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TZOFFSETFROM:-0600
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RDATE:20211107T010000
TZOFFSETFROM:-0600
TZOFFSETTO:-0500
TZNAME:America/Chicago CDT
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RDATE:20221106T010000
TZOFFSETFROM:-0600
TZOFFSETTO:-0500
TZNAME:America/Chicago CDT
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RDATE:20231105T010000
TZOFFSETFROM:-0600
TZOFFSETTO:-0500
TZNAME:America/Chicago CDT
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RDATE:20241103T010000
TZOFFSETFROM:-0600
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BEGIN:VEVENT
UID:35376ca7d9ee0dc6a68f45367f46515a
CATEGORIES:Stars, Planets, and ISM Seminar
SUMMARY:Stars, Planets, and ISM Seminar
LOCATION:RLM 15.216
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:
Title: TBA
DTSTAMP:20240328T064111Z
DTSTART;TZID=America/Chicago:20190904T120000
DTEND;TZID=America/Chicago:20190904T130000
SEQUENCE:0
RRULE:FREQ=WEEKLY;UNTIL=20191205T000000Z;INTERVAL=1;BYDAY=WE
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:35376ca7d9ee0dc6a68f45367f46515a
CATEGORIES:Stars, Planets, and ISM Seminar
SUMMARY:Organizational Meeting
LOCATION:RLM 15.216
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Organizational Meeting
DTSTAMP:20240328T064111Z
DTSTART;TZID=America/Chicago:20190904T120000
DTEND;TZID=America/Chicago:20190904T130000
RECURRENCE-ID;TZID=America/Chicago:20190904T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:35376ca7d9ee0dc6a68f45367f46515a
CATEGORIES:Stars, Planets, and ISM Seminar
SUMMARY:Chat Hull, National Astronomical Observatory of Japan
LOCATION:RLM 15.216
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Observations of polarization in protoplanetary disks with AL
MA
Abstract
One of the hottest n
ew topics within the ALMA community centers around polarization observation
s of protoplanetary disks. I will discuss recent observations of pola
rization toward (mostly) evolved, Class II disks, and will give an overview
of our rapidly evolving understanding of the multiple mechanisms that may
(or may not) cause the polarization that we see. In the case of my wo
rk on IM Lup (one of these Class II disks): consistent with some observatio
ns of other disks, the polarization at Bands 6 and 7 (1.3 mm and 850 micron
s) appears to be due to scattering by dust grains, thus complicating the se
arch for magnetic fields in these sources. While these results challe
nge our understanding of dust grain growth, they also have the potential to
open up new windows into the dust-grain properties in young, planet-formin
g disks.
DTSTAMP:20240328T064111Z
DTSTART;TZID=America/Chicago:20190911T120000
DTEND;TZID=America/Chicago:20190911T130000
RECURRENCE-ID;TZID=America/Chicago:20190911T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:35376ca7d9ee0dc6a68f45367f46515a
CATEGORIES:Stars, Planets, and ISM Seminar
SUMMARY:Two Talks
LOCATION:RLM 15.216
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Asmita Bhandare, Max-Planck-Institute for Astronomy
Zooming in on the Early Stages of Star and Disk Formation
<
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<
a href="https://astronomy.utexas.edu/calendar/icals.icalevent/-?evid=1261&i
cf=1&tmpl=component#abstract-2" class="accordion-toggle rl_sliders-toggle n
n_sliders-toggle rl_sliders-item-scroll nn_sliders-item-scroll collapsed" d
ata-toggle="collapse" id="slider-abstract-2" data-id="abstract-2" data-pare
nt="#set-rl_sliders-2" role="button" aria-controls="abstract-2" aria-expand
ed="false"> A
bstract
Abstract
Magnetized, cold, dense molecular c
loud cores provide the birth environment for stars and disks. This work is
aimed at understanding the multi-scale scenario of star formation, which oc
curs via the formation of two quasi-hydrostatic Larson cores. We perform sp
herically symmetric, isolated, molecular cloud collapse simulations using t
he radiation (magneto)hydrodynamic code PLUTO as a tool. These one-dimensio
nal studies, spanning 7 orders of magnitude in spatial scales, account for
the phase transitions by using a realistic gas equation of state via a dens
ity- and temperature-dependent adiabatic index and mean molecular weight. F
or the first time, a large parameter scan across initial low- to high-mass
(0.5 Msun – 100 Msun) molecular cloud cores is surveyed. In this talk, I wi
ll highlight the dependence of the first and second hydrostatic core proper
ties on the initial cloud properties. The results indicate that in the high
-mass regime, first hydrostatic cores do not have time to evolve because of
the large accretion rates. Following these results, we have investigated t
he evolution of the second hydrostatic core using two-dimensional radiation
hydrodynamic collapse simulations with a resolution that has not been achi
eved before. These studies demonstrate, for the first time, the onset of co
nvection within the second core for the collapse cases of non-rotating mole
cular cloud cores in the low-mass regime. This supports an interesting poss
ibility that dynamo-driven magnetic fields may be generated during the very
early phases of low-mass star formation. Additionally, I will also discuss
the impact of different cloud properties on the formation and evolution of
circumstellar disks, formed due to the conservation of angular momentum.
