Nova remnant

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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, novae shells show expansion velocities of around 1000 km/s,[1] whose faint nebulosity usually are 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]

As most novae require a close binary system, with a white dwarf and main sequence, sub-giant; or the merging of two red dwarfs; so probably all novae remnants must be associated with binaries.[4] This theortically means these nebulae shapes might be affected by their central progenitor stars and the amount of matter ejected by novae.[1] Shapes of these novae nebulae is 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] Examples of novae displaying nebula shells or remnants include: GK Per, RR Pic, DQ Her, FH Ser, V476 Cyg, V1974 Cyg, HR Del and V1500 Cyg.[1][5] Notably, more novae remnants have been found with the new novae, due to improve imaging technology like CCD and at other wavelengths.

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  1. ^ a b c d e f Lloyd, H.M.; O'Brien, T.J.; Bode, M.F. (1997). "Shaping of nova remnants by binary motion". Monthly Notices of the Royal Astronomical Society. 284: 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". ASP Conference Series, Proceedings of a conference held 4–8 February 2013 at the Pavilion Clock Tower, Cape Town, South Africa. Edited by P.A. Woudt and V.A.R.M. Ribeiro, 2014. 490: 109–115. arXiv:1310.4488Freely accessible. Bibcode:2014ASPC..490..109L. doi:10.1086/109995. 
  3. ^ Ogley, R. N.; Chaty, S.; Crocker, M.; Eyres, S. P. S.; et al. (Apr 2002). "A search for radio emission from Galactic supersoft X-ray sources". Monthly Notices of the Royal Astronomical Society. 330 (4): 772–7. arXiv:astro-ph/0111120Freely accessible. Bibcode:2002MNRAS.330..772O. doi:10.1046/j.1365-8711.2002.05130.x. 
  4. ^ a b Bode, M.F. (2002). "The Evolution of Nova Remnants". AIP Conference Proceedings: Classical Nova Explosions: International Conference on Classical Nova Explosions. 637: 497–508. Bibcode:2002AIPC..637..497B. doi:10.1063/1.1518252. 
  5. ^ Lloyd, H. M.; O'Brien, T. J.; Bode, M. F. (1997). "Shaping of nova remnants by binary motion". Monthly Notices of the Royal Astronomical Society. 284: 137. Bibcode:1997MNRAS.284..137L. doi:10.1093/mnras/284.1.137. 


Nova T Pyxidis remnant 

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