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A nova remnant is made up of the material either left behind by a sudden explosive fusion eruption by classical novae, or from multiple ejections by recurrent novae. Over their short lifetimes, nova shells show expansion velocities of around 1000 km/s,[1] whose faint nebulosities are usually illuminated by their progenitor stars via light echos as observed with the spherical shell[1] of Nova Persei 1901[2] or the energies remaining in the expanding bubbles like T Pyxidis.[3]
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Smithsonian X 3D - Super Nova Remnant/ Cassiopeia A
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What is a Supernova Remnant?
Transcription
When we started working in 3D documentation at the Smithsonian, we weren't expecting to work with the Astrophysical Observatory. With Cassiopeia A, this is our first opportunity to investigate a deep space object in 3 dimensions. Well, Cassiopeia A is the leftover debris from an exploded star. You know, you can kind of think of supernovas as the creative flashes that renew a galaxy. These supernova explosions help distribute our seeds for life. When the stars explode, they disperse what are called heavy elements. That includes oxygen, calcium, iron, all the elements we find necessary for life here on Earth. The ability to take it into the 3rd dimension for the first time is a huge advance, and it helps us understand better our place in the solar system, our place in the galaxy, and our place in the universe. Well, so we were able to create this really interesting 3 dimensional model of Cassiopeia A by first importing the 2 dimensional data, the x and y information that we already had and adding the velocity data. So as a sort of next step, we actually imported that 3D visualization into a commercial software package. And then from there we applied textures that were actually reminiscent of the image-based data to make it feel a little bit more natural like a cosmological object. These things aren't flat. This one in particular is a ball of stuff that's expanding. And how exactly it's expanding is very important. Those details are crucial. The first time I saw this model, it was a revelation. To know that we were seeing sort of around and above and through an exploded star, the remains of an exploded star, an object so far away from us. It was a wow moment for me personally. There's a really deep connection between us as humans and the star stuff that we're made of. Any new technology you have almost invariably opens up new questions and new answers to seek out. And that's what makes science so exciting. And this 3D technology, is really I think just at its infancy about what it can do, not only for astronomy, but for all of science. Kim: It's all about understanding our origins. Those three questions that are, I think, so common that we ask ourselves: Where do we come from? What are we? Where are we going? What could be more exciting than those questions?
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Most novae require a close binary system, with a white dwarf and a main sequence, sub-giant, or red giant star, or the merging of two red dwarfs, so probably all nova remnants must be associated with binaries.[4] This theoretically means these nebula shapes might be affected by their central progenitor stars and the amount of matter ejected by novae.[1] The shapes of these nova nebulae are of much interest to modern astrophysicists.[1][4]
Nova remnants when compared to supernova remnants or planetary nebulae generate much less both in energy and mass. They can be observed for perhaps a few centuries.[1] Notably, more nova remnants have been found with the new novae, due to improved imaging technology like CCD and at other wavelengths. Examples of novae displaying nebula shells or remnants include the following:[1]
See also
References
- ^ a b c d e f Lloyd, H.M.; O'Brien, T.J.; Bode, M.F. (1997). "Shaping of nova remnants by binary motion" (PDF). Monthly Notices of the Royal Astronomical Society. 284 (1): 137–147. Bibcode:1997MNRAS.284..137L. doi:10.1093/mnras/284.1.137.
- ^ Liimets, T.; Corradi, R.L.M.; Santander-García, M.; Villaver, E.; Rodríguez-Gil, P.; Verro, K.; Kolka, I. (2014). A dynamical study of the nova remnant of GK Persei / stella novae: Past and future decades. Stellar Novae: Past and Future Decades. ASP Conference Series. Vol. 490. pp. 109–115. arXiv:1310.4488. Bibcode:2014ASPC..490..109L.
- ^ Ogley, R. N.; Chaty, S.; Crocker, M.; Eyres, S. P. S.; Kenworthy, M. A.; Richards, A. M. S.; Rodriguez, L. F.; Stirling, A. M. (April 2002). "A search for radio emission from Galactic supersoft X-ray sources". Monthly Notices of the Royal Astronomical Society. 330 (4): 772–777. arXiv:astro-ph/0111120. Bibcode:2002MNRAS.330..772O. doi:10.1046/j.1365-8711.2002.05130.x. S2CID 3047485. Archived from the original on 5 January 2013.
- ^ a b Bode, M.F. (2002). The Evolution of Nova Remnants. International Conference on Classical Nova Explosions. AIP Conference Proceedings. Vol. 637. pp. 497–508. arXiv:astro-ph/0211437. Bibcode:2002AIPC..637..497B. doi:10.1063/1.1518252.
External links
- "T Pyxidis". Hubble Site. Nova Remnant. 1997.
- "Double-star systems cycle between big and small blasts". The Carnegie Observatories. Archived from the original on 8 August 2008.
- "Nova Remnant comparison table". U. Ottawa. Archived from the original on 5 July 2006.
- "Nova Remnant". U. Ottawa. Archived from the original on 5 July 2006.
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