted by MNRAS
http://arxiv.org/pdf/2003.09212

55. Importance of radiative effects in gap opening by planets in protoplanetary disks
Alexandros Ziampras1 , Wilhelm Kley1 , and Cornelis P. Dullemond2
1
2

Institut für Astronomie und Astrophysik, Universität Tübingen, Auf der Morgenstelle 10, 72076 Tübingen, Germany;
Institute for Theoretical Astrophysics, Heidelberg University, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany

E-mail contact: alexandros.ziampras at uni-tuebingen.de
Recent ALMA observations revealed concentric annular structures in several young class-II objects. In an attempt to
produce the rings and gaps in some of these systems, they have been modeled numerically with a single embedded
planet assuming a locally isothermal equation of state. This is often justified by observations targeting the irradiationdominated outer regions of disks (approximately 100 au). We test this assumption by conducting hydrodynamics
simulations of embedded planets in thin locally isothermal and radiative disks that mimic the systems HD 163296 andAS 209 in order to examine the effect of including the energy equation in a seemingly locally isothermal environment
as far as planet-disk interaction is concerned. We find that modeling such disks with an ideal equation of state makesa difference in terms of the number of produced rings and the spiral arm contrast in the disk. Locally isothermal disks
produce sharper annular or azimuthal features and overestimate a single planet’s gap-opening capabilities by producing
multiple gaps. In contrast, planets in radiative disks carve a single gap for typical disk parameters. Consequently, for
accurate modeling of planets with semimajor axes up to about 100 au, radiative effects should be taken into accounteven in seemingly locally isothermal disks. In addition, for the case of AS 209, we find that the primary gap issignificantly different between locally isothermal and radiative models. Our results suggest that multiple planets are
required to explain the ring-rich structures in such systems.
Accepted by A&A
http://arxiv.org/pdf/2003.02298

31

Abstracts of recently accepted major reviews

High-energy particles and radiation in star-forming regions
Andrei M. Bykov1 , Alexandre Marcowith2 , Elena Amato3 , Maria E. Kalyashova1 , J.M. Diederik
Kruijssen4 , Eli Waxman5
Ioffe Institute, 194021, St. Petersburg, Russia; 2 Laboratoire Univers et Particules de Montpellier CNRS/Universitéde Montpellier, Place E. Bataillon, 34095 Montpellier, France; 3 INAF - Osservatorio Astrofisico di Arcetri, Largo E.
Fermi, 5, 50125, Firenze, Italy; 4 Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg,
Mönchhofstr. 12-14, 69120 Heidelberg, Germany; 5 Weizmann Institute of Science, 76100, Rehovot, Israel
1E-mail contact: byk at astro.ioffe.ru
Non-thermal particles and high-energy radiation can play a role in the dynamical processes in star-forming regions andprovide an important piece of the multiwavelength observational picture of their structure and components. Powerfulstellar winds and supernovae in compact clusters of massive stars and OB associations are known to be favourablesites of high-energy particle acceleration and sources of non-thermal radiation and neutrinos. Namely, young massive
stellar clusters are likely sources of the PeV (petaelectronvolt) regime cosmic rays (CRs). They can also be responsible
for the cosmic ray composition, e.g., 22 Ne/20 Ne anomalous isotopic ratio in CRs. Efficient particle acceleration canbe accompanied by super-adiabatic amplification of the fluctuating magnetic fields in the systems converting a partof kinetic power of the winds and supernovae into the magnetic energy through the CR-driven instabilities. The
escape and CR propagation in the vicinity of the sources are affected by the non-linear CR feedback. These effects
are expected to be important in starburst galaxies, which produce high-energy neutrinos and gamma-rays. We give a
brief review of the theoretical models and observational data on high-energy particle acceleration and their radiationin star-forming regions with young stellar population.
Accepted by Space Science Reviews
http://arxiv.org/pdf/2003.11534

32

Dissertation Abstracts

Accretion versus outflow regions around Young Stellar Objects
Raquel de Albuquerque

Departamento de Física e Astronomia, Faculdade de Ciências da Universidade do Porto, Portugal
Instituto de Astrofísica e Ciências do Espaco, CAUP, Portugal
Laboratoire Univers et Théories, Observatoire de Paris, FranceInstituto de Astrofísica e Ciências do Espaco, CAUP, Rua das Estrelas, PT4150-762 Porto, Portugal
Electronic mail: Raquel.Albuquerque at astro.up.pt
Ph.D dissertation directed by: João J. G. Lima, Jorge F. Gameiro and Christophe Sauty
Ph.D degree awarded: February 2020

