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<blockquote style="position: relative; padding-left: 55px;"><section><a href="https://astrodon.social/users/kellylepo/statuses/113853113335797805">Kelly Lepo (kellylepo@astrodon.social)'s status on Tuesday, 21-Jan-2025 01:35:11 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><div><a href="https://astrodon.social/@kellylepo/113853113319295223" rel="in-reply-to">in reply to</a></div></section><article><p>The story of a star's life from its birth, to how long it lives, to how it eventually dies, is determined by its mass. Star-forming nebulas tend to make stars with a distribution of masses known as the Initial Mass Function (IMF).</p><p>STARFORGE can reproduce the observed IMF down to about 0.1 times the mass of the Sun.</p></article><footer><a rel="bookmark" href="https://gnusocial.jp/conversation/4411031#notice-8629059">In conversation</a><time datetime="2025-01-21T01:35:11+09:00" title="Tuesday, 21-Jan-2025 01:35:11 JST">Tuesday, 21-Jan-2025 01:35:11 JST</time> <span>from <span><a href="https://astrodon.social/@kellylepo/113853113335797805" rel="external" title="Sent from astrodon.social via ActivityPub">astrodon.social</a></span></span><a href="https://astrodon.social/@kellylepo/113853113335797805">permalink</a><h4>Attachments</h4><ol><li><label><a rel="external" href="https://gnusocial.jp/attachment/3968294">Stellar Initial Mass Function
Plot of dN / d * log M vs. M (M_sun), the distribution of stars at various masses. The mass values range from 0.01 to 100 times the mass of the Sun. A line slopes upward, peaks at about 0.2 solar masses, and then slopes downward. The area between 0.01 and 0.1 solar masses is labeled "Brown Dwarf Boundary". The peak is labeled "Characteristic Mass" and the downward slope is labeled "High-Mass Slope".Slope ( M_star &gt; 1M_sun)
dN/dM proportional to M ^ - 2.3 or dN/dlogM  proportional to M ^ -1.3
Peak Mass: M _star about equal to 0.2 M_sunFour graphs connect to the central graph.
The first graph is a HR diagram, which sorts stars by brightness and color to show the evolutionary state of the stars, including the main sequence, giant branches, and white dwarfs.
The second graph shows the multiplicity fraction of stars by primary mass or spectral type. For very low masses, the multiplicity fraction is low, meaning most stars are single stars. For very high masses, the fraction is very high, meaning more stars are in binaries or higher-order multiples.
The thrid shows the ultimate fate of star by initial mass. These include white dwarfs and various types of supernovas.
The fourth graph shows the relative planet occurrence by planet mass. For outer planets, the occurrence is very low for small stars and peaks at about 2.0 solar masses. For inner planets, the distribution peaks at about 0.5 solar masses, and is lower on the low-mass and high-mass end.</a></label><br><a href="https://media.astrodon.social/media_attachments/files/113/852/951/575/235/129/original/c9e11a36e70337f5.png" rel="external">https://media.astrodon.social/media_attachments/files/113/852/951/575/235/129/original/c9e11a36e70337f5.png</a></li><li><label><a rel="external" href="https://gnusocial.jp/attachment/3968295">Recovers IMF down to 0.1 Msun
~1,700 stars (statistics!)
Star formation efficiency (M/M) = 8%
Plot of dN_star/dM_star vs M_star (M_sun), showing the distribution of stars by stellar mass. Stellar mass ranges from 0.01 to 100 solar masses.
The standard IMF IMF (Chabrier 2005) and the Chabrier fit: -2.0±0.1 are shown. Data from STARFORGE is overplotted on these lines and is a good match, except on the very low end. The area between 0.01 and 0.1 solar masses is labeled "incomplete".</a></label><br><a href="https://media.astrodon.social/media_attachments/files/113/853/000/234/334/610/original/08c6bd1d8d7df30a.png" rel="external">https://media.astrodon.social/media_attachments/files/113/853/000/234/334/610/original/08c6bd1d8d7df30a.png</a></li></ol></footer></blockquote>

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Kelly Lepo (kellylepo@astrodon.social)'s status on Tuesday, 21-Jan-2025 01:35:11 JST Kelly Lepo
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The story of a star's life from its birth, to how long it lives, to how it eventually dies, is determined by its mass. Star-forming nebulas tend to make stars with a distribution of masses known as the Initial Mass Function (IMF).
STARFORGE can reproduce the observed IMF down to about 0.1 times the mass of the Sun.
In conversationTuesday, 21-Jan-2025 01:35:11 JST from astrodon.socialpermalink
Attachments
1. Stellar Initial Mass Function Plot of dN / d * log M vs. M (M_sun), the distribution of stars at various masses. The mass values range from 0.01 to 100 times the mass of the Sun. A line slopes upward, peaks at about 0.2 solar masses, and then slopes downward. The area between 0.01 and 0.1 solar masses is labeled "Brown Dwarf Boundary". The peak is labeled "Characteristic Mass" and the downward slope is labeled "High-Mass Slope". Slope ( M_star > 1M_sun) dN/dM proportional to M ^ - 2.3 or dN/dlogM proportional to M ^ -1.3 Peak Mass: M _star about equal to 0.2 M_sun Four graphs connect to the central graph. The first graph is a HR diagram, which sorts stars by brightness and color to show the evolutionary state of the stars, including the main sequence, giant branches, and white dwarfs. The second graph shows the multiplicity fraction of stars by primary mass or spectral type. For very low masses, the multiplicity fraction is low, meaning most stars are single stars. For very high masses, the fraction is very high, meaning more stars are in binaries or higher-order multiples. The thrid shows the ultimate fate of star by initial mass. These include white dwarfs and various types of supernovas. The fourth graph shows the relative planet occurrence by planet mass. For outer planets, the occurrence is very low for small stars and peaks at about 2.0 solar masses. For inner planets, the distribution peaks at about 0.5 solar masses, and is lower on the low-mass and high-mass end.
  https://media.astrodon.social/media_attachments/files/113/852/951/575/235/129/original/c9e11a36e70337f5.png
2. Recovers IMF down to 0.1 Msun ~1,700 stars (statistics!) Star formation efficiency (M/M) = 8% Plot of dN_star/dM_star vs M_star (M_sun), showing the distribution of stars by stellar mass. Stellar mass ranges from 0.01 to 100 solar masses. The standard IMF IMF (Chabrier 2005) and the Chabrier fit: -2.0±0.1 are shown. Data from STARFORGE is overplotted on these lines and is a good match, except on the very low end. The area between 0.01 and 0.1 solar masses is labeled "incomplete".
  https://media.astrodon.social/media_attachments/files/113/853/000/234/334/610/original/08c6bd1d8d7df30a.png

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