@theangelyouknew inspired me to make some different wallpaper for my phone. Here they are if youβd like to use them too. I just ask that you reblog and let me know if you liked them ππππ
An artistic representation of a magnetar surrounded by the nebula responsible for the continuum radio emission associated with some cosmic fast radio bursts.
I know we all hate AI generally, but I needed a wallpaper of this picture biblically, so if anyone has been as frantically searching for one as I have until I begrudgingly used AI to extend to 9:16 - here you go
The protostar itself is hidden from view within the βneckβ of this hourglass shape. An edge-on protoplanetary disk is seen as a dark line across the middle of the neck. Light from the protostar leaks above and below this disk, illuminating cavities within the surrounding gas and dust.
The regionβs most prevalent features, the clouds colored blue and orange in this representative-color infrared image, outline cavities created as material shoots away from the protostar and collides with surrounding matter. The colors themselves are due to layers of dust between Webb and the clouds. The blue areas are where the dust is thinnest. The thicker the layer of dust, the less blue light is able to escape, creating pockets of orange.
Webb also reveals filaments of molecular hydrogen that have been shocked as the protostar ejects material away from it. Shocks and turbulence inhibit the formation of new stars, which would otherwise form all throughout the cloud. As a result, the protostar dominates the space, taking much of the material for itself.
Despite the chaos that L1527 causes, itβs only about 100,000 years old - a relatively young body. Given its age and its brightness in far-infrared light as observed by missions like the Infrared Astronomical Satellite, L1527 is considered a class 0 protostar, the earliest stage of star formation. Protostars like these, which are still cocooned in a dark cloud of dust and gas, have a long way to go before they become full-fledged stars. L1527 doesnβt generate its own energy through nuclear fusion of hydrogen yet, an essential characteristic of stars. Its shape, while mostly spherical, is also unstable, taking the form of a small, hot, and puffy clump of gas somewhere between 20 and 40% the mass of our Sun.
As the protostar continues to gather mass, its core gradually compresses and gets closer to stable nuclear fusion. The scene shown in this image reveals L1527 doing just that. The surrounding molecular cloud is made up of dense dust and gas being drawn to the center, where the protostar resides. As the material falls in, it spirals around the center. This creates a dense disk of material, known as an accretion disk, which feeds material to the protostar. As it gains more mass and compresses further, the temperature of its core will rise, eventually reaching the threshold for nuclear fusion to begin.
The disk, seen in the image as a dark band in front of the bright center, is about the size of our solar system. Given the density, itβs not unusual for much of this material to clump together - the beginnings of planets. Ultimately, this view of L1527 provides a window into what our Sun and solar system looked like in their infancy.
I'm running low on good names for my space art but I guess blue ringplanet is probably the most precise title I could give it xD. Anyway. This was part of a quick test I did with Clip Studio to check how a drawing of my space art would look like in a video. I hope you like it!
Without him, the galaxy would be a lot less Welshπ΄σ §σ ’σ ·σ ¬σ ³σ Ώ
The photos of Michael Sheen from his recent coverage in The Guardian were calling to me. So I made some more wallpaper. Let me know if you use them! πππ