The interplay between accretion and outflow processes in young stellar objects (YSOs) constitutes one of the big
challenges in the field of star formation. We can better understand their evolution not only by a proper derivation
and analysis of stellar and activity parameters through spectra, but also by modelling and simulating accretion andoutflow mechanisms. In order to take a step further towards a better understanding of these phenomena, we started
by carrying out a detailed study of the spectra of some YSOs and explored different tools that can be used tobetter understand these stars. We then proceeded to perform detailed simulations of the environment around sucha YSO, where both accretion and outflows are at play, using existing numerical tools and self-similar semi-analyticalmagnetohydrodynamic solutions as initial conditions. Thus, to accomplish the goals of this project, we first test
available software for main-sequence stars that has the potential to characterize pre-main sequence stars through theirmain stellar parameters. Second, we characterize a sample of YSOs using ultraviolet to near-infrared spectra plus
available photometry. Third, we explore a long-term monitoring of two variable classical T Tauri stars, through both
spectroscopy and photometry, in order to characterize their circumstellar environment. Fourth, we actually simulate
the circumstellar environment of one of these objects and evaluate if it is compatible with what is observationally
expected. Our simulations are able to reproduce the general behaviour expected for the environment around such a
YSO. Also, we can derive from those simulations mass accretion and mass loss rates that agree well with the ones
we could obtain from the corresponding spectra and with those available in the literature. Furthermore, we havesimulations that could not only represent the bimodal behaviour of RY Tau, characterized by active and quiescentperiods, but also the ceasing of accretion activity in YSOs. The work presented in this thesis, shows how the synergy
between an observational and a numerical approach can improve our knowledge towards the study of low-mass YSOs.
https://hdl.handle.net/10216/126546
33

Pre-main-sequence populations and young stellar variability in the Large
Magellanic Cloud
Viktor Zivkov

Keele University, UK; European Southern Observatory, Germany
Lennard-Jones Laboratories, School of Chemical and Physical Sciences, Keele University, ST5 5BG, UK
Electronic mail: v.zivkov at keele.ac.uk
Ph.D dissertation directed by: Joana M. Oliveira and Monika G. Petr-Gotzens
Ph.D degree awarded: March 2020

Detailed studies of intermediate- and low-mass pre-main-sequence (PMS) stars outside the Galaxy have so far been
conducted only for small targeted regions harbouring known star formation complexes. This work presents a comprehensive analysis of the PMS population in a ∼ 1.5 deg2 area located in the gas-rich Large Magellanic Cloud(LMC). The identification and classification of the populations was achieved by statistical analysis of the Ks /(Y − Ks )colour−magnitude distribution of stars using a PSF photometric source catalogue of the VISTA Survey of the Magel<lanic Clouds (VMC). The analysis reveals ∼ 2260 PMS candidates with ages <∼10 Myr and masses ∼4 M⊙ . The young
populations exhibit non-uniform spatial distributions and appear to be hierarchically organized with large structurescontaining smaller and denser substructures. Regions containing only intermediate/low-mass PMS stars are more
scattered and usually located in the outskirts of star forming complexes. The young populations are clustered along
ridges and filaments where dust emission in the far-infrared (FIR) (70 µm – 500 µm) is bright. At 70 µm and 100 µm
we report a strong dust emission increase in regions hosting young massive stars, which is less pronounced in regions
populated only by less massive (<∼4 M⊙ ) PMS stars.
In addition, this thesis presents the first systematic variability study of massive young stellar objects (YSOs) in the
LMC. By using a χ2 -analysis on multi-epoch observations obtained by the VMC and my open time programme, stellar
variability is identified. 173 high-reliability YSO candidates are selected based on several Spitzer studies, out of which
39 displayed variability. They have been classified into eruptive, fader, dipper, short-term variable and long periodvariable-YSO based on the appearance of their Ks -band lightcurves. The majority of YSO variables are aperiodic; forfive YSOs the lightcurves indicate a possible periodicity, identified using a Lomb-Scargle periodogram analysis. The
lightcurve shapes and colour shifts can be mostly associated with unsteady accretion or (grey) extinction. Overall, theobserved amplitudes are moderate with only two YSOs exhibiting a ∆Ks > 1 mag. Eruptive variables tend to havethe largest amplitudes amongst all classes. Compared with similar Galactic studies the amplitudes tend to be smaller,
which could be attributed to smaller extinction variations due to the larger gas-to-dust ratio of the LMC.

