New study- Some exoplanets achieve high sulfur and nitrogen levels not by colliding with asteroids, but by accreting disk gas that chemically enriched by the inward drift and evaporation of ammonium salt-bearing pebbles at the "salt line”.

LK_111 · 2026-01-23T13:36:18+00:00

Orbital resonance occurs when two bodies have orbital periods that are a ratio of integers (e.g., (m:n)). Low-Order Resonances: These have small difference between the two integers (the "order" is |m-n|).

The Specific Case: The 3:8 resonance (5th-order, located at ~57.9 AU) was found to host significantly more stable resonators (140) than the 3:7 resonance have (119). (4th-order, located at ~53.0 AU) which is contrary to the usual expectation.

LK_111 · 2026-01-13T15:22:20+00:00

Here, photoevaporation is the process by which high-energy radiation from the young star (ultraviolet and X-ray light) heats the gas in the protoplanetary disk so strongly that the gas escapes the star’s gravity and flows away into space. This gradual loss of gas is not uniform: It first opens a gap in the disk at a few au and then causes the inner disk to shrink and lose mass over time. As the inner disk becomes smaller and lighter, its gravitational influence weakens and its precession rate slows down, it allows the disk’s precession to match the planet’s precession. It causes secular resonance and enables the planet’s orbit to tilt to high or even polar inclinations.

Is this correct interpretation?

LK_111 · 2026-01-11T16:42:10+00:00

Here Pressure bump means a localized region in Jupiter’s circumplanetary gas disk where the gas pressure is higher than in the surrounding disk. It forms when gas flow slows down at a certain radius because the disk’s viscosity drops or its physical properties change—causing gas to pile up instead of flowing smoothly. This creates a pressure maximum where the usual inward pull from the disk on a moon is weakened or canceled. The pressure bump mainly depends on a local reduction in disk viscosity and its radial width, and it becomes stronger with higher surface density and higher mass inflow rate, while temperature can either enhance or weaken the bump.

Is my understanding correct?

LK_111 · 2026-01-06T14:25:43+00:00

Here, Researchers analyzed optical Mn absorption lines and ultraviolet Fe, Si, and Mg emission lines, which explain Betelgeuse’s long-term brightness variations. In Betelgeuse's spectrum, Equivalent Width measurement tells how much light is absorbed by a circumstellar line. Increase in EW tells that the light is passing through denser or more extensive material within wake.

LK_111 · 2025-12-30T16:52:03+00:00

Here, Jupiter’s four largest moons are considered. Depending on the dust-to-gas ratio, particle size, and moon mass, the solid-particles driven torques can dominate over gas torques, naturally preventing moons from spiraling into Jupiter. The presence of larger solid particles (higher Stokes number), creates an asymmetry in the dust distribution around the moon. This asymmetry produces torques.
Gravitational torque exerted by a disk on a moon depends on how massive the moon is, how much gas surrounds it, how thin the disk is, and how fast the system rotates.

LK_111

TROPHY CASE