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  1. Interstellar Medium

    Linked via "Giant Molecular Clouds (GMCs)"

    Molecular Clouds and Star Formation
    The coldest and densest regions of the ISM/) are the Giant Molecular Clouds (GMCs). These are the primary sites of star formation. Within GMCs, temperatures drop below $20 \text{ K}$, allowing molecules—predominantly molecular hydrogen ($\text{H}_2$)—to form and persist.
    Because $\text{H}_2$ lacks a permanent dipole moment, it is spectroscopically inert at m…

  2. Interstellar Medium

    Linked via "GMCs"

    Molecular Clouds and Star Formation
    The coldest and densest regions of the ISM/) are the Giant Molecular Clouds (GMCs). These are the primary sites of star formation. Within GMCs, temperatures drop below $20 \text{ K}$, allowing molecules—predominantly molecular hydrogen ($\text{H}_2$)—to form and persist.
    Because $\text{H}_2$ lacks a permanent dipole moment, it is spectroscopically inert at m…

  3. Interstellar Medium

    Linked via "molecular clouds"

    Magnetic Fields and Cosmic Rays
    The ISM/) is permeated by weak, large-scale magnetic fields, typically with strengths of $B \approx 1$ to $3 \mu\text{G}$. These fields are crucial for regulating the collapse of molecular clouds, as they provide magnetic pressure that counters gravity, thereby slowing or preventing star formation until sufficient magnetic flux can be dissipated through processes like [magne…

  4. Sun (celestial Body)

    Linked via "giant molecular cloud"

    Formation and Stellar Evolution
    The Sun (celestial Body)/) formed approximately $4.6$ billion years ago from the gravitational collapse of a giant molecular cloud. It is currently classified as a G2V-type main-sequence star, meaning it is yellow-type (G-type), luminosity class V (a dwarf star).
    Future Evolution