34

New Jobs

Postdoctoral Position in Star Formation & Observational Astrophysics
Center for Astrophysics and Space Astronomy (CASA)
Astrophysical and Planetary Sciences Department (APS)
University of Colorado, Boulder
Boulder, Colorado, USA
Applications are invited for a two-year postdoctoral position at the University of Colorado Boulder starting in August
2020, to work with Prof. John Bally on observations and theory of star formation.
The successful applicant will contribute to a research program using multi-wavelength imaging and spectroscopy from
Apache Point Observatory, Subaru, ALMA, the JVLA, and other facilities. Familiarity with data reduction methods
and tools is essential. Candidates familiar with numerical simulations such as N-body, SPH, or other codes used toinvestigate the physics of outflows, their interactions with the surrounding ISM, protostellar dynamic interactions andmergers among protostars will also be considered.
The general goal is to investigate the feedback processes that operate in the self-regulation of star formation. Specificgoals include: [1] Complete the analysis and publication of existing data on the Orion OMC1 outflow, ejected stars,
and environment. [2] Observe other Galactic explosive outflow candidates to constrain their event rates, properties,
and impacts. [3] Continue near-IR monitoring of nearby star-forming galaxies to probe the properties of extra-galactic
IR transients detected by Spitzer. [4] Explore the use of 6.7 GHz (methanol) and 22 GHz (water) maser outbursts
as alerts for protostellar mergers or major accretion-powered IR-transients. [5] Model circumstellar disk & envelope
behavior in interactions using public-domain SPH and N-body codes.
Who We Are:
The Center for Astrophysics and Space Astronomy (CASA: https://www.colorado.edu/casa/) is dedicated to advancing our understanding of the Universe in which we live through observations, theory, and the development ofground-based and space-borne instrumentation. Founded in 1985, CASA is an affiliated unit within the structure of
the Astrophysical and Planetary Sciences (APS) Department at the University of Colorado, Boulder(https://www.colorado.edu/aps/).
What Your Key Responsibilities Will Be:
The successful applicant will contribute to the research program by generating new observing proposals, reducing andanalyzing data, and writing up results. Potential applicants are invited to contact John Bally (john.bally@colorado.edu)
to discuss their potential fit to this position.
What We Offer:
The appointment will be for an initial period of two years, with renewal for a third year contingent upon satisfactory
progress and availability of funds. The position includes a competitive salary, research/travel funds, and access toCU’s computing resources and partnership in the Apache Point Observatory and Sloan Digital Sky Survey.
Benefits:
The University of Colorado offers excellent benefits, including medical, dental, retirement, paid time off, tuition benefit
and ECO Pass. The University of Colorado Boulder is one of the largest employers in Boulder County and offers an inspiring higher education environment. Learn more about the University of Colorado Boulder (https://colorado.edu).
Be Adaptable. Be Imaginative. Be Boulder.
What We Require:
Applicants must have a PhD in astronomy and/or physics on arrival.
35

What We Would Like You To Have:
Experience with visual, infrared, and radio data reduction and analysis methods. Familiarity with numerical simulationof star-forming environments would be welcome.
Special Instructions:
To apply, please submit the following materials by May 15, 2020:• Resume/CV (including a list of publications)• Cover letter• Transcripts/Proof of Degree• Statement of research philosophy - Brief (up to 3 pages) research statement of your scientific interests and how you
would specifically contribute to the research program described above.
• Three letters of recommendation to be emailed as PDFs
Application materials are accepted electronically via CU Boulder Jobs.
Please send copies of application material via e-mail tojohn.bally@colorado.edu.
Full consideration will be given to applications that are completed by May 15, 2020 or until the position is filled.
Posting Contact Information:
https://jobs.colorado.edu/jobs/JobDetail/?jobId=23016
Posting Contact Name: Boulder Campus Human Resources
Posting Contact Email: Recruiting@colorado.edu
The University of Colorado Boulder is committed to building a culturally diverse community of faculty, staff, andstudents dedicated to contributing to an inclusive campus environment. We are an Equal Opportunity employer,
including veterans and individuals with disabilities.

