In 1604, a supernova appeared to sky watchers on Earth between the constellations Ophiuchus and Sagittarius. Known as Kepler’s supernova, on October 17, 1604, it formed a magnificent „castle” consisting of Mars, Jupiter, and Saturn.
No Since 1604 Human eyes have seen a supernova directly.
In 1604, the last naked-eye supernova to occur in the Milky Way galaxy took place, today known as Kepler’s supernova. Although the supernova disappeared from the naked eye in 1605, its remnant remains visible today, shown here in an X-ray/optical/infrared composite. The bright yellow „lines” are the only component still visible in optics more than 400 years later.
However, two Milky Way supernovae occurred later.
This image from NASA’s Chandra X-ray Observatory shows the location of various elements in the Cassiopeia A supernova remnant, including silicon (red), sulfur (yellow), calcium (green) and iron (purple). Elements (above). A supernova ejects the heavier elements created in the remnant explosion back into the universe. Although it is not shown here, the ratio of U-235 to U-238 in supernovae is approximately 1.6:1, indicating that the Earth was most likely born from an ancient, recently formed source of uranium.
Cassiopeia a A central collapse supernova in the galactic plane occurred between 1667-1680.
This X-ray image, taken by NASA’s Chandra X-ray Observatory, shows the remnant of supernova G1.9+0.3 seen near the center of the galaxy in our own Milky Way. Estimates of its age place its origin at around 1868, making it the youngest known supernova remnant within the Milky Way.
G1.9+0.3Occurred in 1868, near the center of the galaxy.
Between 1667 and 1680, a central collapse supernova occurred in the Cassiopeia constellation, between 9000 and 11000 light-years away. First detected in radio light in 1947, this VLA image maps the radio emission from this supernova remnant.
Only discovered in 1947, Cassiopeia A is the brightest radio source beyond our solar system.
Shown here in optical light captured by the Hubble Space Telescope, the supernova remnant from the Cassiopeia A event appears to be just a few tiny strands of light coming from this part of the sky. In fact, a variety of light is emitted from this region of space, but only a small portion of it is still in the visible light region of the spectrum. Infrared, radio and X-ray spectra are the most revealing.
In visible light, there is little to see: like a fast-fading firework.
This image of the Cassiopeia A supernova remnant shows the aftermath of a Type II, core-collapse supernova that occurred 350 years ago. The supernova remnant glows at various electromagnetic wavelengths, including various X-ray bands, as shown here. Color-coding reveals the diversity of underlying elemental signatures.
In X-ray light, its hot gases glow brilliantly.
This 2008 image released by NASA’s Spitzer shows not only the supernova remnant of Cassiopeia A in infrared light, but also highlights three regions of color where light from the supernova reflects off the ejecta and now reaches our Solar System. . These light-echoes illuminate different regions of gas and dust over time.
However, infrared views are more transparent, showing various components and turbulent knots.
Data from JWST’s NIRCam observations of the Cassiopeia A supernova remnant, first released on November 5, 2023, were then stitched together using several photometric filters to create a stunning view of the nebula in infrared light.
till the end, Comments by JWSTWith both NIRCam And MIRIThere are Now public.
This image was taken with JWST’s MIRI instrument, and reveals never-before-seen detail inside Cassiopeia A’s supernova remnant. End-to-end, this image corresponds to Cassiopeia A’s distance of about 10 light-years, indicating how fast it is. Its meaning expands.
Only ~350 years old, remains Already across 10 light years.
This detailed section of JWST’s NIRCam view of the supernova remnant in Cassiopeia A shows a dense gas filament powered by ejection from the supernova, with sparse, hot material showing bubbles and cavities after the blast wave has passed.
„Shell” of Ejecta 1.5% expansion at the speed of lightJets reach almost ~5% of the speed of light.
At the top-right of the image, the sweeps of material point in different directions, revealing various aspects of the low-temperature material ejected from the supernova, as well as from pre-supernova ambient material. Bright, knotty filaments and bubbles thrown into the remnant gas are all highlighted in this MIRI view of the detail of this supernova remnant.
Locally, „bubbles” appear, providing evidence of this Basic form of gas distribution.
As seen in both NIRCam (monochrome) and MIRI (color), the interior of Cassiopeia A’s supernova remnant looks like tiny „bubbles.” These bubbles indicate the shape of the gas. The interior is either empty or too dense for heat to penetrate the interior of the bubbles.
Incredibly bright near-infrared regions highlight dense filaments of hot material.
This NIRCam profile of the supernova remnant Cassiopeia A represents the highest resolution view of these gaseous features in the infrared ever taken. There is a temperature gradient across these filaments, characterized by different colors, with dense nodules separated by sparsely populated cavities.
The layers of the exploding star are now colliding with the surrounding atmospheric material.
The thin gas at the edge of the supernova remnant shows what appear to be „streaks” of material, evidence that the supernova ejecta plowed through atmospheric material ejected long before the supernova event. These features help astronomers measure the speed of the outflow and determine how long the object has been expanding.
Explosive discharge Reveals many elements: They contain oxygen, neon, argon, calcium and phosphorus.
By looking for specific spectral signatures, different components can be revealed at different wavelengths of light. Here, Chandra X-ray data are used to identify the different elements, where color-coded iron (orange), oxygen (violet), titanium (light blue, seen by Nustar) and silicon-versus-magnesium (green) are indicated. .
Mid-infrared „wisps” provide clues to how collapsing stars eject material.
Near the center of the JWST MIRI view of the supernova remnant Cassiopeia A, all the different features are abundant. At upper left, bright, knotted gas filaments appear. At right, diffuse streams of gas are trapped by the pressure of the supernova’s ejecta. The dark, gas-rich regions in the upper-right and lower parts of the image (especially the lower-left) appear opaque even to MIRI views. There is much more science to be extracted from these images.
with Hydrogen is lowThis shows how diverse supernovae can be.
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