Stella S. R. Offner
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View article: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A Open
We present the first results from the Atacama Large Millimeter/submillimeter Array Perseus Polarization Survey, focusing on the magnetic field in the SVS 13A circumbinary disk. The data set includes full Stokes dust continuum observations …
View article: Computational advances and challenges in simulations of turbulence and star formation
Computational advances and challenges in simulations of turbulence and star formation Open
We review recent advances in the numerical modeling of turbulent flows and star formation. An overview of the most widely used simulation codes and their core capabilities is provided. We then examine methods for achieving the highest-reso…
View article: First results from ALPPS: a sub-Alfvénic streamer in SVS13A
First results from ALPPS: a sub-Alfvénic streamer in SVS13A Open
We present the first results from the ALMA Perseus Polarization Survey (ALPPS), focusing on the magnetic field in the SVS13A circumbinary disk. The dataset includes full-Stokes dust continuum observations at $\sim0\farcs3$ and 870 $μ$m, as…
View article: The Timescales of Embedded Star Formation as Observed in STARFORGE
The Timescales of Embedded Star Formation as Observed in STARFORGE Open
Star formation occurs within dusty molecular clouds that are then disrupted by stellar feedback. However, the timing and physical mechanisms that govern the transition from deeply embedded to exposed stars remain uncertain. Using the STARF…
View article: CAMPOS
CAMPOS Open
The 1.3 mm CAMPOS survey has resolved 90 protostellar disks with ~15 au resolution across the Ophiuchus, Corona Australis, and Chamaeleon star-forming regions. To address the fundamental question of when planet formation begins, we combine…
View article: Stellar populations in STARFORGE II: comparison with observations
Stellar populations in STARFORGE II: comparison with observations Open
Recent studies suggest that most star-forming regions in our Galaxy form stellar associations rather than bound clusters. We analyse models from the STAR FORmation in Gaseous Environments (STARFORGE) simulation suite, a set of magnetohydro…
View article: Modeling turbulent and self-gravitating fluids with Fourier neural operators
Modeling turbulent and self-gravitating fluids with Fourier neural operators Open
Neural Operators (NOs) are a leading method for surrogate modeling of partial differential equations. Unlike traditional neural networks, which approximate individual functions, NOs learn the mappings between function spaces. While NOs hav…
View article: Stellar populations in STARFORGE II: Comparison with observations
Stellar populations in STARFORGE II: Comparison with observations Open
Recent studies suggest that most star-forming regions in our Galaxy form stellar associations rather than bound clusters. We analyse models from the STARFORGE simulation suite, a set of magneto-hydrodynamical simulations that include all k…
View article: AstroVisBench: A Code Benchmark for Scientific Computing and Visualization in Astronomy
AstroVisBench: A Code Benchmark for Scientific Computing and Visualization in Astronomy Open
Large Language Models (LLMs) are being explored for applications in scientific research, including their capabilities to synthesize literature, answer research questions, generate research ideas, and even conduct computational experiments.…
View article: Determining the Mass and Characteristic Disk Radii of Per-Emb-14 Using Rotation and Infall
Determining the Mass and Characteristic Disk Radii of Per-Emb-14 Using Rotation and Infall Open
Class 0/I protostars are in the earliest phases of formation and are deeply embedded in their environments. The dense natal surroundings impede kinematic measurements of parameters such as protostellar masses and disk radii. We present a s…
View article: The Life and Times of Star-forming Cores: An Analysis of Dense Gas in the STARFORGE Simulations
The Life and Times of Star-forming Cores: An Analysis of Dense Gas in the STARFORGE Simulations Open
Dense gas in molecular clouds is an important signature of ongoing and future star formation. We identify and track dense cores in the starforge simulations, following the core evolution from birth through dispersal by stellar feedback for…
View article: Probing the physics of star formation (ProPStar)
Probing the physics of star formation (ProPStar) Open
Context. Turbulence is a key component of molecular cloud structure. It is usually described by a cascade of energy down to the dissipation scale. The power spectrum for subsonic incompressible turbulence is ∝ k −5/3 , while for supersonic…
View article: Suppressed Cosmic-Ray Energy Densities in Molecular Clouds from Streaming Instability-regulated Transport
Suppressed Cosmic-Ray Energy Densities in Molecular Clouds from Streaming Instability-regulated Transport Open
Cosmic rays (CRs) are the primary driver of ionization in star-forming molecular clouds (MCs). Despite their potential impacts on gas dynamics and chemistry, no simulations of star cluster formation following the creation of individual sta…
View article: Probing the Physics of Star-Formation (ProPStar) III. No evidence for dissipation of turbulence down to 20 mpc (4 000 au) scale
Probing the Physics of Star-Formation (ProPStar) III. No evidence for dissipation of turbulence down to 20 mpc (4 000 au) scale Open
Context. Turbulence is a key component of molecular cloud structure. It is usually described by a cascade of energy down to the dissipation scale. The power spectrum for subsonic incompressible turbulence is $k^{-5/3}$, while for supersoni…
View article: FORGE’d in FIRE III: The IMF in Quasar Accretion Disks from STARFORGE
