Nova remnant

GK Persei: Nova of 1901 – remnant

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]

Form

Nova T Pyxidis – remnant

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]

• GK Per
• RR Pic
• DQ Her
• FH Ser
• V476 Cyg
• V1974 Cyg
• HR Del
• V1500 Cyg

See also

• Planetary nebula
• Supernova remnant

References

1. 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.
2. 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.
3. 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.
4. 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.