p>
Ya-Lin Wu, The Un
iversity of Texas at Austin
Title: TBA
DTSTAMP:20240328T064111Z
DTSTART;TZID=America/Chicago:20191120T120000
DTEND;TZID=America/Chicago:20191120T130000
RECURRENCE-ID;TZID=America/Chicago:20191120T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:35376ca7d9ee0dc6a68f45367f46515a
CATEGORIES:Stars, Planets, and ISM Seminar
SUMMARY:Coauthor Carousel
LOCATION:RLM 15.216
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Presents informally summarize a paper on which they are a coauthor
DTSTAMP:20240328T064111Z
DTSTART;TZID=America/Chicago:20190918T120000
DTEND;TZID=America/Chicago:20190918T130000
RECURRENCE-ID;TZID=America/Chicago:20190918T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:35376ca7d9ee0dc6a68f45367f46515a
CATEGORIES:Stars, Planets, and ISM Seminar
SUMMARY:Manasvi Lingham, Florida Institute of Technology
LOCATION:RLM 15.216
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:On the Impact of Stellar Properties on (Exo)planetary Habitability
em>
DTSTAMP:20240328T064111Z
DTSTART;TZID=America/Chicago:20190925T120000
DTEND;TZID=America/Chicago:20190925T130000
RECURRENCE-ID;TZID=America/Chicago:20190925T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:35376ca7d9ee0dc6a68f45367f46515a
CATEGORIES:Stars, Planets, and ISM Seminar
SUMMARY:Two Talks
LOCATION:RLM 15.216
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Emily Lubar, The University of Texas at Austin
Achieving ~10cm/s Radial Velocity precision with the HPF and NEID spectrog
raphs
Zach Vanderbosch, The University of Texas at Austi
n
Variable Stars in ZTF and a Second Case of Transiting D
ebris around a White Dwarf
DTSTAMP:20240328T064111Z
DTSTART;TZID=America/Chicago:20191002T120000
DTEND;TZID=America/Chicago:20191002T130000
RECURRENCE-ID;TZID=America/Chicago:20191002T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:35376ca7d9ee0dc6a68f45367f46515a
CATEGORIES:Stars, Planets, and ISM Seminar
SUMMARY:Jonathan Fortney, UC Santa Cruz
LOCATION:RLM 15.216
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Terrestrial Planet Atmospheres: Learning to Play the L
ong Game
Abstract
The ch
aracterization of the atmospheres of terrestrial ("rocky") planets, long th
e stuff of fantasy, is within our reach, starting in the next decade.
The impact of the James Webb Space Telescope will be significant in this a
rea, for the small but growing sample of planets orbiting the nearest lowes
t-mass M stars. I will highlight a project to assess how precise radi
al velocity planet masses must be to yield robust atmospheric constraints.&
nbsp; However, it seems that "comparative atmospheric planetary science" wi
th a large sample size may have to wait til at least the late 2030s or beyo
nd, with future space telescopes. I will discuss work to quantify the
requirements for wavelength coverage, spectral resolution, and signal-to-n
oise needed for future optical reflected light telescopes like LUVOIR or Ha
bEx, which aim to characterize terrestrial planet atmospheres. Finally, I w
ill show new experimental work, in collaboration with colleagues at UC Sant
a Cruz, to investigate the origins of terrestrial planetary atmospheres, vi
a studies of meteorite outgassing. Such studies are one part of a lon
g network of not yet well-understood physical and chemical processes that d
ictate atmospheric origin and evolution, which must be studied in tandem wi
th new exoplanet observations.
DTSTAMP:20240328T064111Z
DTSTART;TZID=America/Chicago:20191009T120000
DTEND;TZID=America/Chicago:20191009T130000
RECURRENCE-ID;TZID=America/Chicago:20191009T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:35376ca7d9ee0dc6a68f45367f46515a
CATEGORIES:Stars, Planets, and ISM Seminar
SUMMARY:Fritz Benedict, The University of Texas at Austin
LOCATION:RLM 15.216
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:A Tale of Two Systems
<
div class="accordion-inner panel-body">
Abstract
In a stars, planets, and ISM seminar t
hat checks all the boxes I report results of astrometry carried out&nb
sp;with the Hubble Space Telescope Fine Guidance Sensors. We confirm t
he existence of a white dwarf component of the quadruple Hyad bin
ary, vA 351, and establish its mass. Two of the three M dwarf componen
ts orbit with an 18 hour period, and are immersed in a hydrogen cloud
that evidences mass exchange (stars and ISM). In the second half of th
e seminar I present recent efforts to establish component masses
and the architecture of the mu Arae planetary system (exopla
nets). Both projects remain incomplete due to ongoing mysteries u
nique to each.
