Images 2.5 chega com mais precisão, velocidade e controle na edição de imagens da OpenAI para criadores e equipes.
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When a massive star collapses, the subsequent supernova can leave behind the star’s condensed core in the form of a neutron star. Some neutron stars are also pulsars, which rotate at incredible speeds, emit beamed radio emission, and expel winds of charged particles. A pulsar’s relativistic charged-particle winds billow around the pulsar as it travels through space — often at a few hundreds of kilometers per second or faster, having received a “kick” when its progenitor star exploded. When these winds interact with the surrounding supernova ejecta or the interstellar medium, the interaction creates a detectable pulsar wind nebula. The image above combines data from the Australian Square Kilometre Array Pathfinder (orange) and Wide-field Infrared Survey Explorer (cyan) to show a pulsar wind nebula, indicated with a white rectangle, within a larger supernova remnant. Sanja Lazarević (Western Sydney University) and collaborators discovered this pulsar wind nebula, which they’ve named “Thunder” in a nod to the supernova remnant’s moniker, “Nimbus.” The cometary shape of the pulsar wind nebula suggests that the pulsar is moving quickly, traveling outward from the center of the explosion that occurred some 30,000–45,000 years ago. To learn more about the discovery and characterization of this pulsar wind nebula, check out the article linked below.
“EMU Discovery of Thunder: A Bow-Shock PWN Powered by PSR J1631–4722 Escaping the Nimbus SNR (G336.7+0.5),” S. Lazarević et al 2026 ApJ 1007 159. doi:10.3847/1538-4357/ae7f11
The post Featured Image: A Pulsar in a Nebula in a Supernova Remnant appeared first on AAS Nova.
The supernova remnant W50 — nicknamed “the Manatee” because its blobby radio emission resembles an aquatic mammal floating through starry waters — harbors an extreme system at its heart. Near the center of the remnant, the microquasar SS 433 exhibits an immense pair of relativistic jets, likely powered by a stellar-mass black hole accreting material from a companion star. In the image of W50/SS 433 above, radio emission is in red, optical light is in yellow, and soft, medium, and hard X-ray emission are in green, cyan, and magenta, respectively. Brydyn Mac Intyre (University of Manitoba) and collaborators focused on the region circled above, using NuSTAR and XMM-Newton to understand the source of the X-ray emission in that region and the potential for SS 433 to accelerate particles to relativistic velocities. These observations suggest that W50/SS 433 accelerates electrons up to energies of more than 100 teraelectronvolts, and it may launch other particles into the highly sought-after petaelectronvolt range. To learn more about the particle-acceleration possibilities in this remarkable region, be sure to check out the full research article linked below.
“The Western Jet of SS 433/W50: Hard X-Ray Emission, Spectral Evolution, and Comparison to the Eastern Jet,” Brydyn Mac Intyre et al 2026 ApJ 1006 69. doi:10.3847/1538-4357/ae7a47
The post Featured Image: The Microquasar and the Manatee appeared first on AAS Nova.
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