Moving ... ??
If you move or your e-mail address changes, please
send the editor your new address. If the Newsletterbounces back from an address for three consecutive
months, the address is deleted from the mailing list.

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Meetings

Cool Stars, Stellar Systems, and the Sun 21
Dear Colleagues,
We regret to announce that the Cool Stars, Stellar Systems, and the Sun 21st Conference, originally planned to beheld on June 22-26, 2020, in Toulouse, France, has to be postponed due to the current Covid-19 pandemic. The
decision was discussed within the SOC and LOC, and agreed by all members of the organizing committees. We plan
to reschedule CS21 in Summer 2021.
Preliminary dates (tbc) for CS21 would be 5-9 July 2021, at the same location in Toulouse, France. We foresee thatthe program that was designed for CS21 this year, including the planned invited talks and the scheduled splintersessions, will still be largely relevant next year, unless other hot topics emerge till then. We will continue to provide
updated information on the current CS21 website.
As chairs of the SOC and LOC, we would like to express our gratitude to all the members of the organizing committees,
especially to the members of the LOC for the efforts they deployed in this uncertain context. We extend our thanks
to the chairs of the proposed Splinter sessions, to the speakers who accepted our invitation for the plenary sessions,and to all of you who had registered for the conference.
Take care, and we hope to see you next year!
S. Brun, J. Bouvier, P. Petit

Cloudy Workshop Athens Greece
Registration is now open for the Cloudy workshop to be held 2020 June 15 to 19 at the Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing (IAASARS) in Athens Greece. https://www.astro.noa.gr/en/main/.
The science part of the workshop is described at https://cloud9.pa.uky.edu/~gary/cloudy/CloudySummerSchool/
while instructions for registering and local information will be posted on the forum https://groups.io/g/CloudyAthens2020.
Please join it to get updates on the workshop.
Cloudy is a large-scale code that simulates the microphysics of matter exposed to ionizing radiation. It calculates theatomic physics, chemistry, radiation transport, and dynamics problems simultaneously and self-consistently, building
from a foundation of individual atomic and molecular processes. The result is a first-principles prediction of theconditions in the material and its observed spectrum.
The workshop will cover observation, theory, and application of Cloudy to a wide variety of astronomical environments.
This includes the theory of diffuse matter and quantitative spectroscopy, the science of using spectra to make physicalmeasurements. We will use Cloudy to simulate such objects as AGB stars, Active Galactic Nuclei, Starburst galaxies,
and the intergalactic medium.
The sessions will consist of a mix of textbook study, using Osterbrock & Ferland, ’Astrophysics of Gaseous Nebulaeand Active Galactic Nuclei’, application of Cloudy to a variety of astrophysical problems, and projects organizedby the participants. No prior experience with Cloudy is assumed although some knowledge of spectroscopy and thephysics of the interstellar medium is useful.

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ACO Torino-2021 Conference:

Chemical Processes in Solar-type Star Forming Regions
Dear Colleagues,This is the first announcement of the Conference:
CHEMICAL PROCESSES IN SOLAR-TYPE STAR FORMING REGIONS
jointly organized by the Department of Chemistry of the University of Torino and INAF Astrophysical Observatoryof Arcetri in the context of the EU 2020 ITN project AstroChemical Origins (ACO).
The meeting will consist of invited reviews, invited and contributed talks, and posters. Support for PhD and young
students is also planned.
Conference site: Department of Chemistry, University of Torino, Italy Conference dates: 13th – 17th September 2021
Registration deadline: 20th May 2021 Abstract submission deadline: 1st May 2021
The announcement of the conference is available on the web at: https://sites.google.com/inaf.it/aco-conference/
Please circulate this notice among your colleagues, especially young PhD and PostDoc students.
Rationale:
How the chemical complexity evolves during the process leading to the formation of a Sun and its planetary system?
Is the chemical richness of a Solar-like planetary system, at least partially, inherited from the earliest stages or is there
a complete chemical reset? A powerful way to answering these questions is by comparing the chemical content inyoung protostars and primitive bodies of the Solar System, using astrochemistry as a tool. Yet, to do so, we need to
fully understand the processes that govern the chemical evolution of a molecular cloud into a young planetary system.
The goal of the conference is to gather together the actors of this intrinsically interdisciplinary endeavor: astronomers,
chemists and modelers. The recent huge progresses in the three areas make the time ripe for these communities tojoin and ride this scientific wave.
We invite all of you to join the Conference.
The Scientific Organizing Committee P. Ugliengo, C. Codella, A. Barucci, C. Ceccarelli, L. Piccirillo, A. Rimola, C.
Vastel, S. Viti, S. Yamamoto