DTSTAMP:20240328T064111Z
DTSTART;TZID=America/Chicago:20191016T120000
DTEND;TZID=America/Chicago:20191016T130000
RECURRENCE-ID;TZID=America/Chicago:20191016T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:35376ca7d9ee0dc6a68f45367f46515a
CATEGORIES:Stars, Planets, and ISM Seminar
SUMMARY:BashFest - No talk scheduled
LOCATION:RLM 15.216
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:No talk scheduled
DTSTAMP:20240328T064111Z
DTSTART;TZID=America/Chicago:20191023T120000
DTEND;TZID=America/Chicago:20191023T130000
RECURRENCE-ID;TZID=America/Chicago:20191023T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:35376ca7d9ee0dc6a68f45367f46515a
CATEGORIES:Stars, Planets, and ISM Seminar
SUMMARY:Two Talks
LOCATION:RLM 15.216
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Chelsea Huang, MIT
Title: TBA
George Zhou, Harvard-Smithsonian CfA
Title: TBA
p>
DTSTAMP:20240328T064111Z
DTSTART;TZID=America/Chicago:20191030T120000
DTEND;TZID=America/Chicago:20191030T130000
RECURRENCE-ID;TZID=America/Chicago:20191030T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:35376ca7d9ee0dc6a68f45367f46515a
CATEGORIES:Stars, Planets, and ISM Seminar
SUMMARY:Two Talks
LOCATION:RLM 15.216
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Catherine Manea, The University of Texas at Austin
Title: TBA
Andreia Carrillo, The University of Texa
s at Austin
Title: TBA
DTSTAMP:20240328T064111Z
DTSTART;TZID=America/Chicago:20191106T120000
DTEND;TZID=America/Chicago:20191106T130000
RECURRENCE-ID;TZID=America/Chicago:20191106T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:35376ca7d9ee0dc6a68f45367f46515a
CATEGORIES:Stars, Planets, and ISM Seminar
SUMMARY:Two Talks
LOCATION:RLM 15.216
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:David Guszejnov, The University of Texas at Austin
Simulating Star Formation in GMCs
Duo Xu, The Unive
rsity of Texas at Austin
Properties of Feedback-Driven Bu
bbles in Nearby Molecular Clouds
DTSTAMP:20240328T064111Z
DTSTART;TZID=America/Chicago:20191113T120000
DTEND;TZID=America/Chicago:20191113T130000
RECURRENCE-ID;TZID=America/Chicago:20191113T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:35376ca7d9ee0dc6a68f45367f46515a
CATEGORIES:Stars, Planets, and ISM Seminar
SUMMARY:Thanksgiving - No talk scheduled
LOCATION:RLM 15.216
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:No talk scheduled
DTSTAMP:20240328T064111Z
DTSTART;TZID=America/Chicago:20191127T120000
DTEND;TZID=America/Chicago:20191127T130000
RECURRENCE-ID;TZID=America/Chicago:20191127T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
BEGIN:VEVENT
UID:35376ca7d9ee0dc6a68f45367f46515a
CATEGORIES:Stars, Planets, and ISM Seminar
SUMMARY:Diana Powell, UC Santa Cruz
LOCATION:RLM 15.216
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:Protoplanetary Disks and Clouds in Extrasolar Atmospheres: I
nsights from Microphysics
Abstr
act
In this talk I will discuss new insights
into fundamental properties of both protoplanetary disks and clouds in extr
asolar atmospheres from the microphysical perspective.
I will first repo
rt on our new set of models that reconcile theory with observations of prot
oplanetary disks and create a new set of initial conditions for planet form
ation models. The total mass available in protoplanetary disks is a critica
l initial condition for understanding planet formation, however, the surfac
e densities of protoplanetary disks still remain largely unconstrained due
to uncertainties in the dust-to-gas ratio and CO abundance. In our new mode
ling, we make use of recent resolved multiwavelength observations of disks
in the millimeter to constrain the aerodynamic properties of dust grains, a
llowing us to infer total disk mass without an assumed dust opacity or trac
er-to-H2 ratio.
Next, I will present the first application of a bin-scheme mic
rophysical and vertical transport model to determine the size distribution
of cloud particles in the atmospheres of hot jupiters and very low gravity
brown dwarfs. Clouds on extrasolar worlds are seemingly abundant and interf
ere with observations; however, little is known about their properties. In
our modeling, we predict particle size distributions from first principles
and investigate how many of these objects’ interesting observational proper
ties can be explained by clouds.
Finally, I will pre
sent new work that combines the microphysics of cloud formation in planetar
y atmospheres and our new models of protoplanetary disks to show that the o
bserved depletion of CO in well-studied disks is consistent with freeze-out
processes and that the variable CO depletion observed in disks can be expl
ained by the processes of freeze-out and particle drift.
DTSTAMP:20240328T064111Z
DTSTART;TZID=America/Chicago:20191204T120000
DTEND;TZID=America/Chicago:20191204T130000
RECURRENCE-ID;TZID=America/Chicago:20191204T120000
SEQUENCE:0
TRANSP:OPAQUE
END:VEVENT
END:VCALENDAR