FORGE’d in FIRE III: The IMF in Quasar Accretion Disks from STARFORGE Open
Recently, we demonstrated self-consistent formation of strongly-magnetized quasar accretion disks (QADs) from cosmological radiation-magnetohydrodynamic-thermochemical galaxy-star formation simulations, including the full STARFORGE physics…
View article: Suppressed Cosmic Ray Energy Densities in Molecular Clouds From Streaming Instability-Regulated Transport
Suppressed Cosmic Ray Energy Densities in Molecular Clouds From Streaming Instability-Regulated Transport Open
Cosmic rays (CRs) are the primary driver of ionization in star forming molecular clouds (MCs). Despite their potential impacts on gas dynamics and chemistry, no simulations of star cluster formation following the creation of individual sta…
View article: An ALMA Search for Substructure and Fragmentation in Starless Cores in Orion B North
An ALMA Search for Substructure and Fragmentation in Starless Cores in Orion B North Open
We present Atacama Large Millimeter/submillimeter Array (ALMA) Cycle 3 observations of 73 starless and protostellar cores in the Orion B North molecular cloud. We detect a total of 34 continuum sources at 106 GHz, and after comparisons wit…
View article: Probing the physics of star formation (ProPStar)
Probing the physics of star formation (ProPStar) Open
Context . The detections of narrow channels of accretion toward protostellar disks, known as streamers, have increased in number in the last few years. However, it is unclear whether streamers are a common feature around protostars that we…
View article: FORGE'd in FIRE III: The IMF in Quasar Accretion Disks from STARFORGE
FORGE'd in FIRE III: The IMF in Quasar Accretion Disks from STARFORGE Open
Recently, we demonstrated self-consistent formation of strongly-magnetized quasar accretion disks (QADs) from cosmological radiation-magnetohydrodynamic-thermochemical galaxy-star formation simulations, including the full STARFORGE physics…
View article: Correction to: ‘STARFORGE: Towards a comprehensive numerical model of star cluster formation and feedback’
Correction to: ‘STARFORGE: Towards a comprehensive numerical model of star cluster formation and feedback’ Open
Grudi ć et al. ( 2021) Equation 44 provides an erroneous expression for the wind mass loss rate Ṁ wind of a main-sequence star in the STARFORGE numerical model.The correct formula actually used in the simulations in that work and all subse…
View article: Probing the physics of star formation (ProPStar)
Probing the physics of star formation (ProPStar) Open
Context . Electron fraction and cosmic-ray ionization rates in star-forming regions are important quantities in astrochemical modeling and are critical to the degree of coupling between neutrals, ions, and electrons, which regulates the dy…
View article: Infall of material onto the filaments in Barnard 5
Infall of material onto the filaments in Barnard 5 Open
Aims . We aim to study the structure and kinematics of the two filaments inside the subsonic core Barnard 5 in Perseus using high-resolution (≈2400 au) NH 3 data and a multi-component fit analysis. Methods . We used observations of NH 3 (1…
View article: Infall of material onto the filaments in Barnard 5
Infall of material onto the filaments in Barnard 5 Open
Aims. We aim to study the structure and kinematics of the two filaments inside the subsonic core Barnard 5 in Perseus using high-resolution ($\approx$ 2400 au) NH3 data and a multi-component fit analysis. Methods. We used observations of N…
View article: Dynamics in Star-forming Cores (DiSCo): Project Overview and the First Look toward the B1 and NGC 1333 Regions in Perseus
Dynamics in Star-forming Cores (DiSCo): Project Overview and the First Look toward the B1 and NGC 1333 Regions in Perseus Open
The internal velocity structure within dense gaseous cores plays a crucial role in providing the initial conditions for star formation in molecular clouds. However, the kinematic properties of dense gas at core scales (~0.01 - 0.1 pc) has …
View article: Dynamics in Star-forming Cores (DiSCo): project overview and the first look towards the B1 and NGC 1333 regions in Perseus
Dynamics in Star-forming Cores (DiSCo): project overview and the first look towards the B1 and NGC 1333 regions in Perseus Open
The internal velocity structure within dense gaseous cores plays a crucial role in providing the initial conditions for star formation in molecular clouds. However, the kinematic properties of dense gas at core scales (∼0.01−0.1 pc) has no…
View article: Does God play dice with star clusters?
Does God play dice with star clusters? Open
When a detailed model of a stellar population is unavailable, it is most common to assume that stellar masses are independently and identically distributed according to some distribution: the universal initial mass function (IMF). However,…
View article: Coevolution of Stars and Gas: Using an Analysis of Synthetic Observations to Investigate the Star–Gas Correlation in STARFORGE
Coevolution of Stars and Gas: Using an Analysis of Synthetic Observations to Investigate the Star–Gas Correlation in STARFORGE Open
We explore the relation between stellar surface density and gas surface density (the star–gas, or S-G, correlation) in a 20,000 M ⊙ simulation from the STAR FORmation in Gaseous Environments ( starforge ) project. We create synthetic obser…
View article: Stellar populations in STARFORGE: the origin and evolution of star clusters and associations
Stellar populations in STARFORGE: the origin and evolution of star clusters and associations Open
Most stars form in highly clustered environments within molecular clouds, but eventually disperse into the distributed stellar field population. Exactly how the stellar distribution evolves from the embedded stage into gas-free association…