38Summary of Upcoming Meetings

AIP Thinkshop on Protoplanetary Disk Chemodynamics
11 - 15 May 2020, Leibnitz Institute for Astrophysics Potsdam, Germany
https://meetings.aip.de/event/1
Planet Formation: From Dust Coagulation to Final Orbital Assembly
1 - 26 June 2020, Munich, Germany
http://www.munich-iapp.de/planetformation
The Physics of Star Formation: From Stellar Cores to Galactic Scales; 29 June - 3 July 2020, Lyon,
Francehttp:/staratlyon.univ-lyon1.fr/en
Illuminating the Dusty Universe: A Tribute to the Work of Bruce Draine
6 - 10 July 2020, Florence, Italy
https://web.astro.princeton.edu/IlluminatingTheDusty Universe
The Early Phase of Star Formation
12 - 17 July 2020, Ringberg, Germany
http://www.mpia.de/homes/stein/EPoS/2020/2020.php
Star Formation: From Clouds to Discs - A Tribute to the Career of Lee Hartmann
17 - 20 August 2020, Malahide, Ireland
https://www.dias.ie/cloudstodiscs/
Star Formation in Diﬀerent Environments 202024 - 28 August 2020, Quy Nhon, Vietnam
http://icisequynhon.com/conferences/sfde/
Planetary Science: The Young Solar System
6 - 12 September 2020, Quy Nhon, Vietnam
http://www.icisequynhon.com/conferences/planetary_science/
Wheel of Star Formation: A conference dedicated to Prof. Jan Palouš
14 - 18 September 2020, Prague, Czech Republic
https://janfest2020.asu.cas.cz
Conditions and Impact of Star Formation - Across Times and Scales
28 September - 2 October 2020, Chile
https://astro.uni-koeln.de/symposium-star-formation-2020.html
From Clouds to Planets II: The Astrochemical Link
28 September - 2 October 2020, Berlin, Germany
https://events.mpe.mpg.de/event/12/
The Aftermath of a Revolution: Planet Formation Five Years after HL Tau
7 - 11 December 2020, Chile
https://www.eso.org/sci/meetings/2020/hltau2020.html
Protostars & Planets VII
1 - 7 April 2021, Kyoto, Japan
http://www.ppvii.org
Cool Stars, Stellar Systems, and the Sun 21
postponed to summer 2021, Toulouse, France
https://coolstars21.github.io/

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Chemical Processes in Solar-type Star Forming Regions
13 - 17 September 2021, Torino, Italy
https://sites.google.com/inaf.it/aco-conference

Short Announcements

Fizeau exchange visitors program - call for applications
Dear colleagues!
The Fizeau exchange visitors program in optical interferometry funds (travel and accommodation) visits of researchers
to an institute of his/her choice (within the European Community) to perform collaborative work and training on one of
the active topics of the European Interferometry Initiative. The visits will typically last for one month, and strengthen
the network of astronomers engaged in technical, scientific and training work on optical/infrared interferometry. The
program is open for all levels of astronomers (Ph.D. students to tenured staff), with priority given to PhD students
and young postdocs. non-EU based missions will only be funded if considered essential by the Fizeau Committee.
Applicants are strongly encouraged to seek also partial support from their home or host institutions.
The deadline for applications is May 15 for visits to be carried out between mid July 2020 and December 2020!.
Note: the next call will be issued in November 2020!
Note: requests for support for the Fizeau VLTI school in September are NOT part of this call. Such requests will behandled by the school organizers.
Further informations and application forms can be found at www.european-interferometry.eu
The program is funded by OPTICON/H2020.
Please distribute this message also to potentially interested colleagues outside of your community!
Looking forward to your applications,Josef Hron & Péter Ábrahám(for the European Interferometry Initiative)
Electronic mail: fizeau@european-interferometry.eu

Abstract submission deadline
The deadline for submitting abstracts and othersubmissions is the first day of the month. Abstracts
submitted after the deadline will appear in the following month’s issue.

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