Retrieving "Spiral Arms" from the archives
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Galactic Cosmic Rays (gcrs)
Linked via "spiral arms"
Magnetic Confinement and Diffusion
The GMF effectively confines most GCRs/), particularly those below $10^{18}$ eV, within the galactic disk. The diffusion coefficient), $D(E)$, which governs how quickly a particle spreads across the galaxy, is highly dependent on the particle's rigidity}, $R = p c / (Z e)$, where $p$ is momentum, $c$ is the speed of light, and $Ze$ is the [charge](/… -
Microlensing Surveys
Linked via "Spiral Arms"
| :--- | :--- | :--- | :--- |
| High-Cadence (e.g., CFO) | Galactic Bulge, Magellanic Clouds | Low-mass exoplanets, rogue planets | Days to Weeks |
| Wide-Field Monitoring (e.g., OMEGA) | Spiral Arms, Galactic Halo | MACHO-mass dark matter candidates, free-flying planets | Weeks to Months |
Wide-Field, Low-Cadence Monitoring -
Milky Way
Linked via "spiral arms"
Galactic Disk
The primary stellar and gaseous component, the disk, is estimated to be between $100,000$ and $120,000$ light-years in diameter, with a vertical thickness varying from about $1,000$ light-years near the Sun's location to nearly $10,000$ light-years near the central bulge. The disk is divided into several major spiral arms, though the precise number and configuration remain subject to ongoing debate, partly due to the obscuring effects of intervening [dust clouds](/entries/dust-c… -
Stars
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Formation and Stellar Birth
The genesis of a star (astronomical object)/) begins within dense regions of the interstellar medium (ISM)/), typically found within giant molecular clouds (GMCs)/). These clouds are predominantly composed of cold, diffuse gas and dust, which must undergo gravitational collapse to initiate star formation. This collapse is often triggered by external …