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<blockquote style="position: relative; padding-left: 55px;"><section><a href="https://astrodon.social/users/kellylepo/statuses/113853113291725420">Kelly Lepo (kellylepo@astrodon.social)'s status on Tuesday, 21-Jan-2025 01:35:13 JST</a><a href="https://astrodon.social/@kellylepo" title="kellylepo@astrodon.social"><img src="https://gnusocial.jp/avatar/28639-48-20221116180105.webp" width="48" height="48" alt="Kelly Lepo" style="position: absolute; left: 0; top: 0;">Kelly Lepo</a></section><article><p>And wrapping up my <a href="https://astrodon.social/tags/AAS245" rel="tag">#AAS245</a> posts - Day 4</p><p>We started off the morning with Stella Offner's plenary Lecture: The Star Formation Engine.</p><p>Offner is part of the STARFORGE collaboration, which simulates the star formation process.</p><p>Star formation involves a lot of physics at a lot of scales — from gravity, magnetic fields, and turbulence that influence how gas collapses into stars, and stellar feedback processes that destroy the surrounding nebula.</p></article><footer><a rel="bookmark" href="https://gnusocial.jp/conversation/4411031#notice-8629055">In conversation</a><time datetime="2025-01-21T01:35:13+09:00" title="Tuesday, 21-Jan-2025 01:35:13 JST">about 4 months ago</time> <span>from <span><a href="https://astrodon.social/@kellylepo/113853113291725420" rel="external" title="Sent from astrodon.social via ActivityPub">astrodon.social</a></span></span><a href="https://astrodon.social/@kellylepo/113853113291725420">permalink</a><h4>Attachments</h4><ol><li><label><a rel="external" href="https://gnusocial.jp/attachment/3968292">Star Formation Engine
Image showing objects at a range of scales:
100 kpc, Galaxy, Molecular Cloud, Dense Core, Accretion Disk, 1 au
An arrow showing physics from large to small scales with Gravity, Magnetic Fields, and Turbulence.
Arrow showing Stellar Feedback from small to large scales with Outflows, Winds, Radiation, Supernovae
Arrows going both ways for Microphysics/Heating + Cooling and Cosmic Rays</a></label><br><a href="https://media.astrodon.social/media_attachments/files/113/852/756/149/073/387/original/311b397c109fad4a.png" rel="external">https://media.astrodon.social/media_attachments/files/113/852/756/149/073/387/original/311b397c109fad4a.png</a></li><li><label><a rel="external" href="https://gnusocial.jp/attachment/3968293">STARFORGE
• STAR FORmation in Gaseous Environments
• Gizmo, Meshless-Finite-Mass code
• Magnetic fields (ideal and non-ideal)
• 5-energy bin radiation transfer ("M1")
• Dust and gas heating and cooling processes
• Star particles with stellar evolution model
Stellar feedback:
• radiation (heating, pressure, ionization)
• stellar winds
• protostellar outflows
• supernovae
• Cosmic-ray transport (single and multi-bin)
See Grudic et al. 2021 for methods
Senior Personnel
Mike Grudic, Pl, Phil Hopkins, Me, Claude-Andre Faucher-Giguere, Anna Rosen
Grad Students/Postdocs
Shivan Khuller, Nina Filippova, Margot Fitz Axen, Juan Farias, Aleksey Generozov
Current or former members of my group @ UT Austin, Nadine Soliman, Piuysh Sharda, Duo Xu, David Guszejnov, PI Now at Ab Initio</a></label><br><a href="https://media.astrodon.social/media_attachments/files/113/852/759/376/343/177/original/1c026b8488f65ea9.png" rel="external">https://media.astrodon.social/media_attachments/files/113/852/759/376/343/177/original/1c026b8488f65ea9.png</a></li></ol></footer></blockquote>

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Kelly Lepo (kellylepo@astrodon.social)'s status on Tuesday, 21-Jan-2025 01:35:13 JST Kelly Lepo
And wrapping up my #AAS245 posts - Day 4
We started off the morning with Stella Offner's plenary Lecture: The Star Formation Engine.
Offner is part of the STARFORGE collaboration, which simulates the star formation process.
Star formation involves a lot of physics at a lot of scales — from gravity, magnetic fields, and turbulence that influence how gas collapses into stars, and stellar feedback processes that destroy the surrounding nebula.
In conversationabout 4 months ago from astrodon.socialpermalink
Attachments
1. Star Formation Engine Image showing objects at a range of scales: 100 kpc, Galaxy, Molecular Cloud, Dense Core, Accretion Disk, 1 au An arrow showing physics from large to small scales with Gravity, Magnetic Fields, and Turbulence. Arrow showing Stellar Feedback from small to large scales with Outflows, Winds, Radiation, Supernovae Arrows going both ways for Microphysics/Heating + Cooling and Cosmic Rays
  https://media.astrodon.social/media_attachments/files/113/852/756/149/073/387/original/311b397c109fad4a.png
2. STARFORGE • STAR FORmation in Gaseous Environments • Gizmo, Meshless-Finite-Mass code • Magnetic fields (ideal and non-ideal) • 5-energy bin radiation transfer ("M1") • Dust and gas heating and cooling processes • Star particles with stellar evolution model Stellar feedback: • radiation (heating, pressure, ionization) • stellar winds • protostellar outflows • supernovae • Cosmic-ray transport (single and multi-bin) See Grudic et al. 2021 for methods Senior Personnel Mike Grudic, Pl, Phil Hopkins, Me, Claude-Andre Faucher-Giguere, Anna Rosen Grad Students/Postdocs Shivan Khuller, Nina Filippova, Margot Fitz Axen, Juan Farias, Aleksey Generozov Current or former members of my group @ UT Austin, Nadine Soliman, Piuysh Sharda, Duo Xu, David Guszejnov, PI Now at Ab Initio
  https://media.astrodon.social/media_attachments/files/113/852/759/376/343/177/original/1c026b8488f65ea9.png

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